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Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
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they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
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1

Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and  

Open Energy Info (EERE)

Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and Year End Results Jump to: navigation, search OpenEI Reference LibraryAdd to library Web Site: Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and Year End Results Authors Ormat Technologies and Inc. Published Publisher Not Provided, Date Not Provided DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and Year End Results Citation Ormat Technologies, Inc.. Ormat Technologies Inc. Ormat Technologies Reports 2012 Fourth Quarter and Year End Results [Internet]. [updated 2013;cited 2013]. Available from: http://www.ormat.com/news/latest-items/ormat-technologies-reports-2012-fourth-quarter-and-year-end-results

2

Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash  

Open Energy Info (EERE)

Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash Pre-Tax Charge for Impairment to Its North Brawley Geothermal Power Plant Jump to: navigation, search OpenEI Reference LibraryAdd to library Web Site: Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash Pre-Tax Charge for Impairment to Its North Brawley Geothermal Power Plant Author Ormat Technologies Inc. Published Publisher Not Provided, Date Not Provided DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash Pre-Tax Charge for Impairment to Its North Brawley Geothermal Power Plant Citation Ormat Technologies Inc.. Ormat Technologies Inc. Ormat Technologies, Inc. Announces a Non-Cash Pre-Tax Charge for Impairment to Its North Brawley

3

Ormat Technologies Inc. North Brawley, California USA | Open Energy  

Open Energy Info (EERE)

Ormat Technologies Inc. North Brawley, California USA Ormat Technologies Inc. North Brawley, California USA Jump to: navigation, search OpenEI Reference LibraryAdd to library Web Site: Ormat Technologies Inc. North Brawley, California USA Authors Ormat Technologies and Inc. Published Publisher Not Provided, Date Not Provided DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for Ormat Technologies Inc. North Brawley, California USA Citation Ormat Technologies, Inc.. Ormat Technologies Inc. North Brawley, California USA [Internet]. [updated 2013;cited 2013]. Available from: http://www.ormat.com/case-studies/north-brawley-california-usa Retrieved from "http://en.openei.org/w/index.php?title=Ormat_Technologies_Inc._North_Brawley,_California_USA&oldid=682480" Categories:

4

Ormat Technologies Inc | Open Energy Information  

Open Energy Info (EERE)

(Redirected from Ormat) (Redirected from Ormat) Jump to: navigation, search Name Ormat Technologies Inc Place Reno, Nevada Zip 89511-1136 Sector Geothermal energy Product Nevada-based, vertically integrated company primarily engaged in the geothermal and recovered energy power business. Coordinates 32.944065°, -97.578279° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":32.944065,"lon":-97.578279,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

5

Ormat Funding Corp | Open Energy Information  

Open Energy Info (EERE)

Ormat Funding Corp Ormat Funding Corp Jump to: navigation, search Name Ormat Funding Corp Place Sparks, Nevada Zip 89431 Sector Geothermal energy Product Primarily engaged in the geothermal power business. Coordinates 35.61145°, -96.821309° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":35.61145,"lon":-96.821309,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

6

Energy Department Finalizes Loan Guarantee for Ormat Geothermal...  

Energy Savers [EERE]

for Ormat Geothermal Project in Nevada Energy Department Finalizes Loan Guarantee for Ormat Geothermal Project in Nevada September 23, 2011 - 3:37pm Addthis Washington, D.C. - U.S....

7

BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project |  

Open Energy Info (EERE)

BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project Jump to: navigation, search OpenEI Reference LibraryAdd to library Report: BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project Abstract No abstract available. Author Bureau of Land Management Organization Bureau of Land Management, Carson City Field Office, Nevada Published U.S. Department of the Interior, 2011 DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project Citation Bureau of Land Management (Bureau of Land Management, Carson City Field Office, Nevada). 2011. BLM Fact Sheet- Ormat Technologies Salt Wells Geothermal Energy Project. Carson City, Nevada: U.S. Department of the

8

Ormat Technologies Inc | Open Energy Information  

Open Energy Info (EERE)

Jump to: navigation, search Jump to: navigation, search Name Ormat Technologies Inc Place Reno, Nevada Zip 89511-1136 Sector Geothermal energy Product Nevada-based, vertically integrated company primarily engaged in the geothermal and recovered energy power business. Coordinates 32.944065°, -97.578279° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":32.944065,"lon":-97.578279,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

9

Glass Buttes Exploration and Drilling: 2010 Geothermal Technologies Program Peer Review Presentation, Walsh, et al, Ormat  

SciTech Connect (OSTI)

Glass Buttes Exploration and Drilling: 2010 Geothermal Technologies Program Peer Review Presentation, Walsh, et al, Ormat

Ezra Zemach

2010-01-01T23:59:59.000Z

10

Energy Department Finalizes Loan Guarantee for Ormat Geothermal Project in  

Broader source: Energy.gov (indexed) [DOE]

Ormat Geothermal Ormat Geothermal Project in Nevada Energy Department Finalizes Loan Guarantee for Ormat Geothermal Project in Nevada September 23, 2011 - 3:37pm Addthis Washington, D.C. - U.S. Energy Secretary Steven Chu today announced the Department finalized a partial guarantee for up to a $350 million loan to support a geothermal power generation project. The project, sponsored by Ormat Nevada, Inc., is expected to produce up to 113 megawatts (MW) of clean, baseload power from three geothermal power facilities and will increase geothermal power production in Nevada by nearly 25 percent. The facilities are Jersey Valley in Pershing County, McGinness Hills in Lander County and Tuscarora in Elko County. The company estimates the project will fund 332 jobs during construction and 64 during operations.

11

EA-1849-S1: Phase II Facility - Ormat Tuscarora Geothermal Power...  

Energy Savers [EERE]

EA-1849-S1: Phase II Facility - Ormat Tuscarora Geothermal Power Plant in Tuscarora, NV EA-1849-S1: Phase II Facility - Ormat Tuscarora Geothermal Power Plant in Tuscarora, NV...

12

EA-1944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV  

Broader source: Energy.gov (indexed) [DOE]

944: Ormat Technologies Brady Hot Springs Project, Churchill 944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV EA-1944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV SUMMARY Ormat Technologies, Inc. (Ormat) proposes to use DOE and cost share funding to study the Brady Hot Springs geothermal Field 15-12RD well. This is an EGS Demonstration project divided into three phases. During Phase 1, Ormat characterized the target well to prepare for stimulation activities in Phase 2, Phase 2: Well Stimulation and Collection/Analysis of Stimulation Monitoring Data and Phase 3: Long-term testing of the system. Phase 2 and 3 activities would occur at Ormat's Brady Hot Springs geothermal field in Churchill County, NV on public lands managed by the Bureau of Land Management (BLM) and Bureau of Reclamation (BOR). Since Phases 2 and 3

13

EA-1944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV  

Broader source: Energy.gov (indexed) [DOE]

944: Ormat Technologies Brady Hot Springs Project, Churchill 944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV EA-1944: Ormat Technologies Brady Hot Springs Project, Churchill County, NV SUMMARY Ormat Technologies, Inc. (Ormat) proposes to use DOE and cost share funding to study the Brady Hot Springs geothermal Field 15-12RD well. This is an EGS Demonstration project divided into three phases. During Phase 1, Ormat characterized the target well to prepare for stimulation activities in Phase 2, Phase 2: Well Stimulation and Collection/Analysis of Stimulation Monitoring Data and Phase 3: Long-term testing of the system. Phase 2 and 3 activities would occur at Ormat's Brady Hot Springs geothermal field in Churchill County, NV on public lands managed by the Bureau of Land Management (BLM) and Bureau of Reclamation (BOR). Since Phases 2 and 3

14

MEMORANDUM OWNER(S)  

Office of Legacy Management (LM)

OWNER(S) OWNER(S) -------- past : Lb-J ' 0-c @+a+~-~% current: -- ________________________ ------7--- -- Owner cantacted 0 yes 4t no; if yes, date contacted TYPE OF OPERATION ----------------- q Research & Development 0 Facility Type 0 Production scale testing 0 Manufacturing 0 Pilat Scale 0 Bench Scale Process i Theoretical Studies Sample & Analysis 0 Production 0 Di5posal/Storage TYPE OF CONTRACT ----_----------- 0 Prime q Subcontractor Cl Purchase Order 0 University 0 Research Organization 0 Government Spohscred Facility 0 Other --------------------- . 0 Other information (i.e., cost + fixed fee, unit price, time 84 material, e,tc:) ------- 'Canfract/Purchase Order # --. CONTRACTING PERIOD: r4J~--___-----___---_____________ ----- OWNERSHIP:

15

Ormat's North Brawley plant with 17MW short of its 50MW potential | Open  

Open Energy Info (EERE)

Ormat's North Brawley plant with 17MW short of its 50MW potential Ormat's North Brawley plant with 17MW short of its 50MW potential Jump to: navigation, search OpenEI Reference LibraryAdd to library Web Site: Ormat's North Brawley plant with 17MW short of its 50MW potential Author Think Geoenergy Published Publisher Not Provided, Date Not Provided DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for Ormat's North Brawley plant with 17MW short of its 50MW potential Citation Think Geoenergy. Ormat's North Brawley plant with 17MW short of its 50MW potential [Internet]. [updated 40219;cited 2010]. Available from: http://thinkgeoenergy.com/archives/3654 Retrieved from "http://en.openei.org/w/index.php?title=Ormat%27s_North_Brawley_plant_with_17MW_short_of_its_50MW_potential&oldid=682479"

16

EA-1849: Department of Energy Loan Guarantee to Ormat Nevada, Inc. for a  

Broader source: Energy.gov (indexed) [DOE]

EA-1849: Department of Energy Loan Guarantee to Ormat Nevada, Inc. EA-1849: Department of Energy Loan Guarantee to Ormat Nevada, Inc. for a Geothermal Power Facility in Nevada EA-1849: Department of Energy Loan Guarantee to Ormat Nevada, Inc. for a Geothermal Power Facility in Nevada Overview Ormat Nevada Inc. (ORMAT), through its subsidiaries, proposes to construct and operate three geothermal power production facilities and associated power transmission lines in northern Nevada. The power production facilities include the Tuscarora Geothermal Power Plant Facility (Tuscarora Facility) in Elko County, the Jersey Valley Geothermal Development Facility (Jersey Valley Facility) in Pershing County, and the McGinness Hills Geothermal Facility (McGinness Hills Facility) in Lander County (Figure 1). The Hot Sulphur Springs Transmission Line (Transmission Line) would connect

17

OWNER(S) Past:  

Office of Legacy Management (LM)

--------------__ --------------__ CITY: ' -* -I c.l.&&!,Ck -------------------------- OWNER(S) ------__ Past: Owner contacted q yes current: -------------------------- if yea, date contacted ------_---___ TYPE OF OPERATION --------~~_~----_ q Research & Development 0 Production scale testing 0 Pilot Scale 0 Bench Scale Process,. 0 Theoretical Studies 0 Sample & Analysis 0 Production 0 Disposal/Storage 0 Facility Type a Manufacturing (I University, 0 Research Organization 0 Government Sponsored Facility 0 Other ~~~--~~~---~~~------_ TYPE OF CONTRACT ---_---__------_ 0 Prinie 0 Subcantractbr 0 Purchase Order 0 Other information (i.e., cast + fixed fee, unit price, time b material, qtc) ----'w-- ~~--~~-~~~----~~----________ Contract/Purchase ' Order

18

Draft Environmental Assessment Ormat Nevada Northern Nevada Geothermal Power Plant Projects  

Broader source: Energy.gov (indexed) [DOE]

9 9 FINAL ENVIRONMENTAL ASSESSMENT Ormat Nevada Northern Nevada Geothermal Power Plant Projects Department of Energy Loan Guarantee for ORMAT LLC's Tuscarora Geothermal Power Plant, Elko County, Nevada; Jersey Valley Geothermal Project, Pershing County, Nevada; and McGinness Hills Geothermal Project, Lander County, Nevada U.S. Department of Energy Loan Guarantee Program Office Washington, D.C. 20585 August 2011 NORTHERN NEVADA GEOTHERMAL POWER PLANT PROJECTS - ORMAT NEVADA AUGUST 2011 FINAL ENVIRONMENTAL ASSESSMENT i TABLE OF CONTENTS 1.0 INTRODUCTION.................................................................................................................1 1.1 SUMMARY AND LOCATION OF PROPOSED ACTION .....................................................1

19

SUBJECT: OWNER(S)  

Office of Legacy Management (LM)

HEHORANDUH HEHORANDUH ;;&; DC&b ------w--v SUBJECT: OWNER(S) -------- P1st a Owner contrctmd TYPE OF OPERATION ----------------- 0 Research I Development 0 Facility Type 0 Production scale testing 0 Pilot Scrlr 0 Bench Seal0 Procemm 0 Theoretical Studier 0 Sample & Anrlyri l 0 Production x Dimpomrl/Storrgr 0 Hmufrcturing 0 University 0 Rmsmarch Organization 0 Government Sponmored Facility 0 Other -II---------------- TYPE OF CONTRACT ----u---------- 0 d ime Subcontract& 0 Purchrre Order 0 Other information (i.e., comt -w-e--- Contrrct/Purchrsa Order 0 CONTRACTING PERIOD: ------------------ . OWNERSHIPa AEC/HED OWNED m---w LANDS 0 BUILDINSS 0 EQUIPMENT 0 ORE OR RAW HA-I-L 0 FINAL PRODUCT q WASTE & RESIDUE 0 AEC/HED LEASED ---w-w E 0 0

20

OWNER(S)  

Office of Legacy Management (LM)

l . . l . . ; * 3Tb'-j .I OWNER(S) rf yea, date contacted ___ TYPE OF OPERATION --~~----~---__--_ aResearch & Development q Facility Type 0 Production scale testing Et Pilot Scale q Hanufacturing 0 Bench Scale Process 0 University 0 Theoretical Studies 0 Research Organization Cl 0 Government Sponsored Facility Sample SC Analysis Cl Other --------__----___--_ 3 Production 1 Disposal/Storage TYPE OF CONTRACT --~_---__---____ m.p rime SC5 sLta4rM-J / Cl Subcqntractor 0 Purchase Order 0 Other information (i.e., cost + fixed fee, unit price? Contract/Purchase Order # ~~~ti~ --------------------_____________ AECf MED OWNED -_--_ LANDS BUILDINGS ' EQUIPMENT ORE OR RAW MATL [3 FINAL PRODUCT 0 WASTE & RESIDUE q GOVT OWNED ----- GOUT LEASED -----_ E

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


21

OWNER(S)  

Office of Legacy Management (LM)

------ - ------ - Past: ~~~-~~~-~~~~~~~~~~rrent: Owner contacted q yes tina;-. ____ c-lti&pJ-~ lf yes, date contacted -_---__---___ TYPE OF OPERATION -_-----_--_--____ q Research & Development 0 Production scale testing 0 Pilot Scale 0 Bench Scale Process : 'Theoretical Studier Sample & Analysis G Production 0 Disposal/Storage TYPE OF CONTRACT ~-~~~----~~----_ &, Facility Type q Manufacturing 0 University a Research Organizaticn a Other information (i.e., cost + fixed fee,, unit price, -_---- yryoi -37 J-1 4:~zL~~:~:q~&- ,-antract,purchase Order # ,L,U,-37-?\- ---------------------------- --------------------_____________ my~mx~~ai_~Gi~~~Q : _I 7 v 3 _ I 9 V-Y, ---_--_------------------------------ OWNERSHIP: AEC/MED AEC/MED GOUT GOUT

22

OWNER(S)  

Office of Legacy Management (LM)

_----- _----- past: %J +c - fl*+;o.rrq -____------------- Owner contacted 0 yes Curr@nt: ______ -----------L-----l- if yes, date contacted TYPE OF OPERATION Reeearch & Development 0 Facility Type 0 Production scale testing Cl Pilot Scale 0 Bench Scale Process 0 0 Research Organization Theoretical Studies 0 0 Government Sponsored Facility ~ ~*a;~a.a~~plysis 0 Other ~~~~~~~~------____--- 0 Production 0 DispdsalfStoraqe TYPE OF CONTRACT ---------------- 0 Prime 0 Subcontractor 0 Purchase Order 0 Other information (i.e., cost + fixed fee, unit price, time & mater!&, etc) ------- --------------------LA------ ~~------------~~~-~--------- Contract/Purchase Order # ~-----~-~~~~~~~--~~~_____________ CONTRACTING PERIOD: f?Ar! lts' d' ------------------ ___-_ +----a-

23

ORNI 9, LLC, AND ORMAT NEVADA INC. APPLICATIONS FOR PERMIT TO DRILL  

Broader source: Energy.gov (indexed) [DOE]

ORNI 9, LLC, AND ORMAT NEVADA INC. ORNI 9, LLC, AND ORMAT NEVADA INC. APPLICATIONS FOR PERMIT TO DRILL GEOTHERMAL OBSERVATION WELLS 82-14 AND 55-14 AND GEOTHERMAL PRODUCTION WELL 15-12 AND POSSIBLE FUTURE GEOTHERMAL WELLS LOCATED IN SECTIONS 12, and 14, T22N, R26E, MDB&M BLM Geothermal Leases NVN-065558 and NVN-065561 BLM Environmental Assessment No. NV-020-05-07 CONDITIONS OF APPROVAL 1. This approval is contingent upon the lessee/operator being in receipt of and in compliance with all appropriate federal, state, and local permits. 2. When cultural or paleontological resources, including but not limited to historic ruins, prehistoric artifacts and fossils, are discovered in the performance of the permit, the resources shall be left intact and immediately brought to the attention of the BLM authorized officer.

24

Information System Owner | Department of Energy  

Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

Owner Information System Owner The Information System Owner (also referred to as System Owner) is the individual responsible for the overall procurement, development, integration,...

25

TO: FILE MEMORANDUM SUBJECT: ALTERNATE OWNER(S)  

Office of Legacy Management (LM)

SUBJECT: SUBJECT: ALTERNATE OWNER(S) -__----- Owner csntacted r~ yes current: --------------------A----- if yes, date contacted TYPE OF OPERATION ------------_____ Research & Development 0 Facility Type 0 Production seal e testing 0 Pilot Scale 0 Bench Scale Process i Theoretical Studi es Sample & Analysis Producti on Di spas.31 /Storage a' Manufacturing q University 0 Research Organization 0 Government Sponsored Facility Cl Other ~~~~~~~----~~-------- 0 0 Prime q Other information (i.e., cast 0 Subcontractor 0 'Purchase Order + fixed fee, unit piice, pi time & material, gtc) ~~-----_------~~_-------~-~- .Contract./Purchaee Order # fi~k~ti;3 -----------_---------------- CONTRACTING PEXIOD: tit-k ------------------ would -------------------------------------

26

User_OrgOwner_Overview  

Broader source: Energy.gov (indexed) [DOE]

Organization Owner Overview Organization Owner Overview © 2011 SuccessFactors, Inc. - 1 - SuccessFactors Learning Confidential. All rights reserved. Job Aid: Organization Owner Overview Purpose The purpose of this job aid is to guide organization owners through the step-by-step process of available features within SuccessFactors Learning. The organization dashboard is a collection of charts and data tables that summarize learning data for your organizations and sub-organizations. Note: Depending on how permissions were configured in, access to the following features will vary for each organization. Task A. Organization Dashboard From the Home page, roll-over the Organization tab and select Dashboard from the list. 1 1 Succession Planner 7 Steps

27

Owners of nuclear power plants  

SciTech Connect (OSTI)

Commercial nuclear power plants in this country can be owned by a number of separate entities, each with varying ownership proportions. Each of these owners may, in turn, have a parent/subsidiary relationship to other companies. In addition, the operator of the plant may be a different entity as well. This report provides a compilation on the owners/operators for all commercial power reactors in the United States. While the utility industry is currently experiencing changes in organizational structure which may affect nuclear plant ownership, the data in this report is current as of July 1996. The report is divided into sections representing different aspects of nuclear plant ownership.

Hudson, C.R.; White, V.S.

1996-11-01T23:59:59.000Z

28

Olkaria III Geothermal Power Plant | Open Energy Information  

Open Energy Info (EERE)

Type Single Flash Owner Ormat Technologies, Inc. Developer Ormat Technologies, Inc. Energy Purchaser Kenya Power and Lighting Company Limited Commercial Online Date 2014...

29

Institutional owners and competitive rivalry  

E-Print Network [OSTI]

strategies for gaining advantage over their rivals. As such, scholars have sought to measure competitive rivalry in order to study factors that influence it. Industry rivals constitute a particularly appropriate arena for competitive dynamics research... that these owners can and do affect broad strategies, there is little empirical support for the extent to which institutional investors involve themselves at the level of strategic competitive actions that firms undertake. This raises the question: How do...

Connelly, Brian Lawrence

2008-10-10T23:59:59.000Z

30

Property:Owners | Open Energy Information  

Open Energy Info (EERE)

Owners Owners Jump to: navigation, search Property Name Owners Property Type Page Description A unique list of owners of all power plants in the area. Automatically populated using ask query on Property: Owner of Category: Energy Generation Facility with property InGeothermalResourceArea set to the the variable vName of the Geothermal Resource Area Subproperties This property has the following 301 subproperties: A Abraham Hot Springs Geothermal Area Adak Geothermal Area Akun Strait Geothermal Area Akutan Fumaroles Geothermal Area Alum Geothermal Area Alvord Hot Springs Geothermal Area Arrowhead Hot Springs Geothermal Area Ashton Warm Springs Geothermal Area Astor Pass Geothermal Area Augusta Mountains Geothermal Area B Bailey Bay Hot Springs Geothermal Area Baker Hot Spring Geothermal Area

31

Danish Wind Turbine Owners Association | Open Energy Information  

Open Energy Info (EERE)

Owners Association Owners Association Jump to: navigation, search Name Danish Wind Turbine Owners' Association Place Aarhus C, Denmark Zip DK-8000 Sector Wind energy Product Danish Wind Turbine Ownersâ€(tm) Association is a non-profit, independent association overseeing wind turbine ownersâ€(tm) mutual interests regarding the authorities, political decision-makers, utilities and wind turbine manufacturers. References Danish Wind Turbine Owners' Association[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Danish Wind Turbine Owners' Association is a company located in Aarhus C, Denmark . References ↑ "Danish Wind Turbine Owners' Association" Retrieved from "http://en.openei.org/w/index.php?title=Danish_Wind_Turbine_Owners_Association&oldid=344068

32

Tips For Residential Heating Oil Tank Owners  

E-Print Network [OSTI]

· · · · · · · · · · · · · · · · · · · · · · Tips For Residential Heating Oil Tank Owners Source: DEP Fact Sheet Residential heating oil tanks are used to store fuel for furnaces or boilers to heat homes. The tanks can either be aboveground tanks, normally located in basements or utility rooms

Maroncelli, Mark

33

Owner/contractor work structure process with integrated alignment framework  

E-Print Network [OSTI]

appropriate use, strategically, of owner resources in working relationships with contractors to successfully develop and execute projects and to achieve corporate and project objectives recognizing less owner engineering resources. This work process...

Sullivan, George Ray

1996-01-01T23:59:59.000Z

34

TO: FILE GiR FROM: SUBJECT: I OWNER(S) Past: Current:  

Office of Legacy Management (LM)

3 749 3 749 '*,. .,;L ----.-. _ 5' . iMEMORANDUM TO: FILE GiR FROM: , SUBJECT: I OWNER(S) ------__ Past: ------------------_----~ Current: Owner contacted q yes qnnc; ~~-~~~---------~~--_______ if yes, date contacted 1 ! I TYPE OF OPERATION --~_--___~---_--_ $ Research b Development a Facility Type 1 I 0 Production scale testing 0 Pilot Scale Bench Scale Process Theoretical 'Studies 0 Sample & Analysis G Production E Disposal/Storage 0 Research 0 Uther --------------T------ I T'/PE OF CONTRACT -----------_____ 0 Prime I2 C! Subcontractor Other information (i.e.:, cost q Purchase Order + fixed fee, unit Arice, time 84 material, etr) i ------- 'I ----------------------i__--_ Contract/Purchase Qrdei. W -----------I--k---j----- ~PJKJbL-I @J OWNERSHIP:

35

CYBERSECURITY FUNDAMENTALS FOR SMALL BUSINESS OWNERS Shirley Radack, Editor  

E-Print Network [OSTI]

CYBERSECURITY FUNDAMENTALS FOR SMALL BUSINESS OWNERS Shirley Radack, Editor Computer Security and Technology (NIST) recently issued a new guide that tailors basic information on cybersecurity to the specific

36

Rights and Duties of Mines and Mine Owners, General (Missouri)  

Broader source: Energy.gov [DOE]

This legislation addresses general operational guidelines for mine owners regarding public notices, fees, land and mineral ownership, requirements for mining in certain municipalities, and mining...

37

Property:Owner | Open Energy Information  

Open Energy Info (EERE)

property of type Page. property of type Page. Subproperties This property has the following 1 subproperty: G GRR/Section 4-FD-a - Exploration Permit BLM Pages using the property "Owner" Showing 25 pages using this property. (previous 25) (next 25) A AB Tehachapi Wind Farm + Coram Energy + AFCEE MMR Turbines + AFCEE + AG Land 1 + AG Land Energy LLC + AG Land 2 + AG Land Energy LLC + AG Land 3 + AG Land Energy LLC + AG Land 4 + AG Land Energy LLC + AG Land 5 + AG Land Energy LLC + AG Land 6 + AG Land Energy LLC + AVTEC + AVTEC + Aberdeen Biomass Facility + Sierra Pacific Industries + Adair Wind Farm I + Shafer Systems + Adair Wind Farm II + MidAmerican Energy + Aero Turbine + AeroTurbine Energy Company + Aeroman Repower Wind Farm + Coram Energy + Affinity Wind Farm + Affinity Wind LLC +

38

Ship-owners' decisions to outsource vessel management  

E-Print Network [OSTI]

of domiciliation, number of vessels). In addition, a specific country effect is identified for Greek shipEA 4272 Ship-owners' decisions to outsource vessel management Pierre Cariou* Francois-Charles Wolff,version1-17May2011 #12;Ship-owners' decisions to outsource vessel management Pierre CARIOU Corresponding

Paris-Sud XI, Université de

39

Tips for Renters and Property Owners | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

Tips for Renters and Property Owners Tips for Renters and Property Owners Tips for Renters and Property Owners July 5, 2012 - 4:51pm Addthis Tips for Renters and Property Owners If you rent, or if you own a rental unit, you can use many of the tips throughout this guide to save money and energy. Renters You can reduce your utility bills by following the tips in these sections: Lighting Heating and Cooling (if you control the thermostat) Appliances Home Office and Home Electronics Windows Transportation Encourage your landlord to follow these tips as well. They'll save energy and money, improving your comfort and lowering your utility bills even more. Property Owners Nearly all of the information in this guide applies to rental units. The section on Your Home's Energy Use focuses on air leaks, insulation, heating

40

Visiting With Santa Fe Small Business Owners | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

Visiting With Santa Fe Small Business Owners Visiting With Santa Fe Small Business Owners Visiting With Santa Fe Small Business Owners May 10, 2012 - 9:02am Addthis Dot Harris Dot Harris The Honorable Dot Harris, Director, Office of Economic Impact and Diversity You've got to do your homework in order to contract with the federal government. Whether you are a large or small business owner, learning the ins and outs of government contracting takes dedication, perseverance, and taking advantage of opportunities to meet face-to-face with procurement experts and other businesses. That's where our Small Business Roundtables, Business Opportunity Sessions, conference booths, and Regional Small Business Summits come in. We want to meet directly with small business owners, managers, and staffers, to hear what you need to learn from us to make the contracting

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


41

Guide to Combined Heat and Power Systems for Boiler Owners and...  

Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

Guide to Combined Heat and Power Systems for Boiler Owners and Operators, July 2004 Guide to Combined Heat and Power Systems for Boiler Owners and Operators, July 2004 Many owners...

42

"Table HC3.10 Home Appliances Usage Indicators by Owner-Occupied...  

U.S. Energy Information Administration (EIA) Indexed Site

0 Home Appliances Usage Indicators by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing...

43

Microsoft Word - 2.9 Chemical Owners 0913.docx  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Chemical Owners Chemical Owners AFRD Line Management personnel who authorize the use of chemicals in their group's work retain responsibility for ensuring that the chemicals are properly inventoried, labeled, stored, used, and disposed. They may choose to remain Chemical Owners as described in the LBNL Chemical Hygiene and Safety Plan and manage the chemicals themselves, or delegate chemical management tasks to appropriately trained AFRD or matrixed personnel who have knowledge of the chemicals' hazards, controls, and procedures for using and storing them safely. The chemical inventory for each AFRD work area must be maintained on the Chemical Management System. When chemical management tasks are delegated, the AFRD Line Management personnel must also

44

Guide to Combined Heat and Power Systems for Boiler Owners and...  

Broader source: Energy.gov (indexed) [DOE]

Combined Heat and Power Systems for Boiler Owners and Operators Guide to Combined Heat and Power Systems for Boiler Owners and Operators This guide presents useful information for...

45

Business Owners: Prepare a Business Recovery Plan | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

a Business Recovery Plan a Business Recovery Plan Business Owners: Prepare a Business Recovery Plan Business Owners: Prepare a Business Recovery Plan Smart business owners develop and test a written business recovery plan to support them through disasters and help them stay in operation. Planning ahead will help your company get back to business more quickly. Consider your risks-How might a disaster affect your business operations? What natural disasters are most likely where you operate? Identify your critical business functions-What resources and personnel will you need to restore or reproduce these functions during a recovery? Assign disaster response duties to your employees. Identify critical suppliers-Identify suppliers, providers, shippers, resources, and other businesses you typically interact with and

46

Energy Efficiency: Helping Home Owners and Businesses Understand Energy  

Broader source: Energy.gov (indexed) [DOE]

Efficiency: Helping Home Owners and Businesses Understand Efficiency: Helping Home Owners and Businesses Understand Energy Usage Energy Efficiency: Helping Home Owners and Businesses Understand Energy Usage November 7, 2013 - 3:55pm Addthis Building 90, an 89,000-square foot office building at Berkeley Lab, served as the commercial setting for the miscellaneous and electronic loads (MELs) study. 460 meters were placed throughout the building to serve as a representative sample of a wide range of device types. | Photo courtesy of Berkeley Lab. Building 90, an 89,000-square foot office building at Berkeley Lab, served as the commercial setting for the miscellaneous and electronic loads (MELs) study. 460 meters were placed throughout the building to serve as a representative sample of a wide range of device types. | Photo courtesy of

47

Realities of Chiller Plant Operation: Utility Impacts on Owner Operating  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Realities of Chiller Plant Operation: Utility Impacts on Owner Operating Realities of Chiller Plant Operation: Utility Impacts on Owner Operating Costs and Societal Environmental Issues Speaker(s): Don Aumann Date: March 21, 2000 - 12:00pm Location: Bldg. 90 Seminar Host/Point of Contact: Satkartar K. Kinney Don Aumann, a Senior Consultant from BKi in Oakland, will present an overview of two projects he completed for the electric utility industry. The first, a case study evaluation of a hybrid chiller plant in Jefferson City, Missouri, demonstrates the importance of carefully evaluating the impact of utility rate structures on plant operating costs. The building owner, another engineering consultant, and the local utility representatives were confused by the rates and missed an opportunity to cut chiller-plant operating costs by about 20%, totaling $15,000 per year. In

48

Business Owners: Respond to an Energy Emergency | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

Respond to an Energy Emergency Respond to an Energy Emergency Business Owners: Respond to an Energy Emergency Business Owners: Respond to an Energy Emergency Ensure your building is safe to occupy-Initially allow only essential, critical-operations staff into restricted areas. Ask your local or State health department for guidance on determining the safety of your building. Decide whether to activate backup power-If your backup generator doesn't automatically turn on during a power outage, you'll have to determine when to activate backup systems. First determine whether power is likely to be restored within 24 hours. If not, you may want to activate those systems to protect your business assets. Learn more Contact your fuel supplier-If you rely on fuel supplies for your business, vehicles, generators, and other equipment, contact your fuel

49

Business Owners: Prepare for Fuel Shortages | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

Fuel Shortages Fuel Shortages Business Owners: Prepare for Fuel Shortages Business Owners: Prepare for Fuel Shortages You may need fuel for vehicles, generators, and other equipment to continue operating your business during an emergency. During a shortage, local authorities and fuel suppliers will prioritize getting fuel to key assets such as emergency operations centers, hospitals, food supply dealers, water supply plants, and telecommunication networks. Plan ahead to help make sure you have adequate supplies. Review your fuel supply contracts-Arrange priority contacts with fuel suppliers, including an out-of-region supplier, and include language for providing fuel supplies during an emergency. Can your fuel suppliers operate with no power? Do they have gravity-fed systems? What if your fuel

50

Business Owners: Prepare for Utility Disruptions | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

for Utility Disruptions for Utility Disruptions Business Owners: Prepare for Utility Disruptions Business Owners: Prepare for Utility Disruptions Have a plan in place in case a natural disaster or other hazard knocks out your business's electricity or natural gas service. Identify energy utilities-The utilities that are absolutely necessary to running your business. How might a disaster impact the availability of those utilities? Determine backup options-Contact your utility companies to discuss potential backup options, such as portable generators to provide power. Learn how and when to turn off utilities-For example, if you turn off your natural gas, a professional technician must turn it back on. Learn more Consider using backup generators-Generators can power the most important aspects of your business in an emergency. This will involve:

51

River resort owners find LPG a power behind their success  

SciTech Connect (OSTI)

This paper reports on a restaurant and resort which runs entirely on LPG. It has two generators converted to LPG that supply the power for the complex. Energy supplied from the propane is used in the kitchens, to drive the water pump and provide electricity for lighting and other power needs, and to heat the swimming pool. Far more importantly for the owners has been the fuel cost savings of at least 60%.

Not Available

1991-01-01T23:59:59.000Z

52

The B & W Owners` Group Generic License Renewal Program  

SciTech Connect (OSTI)

Since the late 1970s, the Babcock & Wilcox (B & W) Owners Group (BWOG) has sponsored significant activities that address technical, economic, and licensing issues to ensure that the B & W nuclear steam supply system (NSSS) power plants operate until the end of their current plant licensed life and to preserve the license renewal option. It should be no surprise that the BWOG decided in late 1992 to aggressively pursue a license renewal effort. This effort, the Generic License Renewal Program (GLRP), has over the past 18 months contributed significantly to the industry`s license renewal initiative. The GLRP was established as a project with a full-time management organization within the BWOG structure. Its primary objective was the development and demonstration of an integrated plant assessment (IPA) process that would meet the requirements of the License Renewal Rule, published by the US Nuclear Regulatory Commission (NRC) in December 1991. The BWOG consists of five utilities with plants of very similar design, operation, and age. The owners, along with technical support from B & W Nuclear Technologies, created a highly capable and effective team to address the elements of the license renewal rule. This paper presents the BWOG strategy from the beginning of the program, the accomplishments to date, and the current role of the BWOG GLRP.

Gill, R.L. Jr.

1994-12-31T23:59:59.000Z

53

Physics of Binary Information  

E-Print Network [OSTI]

Basic concepts of theoretical particle physics, including quantum mechanics and Poincar\\'e invariance, the leptonic mass spectrum and the proton mass, can be derived, without reference to first principles, from intrinsic properties of the simplest elements of information represented by binary data. What we comprehend as physical reality is, therefore, a reflection of mathematically determined logical structures, built from elements of binary data.

Walter Smilga

2005-05-05T23:59:59.000Z

54

Very Cool Close Binaries  

E-Print Network [OSTI]

We present new observations of cool <6000K and low mass <1Msun binary systems that have been discovered by searching several modern stellar photometric databases. The search has led to a factor of 10 increase in the number of known cool close eclipsing binary systems.

J. Scott Shaw; Mercedes Lopez-Morales

2006-03-28T23:59:59.000Z

55

Gamma-ray binaries  

E-Print Network [OSTI]

Recent observations have shown that some compact stellar binaries radiate the highest energy light in the universe. The challenge has been to determine the nature of the compact object and whether the very high energy gamma-rays are ultimately powered by pulsar winds or relativistic jets. Multiwavelength observations have shown that one of the three gamma-ray binaries known so far, PSR B1259-63, is a neutron star binary and that the very energetic gamma-rays from this source and from another gamma-ray binary, LS I +61 303, may be produced by the interaction of pulsar winds with the wind from the companion star. At this time it is an open question whether the third gamma-ray binary, LS 5039, is also powered by a pulsar wind or a microquasar jet, where relativistic particles in collimated jets would boost the energy of the wind from the stellar companion to TeV energies.

I. F. Mirabel

2006-10-24T23:59:59.000Z

56

Which idling reduction system is most economical for truck owners?  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Which idling reduction system is Which idling reduction system is most economical for truck owners? Linda Gaines Center for Transportation Research Argonne National Laboratory Commercial Vehicle Engineering Congress and Exposition Rosemont, Il October 7-9, 2008 The price of diesel is high *Idling a Class 8 truck uses 0.6-1.2 gallons per hour *That can total over $50 a night! *So even without regulations, there's an incentive to reduce idling *Even if the price goes down more, idling reduction makes sense 2 Why do sleepers idle overnight? For services to resting driver and friend y Heating, ventilation, and air conditioning (HVAC) y Power for appliances 8TV, microwave, refrigerator, computer, hair drier To keep fuel and engine warm To mask out noises and smells Because other drivers do it

57

DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec  

Broader source: Energy.gov (indexed) [DOE]

NSTB Researchers Demonstrate R&D Successes to Asset Owners at NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference More than 150 energy sector leaders-including nearly 100 asset owners and operators-gathered at the 2009 EnergySec Annual Summit in Seattle, WA, on Sept. 23-24, where researchers from the Department of Energy's National SCADA Test Bed (NSTB) Program gave a four-hour demonstration and presentation of their Roadmap-related control systems security work. DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference More Documents & Publications DOE/OE National SCADA Test Bed Fiscal Year 2009 Work Plan Security is Not an Option DOE National SCADA Test Bed Program Multi-Year Plan

58

DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec  

Broader source: Energy.gov (indexed) [DOE]

DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference October 1, 2009 - 1:26pm Addthis More than 150 energy sector leaders-including nearly 100 asset owners and operators-gathered at the 2009 EnergySec Annual Summit in Seattle, WA, on Sept. 23-24, where researchers from the Department of Energy's National SCADA Test Bed (NSTB) Program gave a four-hour demonstration and presentation of their Roadmap-related control systems security work. EnergySec is an information sharing forum with more than 230 utility members representing 75 energy companies across the nation. Its fifth annual conference drew asset owners, vendors, and government

59

DOE/NNSA Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

Facility Management Contracts Facility Management Contracts Facility Owner Contractor Award Date End Date Options/Award Term Ultimate Potential Expiration Date Contract FY Competed Parent Companies/ LLC Partners DOE Site Procurement Director DOE Contracting Officer SLAC National Accelerator Laboratory (SLAC) SC Stanford University DE-AC03-76SF00515 1/25/1981 9/30/2017 9/30/2017 M&O 1981 Stanford University Barbara Jackson 865-576-0976 Kyong H. Watson 650-926-5203 Pacific Northwest National Laboratory (PNNL) SC Battelle Memorial Institute DE-AC05-76RL01830 12/30/2002 9/30/2017 9/30/2017 M&O 1965 Battelle Memorial Institute Barbara Jackson 865-576-0976 Ryan Kilbury 509-372-4030 Brookhaven National Laboratory (BNL) SC Brookhaven Science Associates, LLC DE-AC02-98CH10886 1/5/1998 1/4/2015 1/4/2015 M&O 1998 Battelle Memorial Institute

60

DOE/NNSA Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

Facility Management Contracts Facility Management Contracts Facility Owner Contractor Award Date End Date Options/Award Term Ultimate Potential Expiration Date Contract FY Competed Parent Companies/ LLC Partners DOE Site Procurement Director DOE Contracting Officer SLAC National Accelerator Laboratory (SLAC) SC Stanford University DE-AC03-76SF00515 1/25/1981 9/30/2017 9/30/2017 M&O 1981 Stanford University Barbara Jackson 865-576-0976 Kyong H. Watson 650-926-5203 Pacific Northwest National Laboratory (PNNL) SC Battelle Memorial Institute DE-AC05-76RL01830 12/30/2002 9/30/2017 9/30/2017 M&O 1965 Battelle Memorial Institute Barbara Jackson 865-576-0976 Ryan Kilbury 509-372-4030 Brookhaven National Laboratory (BNL) SC Brookhaven Science Associates, LLC DE-AC02-98CH10886 1/5/1998 1/4/2015 1/4/2015 M&O 1998 Battelle Memorial Institute

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


61

SharePoint 2010 Security for the Site Owner: and for Administrators and Developers!, 1st edition  

Science Journals Connector (OSTI)

Finally a SharePoint security book for the Site Owner! There are many books for administrators, but few for the Site Owner. This one is for you, the SharePoint Site Collection Administrator, Site Owner and the SharePoint power user. It's also for the ...

Michael T. Smith

2014-07-01T23:59:59.000Z

62

Letter of Intent: Commercial Real Estate Developer/Owner | ENERGY STAR  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Letter of Intent: Commercial Real Estate Developer/Owner Letter of Intent: Commercial Real Estate Developer/Owner Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In This Section Campaigns Commercial building design Communications resources Energy management guidance Financial resources Portfolio Manager Products and purchasing Recognition Research and reports Service and product provider (SPP) resources

63

Hypervelocity binary stars: smoking gun of massive binary black holes  

E-Print Network [OSTI]

The hypervelocity stars recently found in the Galactic halo are expelled from the Galactic center through interactions between binary stars and the central massive black hole or between single stars and a hypothetical massive binary black hole. In this paper, we demonstrate that binary stars can be ejected out of the Galactic center with velocities up to 10^3 km/s, while preserving their integrity, through interactions with a massive binary black hole. Binary stars are unlikely to attain such high velocities via scattering by a single massive black hole or through any other mechanisms. Based on the above theoretical prediction, we propose a search for binary systems among the hypervelocity stars. Discovery of hypervelocity binary stars, even one, is a definitive evidence of the existence of a massive binary black hole in the Galactic center.

Youjun Lu; Qingjuan Yu; D. N. C. Lin

2007-07-12T23:59:59.000Z

64

MOTION TO INTERVENE OF THE NEW YORK TRANSMISSION OWNERS PP-230-4 |  

Broader source: Energy.gov (indexed) [DOE]

MOTION TO INTERVENE OF THE NEW YORK TRANSMISSION OWNERS PP-230-4 MOTION TO INTERVENE OF THE NEW YORK TRANSMISSION OWNERS PP-230-4 MOTION TO INTERVENE OF THE NEW YORK TRANSMISSION OWNERS PP-230-4 Pursuant to Rules 212 and 214 of the Rules of Practice and Procedure, 18 C.F.R. §§ 385.212 and 385.214 (2010), Central Hudson Gas & Electric Corporation, Consolidated Edison Company of New York, Inc., Long Island Power Authority, New York Power Authority, New York State Electric & Gas Corporation, Niagara Mohawk Power Corporation d/b/a National Grid, Orange and Rockland Utilities, Inc., and Rochester Gas and Electric Corporation (referred to herein as the "New York Transmission Owners"), individually and collectively move to intervene in the above-captioned proceeding and request an opportunity to comment on International Transmission Company's d/b/a/ ITCTransmission

65

Calculating the Financial Benefits of an Energy Efficiency Project: The Building Owner's and Invester's Perspective  

E-Print Network [OSTI]

CALCULATING THE FINANCIAL BENEFITS OF AN ENERGY EFFICIENCY PROJECT: THE BUILDING OWNER'S AND INVESTOR'S PERSPECTIVES James K. Watson, P.E. Energy Investment, Inc. Boston, Massachusetts ABSTRACT Recognizing that energy costs are controllable...CALCULATING THE FINANCIAL BENEFITS OF AN ENERGY EFFICIENCY PROJECT: THE BUILDING OWNER'S AND INVESTOR'S PERSPECTIVES James K. Watson, P.E. Energy Investment, Inc. Boston, Massachusetts ABSTRACT Recognizing that energy costs are controllable...

Watson, J. K.

66

A comparison of noxious facilities` impacts for home owners versus renters  

SciTech Connect (OSTI)

The siting of noxious facilities, such as hazardous waste facilities, is often vigorously opposed by local residents, and thus it is now common for local residents to be compensated for the presence of the facility. One technique that has been employed to implicitly value noxious facilities is the intercity hedonic approach, which examines the wage and land rent premia between cities that result from the presence of the facility. However, most of the focus has been on the behavior of home owners as opposed to renters. Since these two groups of residents vary on numerous dimensions such as marital status, age, sex, and personal mobility, it would not be surprising to find different marginal valuations of local site characteristics. The authors use 1980 Census data to derive separate estimates for owners and renters of the implicit value placed on eight different types of noxious facilities. They find that renters and owners differ in their response to noxious facilities, although the differences are not systematic. Furthermore, the differences between owners and renters are not primarily due to differential mobility or socio-demographic factors. Controlling those factors decreases the differences between renters` and owners` implicit valuations of noxious facilities by less than 10%. Unmeasured differences between the two groups, such as tastes, risk aversion, or commitment to the community, must account for the remaining difference in valuations. These findings suggest that policymakers should separately consider the responses of owners and renters when estimating noxious facility impacts.

Clark, D.E. [Marquette Univ., Milwaukee, WI (United States). Dept. of Economics]|[Argonne National Lab., IL (United States); Nieves, L.A. [Argonne National Lab., IL (United States)

1995-01-01T23:59:59.000Z

67

X-ray binaries  

E-Print Network [OSTI]

We review the nuclear astrophysics aspects of accreting neutron stars in X-ray binaries. We summarize open astrophysical questions in light of recent observations and their relation to the underlying nuclear physics. Recent progress in the understanding of the nuclear physics, especially of X-ray bursts, is also discussed.

H. Schatz; K. E. Rehm

2006-08-01T23:59:59.000Z

68

Secretaries Chu and Donovan to Host Conference Call on Home Owners  

Broader source: Energy.gov (indexed) [DOE]

Donovan to Host Conference Call on Home Owners Donovan to Host Conference Call on Home Owners Energy-Saving Improvements Program Secretaries Chu and Donovan to Host Conference Call on Home Owners Energy-Saving Improvements Program April 20, 2011 - 12:00am Addthis WASHINGTON - Thursday, April 21st, U.S. Department of Energy Secretary Steven Chu and U.S. Housing and Urban Development Secretary Shaun Donovan will launch a new pilot program intended to offer homeowners low-cost financing to help make their homes more energy efficient. The Federal Housing Administration's (FHA) new PowerSaver Program will offer homeowners up to $25,000 to finance the installation of insulation, duct sealing, replacement doors and windows, HVAC systems, water heaters, solar panels, and geothermal systems. Donovan and Chu will speak with reporters following a tour of a local

69

Step 8: Work with the building owner to complete the ENERGY STAR lifecycle  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

8: Work with the building owner to complete the ENERGY STAR 8: Work with the building owner to complete the ENERGY STAR lifecycle Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Why you should design to earn the ENERGY STAR Follow EPA's step-by-step process Step 1: Assemble a team Step 2: Set an energy performance target Step 3: Evaluate your target using ENERGY STAR tools Step 4: Design to be energy efficient

70

REVIEW OF TRANSAMERICA DELAVAL INC. DIESEL GENERATOR OWNERS' GROUP ENGINE REQUALIFICATION PROGRAM  

SciTech Connect (OSTI)

In December 1983, 13 nuclear utilities that own TDI diesel generators formally established an Owners Group to address concerns regarding the reliability and operability of these engines. The Owners' Group program for engine requalification consisted of four major elements: 1) resolution of known problems with potentially generic implications, 2) a design review and quality revalidation (DR/QR) effort aimed at identifying and correcting potential problems with the important engine components, 3) expanded engine testing and inspection, and 4) enhanced engine maintenance and surveillance (M/S) to maintain the qualification of the diesel engines for the lifetime of the nuclear plants that they service. In providing technical support to NRC, the PNL project staff, assisted by a number of diesel engine consultants, focused on the four major elements of the Owners' Group engine requalification program, addressing both generic and plant-specific areas.

Berlinger, C. H.

1985-12-01T23:59:59.000Z

71

A comparison of noxious facilities` impacts for home owners versus renters  

SciTech Connect (OSTI)

The siting of noxious facilities, such as hazardous waste facilities, is often vigorously opposed by local residents. As a result, one would expect people`s residential and employment choices to reflect a desire to avoid proximity to such facilities. Ibis behavior would in turn affect labor and housing prices. One technique that has been employed to implicitly value impacts of noxious facilities is the intercity hedonic approach, which examines the wage and land rent differentials among cities that result from environmental amenities and disamenities. However, most of the research focus has been on the behavioral response of home owners as opposed to renters. Since these two groups of residents vary on numerous dimensions such as marital status, age, sex, and personal mobility, it would not be surprising to find different marginal valuations of local site characteristics. We use 1980 Census data to derive separate estimates for owners and renters of the implicit value placed on eight different types of noxious facilities. Although the magnitude of the responses of renters and owners to noxious facilities and other environmental characteristics varies, the signs are generally consistent. The differences in values between owners and renters are not primarily due to differential mobility or sociodemographic factors. Controlling those factors decreases the differences between renters` and owners` implicit valuations by less than 10%. Unmeasured differences in characteristics between the two groups, such as tastes, risk aversion, or commitment to the community, must account for the remaining difference in valuations. These findings suggest that policymakers should separately consider the responses of owners and renters when estimating noxious facility impacts.

Clark, D.E. [Marquette Univ., Milwaukee, WI (United States). Dept. of Economics]|[Argonne National Lab., IL (United States); Nieves, L.A. [Argonne National Lab., IL (United States)

1996-09-01T23:59:59.000Z

72

Locating Restricted Facilities on Binary Maps  

E-Print Network [OSTI]

welfare optimization, when the area map is encoded as a binary (0,1) mxn matrix. ... of connected components in binary maps and in Section 7 we conclude.

Mugurel

2008-09-20T23:59:59.000Z

73

Hyperbolic capture of compact binaries  

E-Print Network [OSTI]

Hyperbolic encounters of compact objects are common interactions in dense environments. During this process a significant amount of gravitational radiation is emitted depending on the parameters of the system. Here we give a parametric description of the radial motion valid for general binary orbits and the radiative energy and angular momentum losses for binaries with spinning components.

Mtys Vasth

2014-09-23T23:59:59.000Z

74

Evolutionary Memory in Binary Systems?  

E-Print Network [OSTI]

Correlation between the spins (rotational velocities) in binaries has previously been established. We now continue and show that the degree of spin correlation is independent of the components' separation. Such a result might be related for example to Zhang's non-linear model for the formation of binary stars from a nebula.

Netzach Farbiash; Raphael Steinitz

2004-12-08T23:59:59.000Z

75

Editor's Choice Series on Agricultural Ethics Who Owns Biodiversity, and How Should the Owners  

E-Print Network [OSTI]

Editor's Choice Series on Agricultural Ethics Who Owns Biodiversity, and How Should the Owners 95616�8515 At the World Summit on Sustainable Development, held in Johannesburg in 2002, the Secretary a sustainable future for humanity. These five areas were water and sanitation, energy, health, agricultural

Gepts, Paul

76

Study Says Owners of Energy-Efficient Homes Would Recommend Them to Friends  

Broader source: Energy.gov [DOE]

A recent National Association of Home Builders (NAHB) study aimed at uncovering how owners of energy-efficient homes felt after purchasing their homes found that not only would the majority recommend the same green homes to friends, but more than 50% believed the benefits of energy efficiency outweighed the cost.

77

The Council of Industrial Boiler Owners special project on non-utility fossil fuel ash classification  

SciTech Connect (OSTI)

Information is outlined on the Council of Industrial Boiler Owners (CIBO) special project on non-utility fossil fuel ash classification. Data are presented on; current (1996) regulatory status of fossil-fuel combustion wastes; FBC technology identified for further study; CIBO special project methods; Bevill amendment study factors; data collection; and CIBO special project status.

Svendsen, R.L.

1996-12-31T23:59:59.000Z

78

Audio Binary Halftone Watermarking Algorithm  

Science Journals Connector (OSTI)

Conventional audio watermarking method has the following deficiencies: the embedded watermarking signal bits are too less; the image watermarking pre-process is too simple which reduce the security; the embedded audio watermarking is meaningless binary sequence. To address these problems, we propose a robust audio watermarking algorithm based on audio binary halftone pre-process. The meaningful audio watermarking can be preprocessed to high-fidelity binary audio. The variable dimension operation is used to scramble the host audio. Experiments show the proposed algorithm has big embedding quantity, high security, strong practicability and robustness in enduring common attacks.

Huan Li; Zheng Qin; Xuanping Zhang; Xu Wang

2011-01-01T23:59:59.000Z

79

Ultraviolet studies of interacting binaries  

E-Print Network [OSTI]

Interacting Binaries consist of a variety of stellar objects in different stages of evolution and those containing accreting compact objects still represent a major challenge to our understanding of not only close binary evolution but also of the chemical evolution of the Galaxy. These end-points of binary star evolution are ideal laboratories for the study of accretion and outflow processes, and provide insight on matter under extreme physical conditions. One of the key-questions of fundamental relevance is the nature of SNIa progenitors. The study of accreting compact binary systems relies on observations over the entire electromagnetic spectrum and we outline here those unresolved questions for which access to the ultraviolet range is vital, as they cannot be addressed by observations in any other spectral region.

B. T. Gaensicke; D. de Martino; T. R. Marsh; C. A. Haswell; C. Knigge; K. S. Long; S. N. Shore

2005-10-04T23:59:59.000Z

80

Facility Name Facility Name Facility FacilityType Owner Developer EnergyPurchaser  

Open Energy Info (EERE)

Name Facility Name Facility FacilityType Owner Developer EnergyPurchaser Name Facility Name Facility FacilityType Owner Developer EnergyPurchaser Place GeneratingCapacity NumberOfUnits CommercialOnlineDate WindTurbineManufacturer FacilityStatus Coordinates D Metals D Metals D Metals Definition Small Scale Wind Valley City OH MW Northern Power Systems In Service AB Tehachapi Wind Farm AB Tehachapi Wind Farm AB Tehachapi Definition Commercial Scale Wind Coram Energy AB Energy Southern California Edison Co Tehachapi CA MW Vestas In Service AFCEE MMR Turbines AFCEE MMR Turbines AFCEE MMR Turbines Definition Commercial Scale Wind AFCEE Air Force Center for Engineering and the Environment Distributed generation net metered Camp Edwards Sandwich MA MW GE Energy In Service AG Land AG Land AG Land Definition Community Wind AG Land Energy LLC

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


81

Solar PV Project Financing: Regulatory and Legislative Challenges for Third-Party PPA System Owners (Revised)  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

23 23 Revised February 2010 Solar PV Project Financing: Regulatory and Legislative Challenges for Third-Party PPA System Owners Katharine Kollins Duke University Bethany Speer and Karlynn Cory National Renewable Energy Laboratory National Renewable Energy Laboratory 1617 Cole Boulevard, Golden, Colorado 80401-3393 303-275-3000 * www.nrel.gov NREL is a national laboratory of the U.S. Department of Energy Office of Energy Efficiency and Renewable Energy Operated by the Alliance for Sustainable Energy, LLC Contract No. DE-AC36-08-GO28308 Technical Report NREL/TP-6A2-46723 Revised February 2010 Solar PV Project Financing: Regulatory and Legislative Challenges for Third-Party PPA System Owners Katharine Kollins Duke University Bethany Speer and Karlynn Cory

82

Binary Cycle Power Plant | Open Energy Information  

Open Energy Info (EERE)

Binary Cycle Power Plant Binary Cycle Power Plant (Redirected from Binary) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Binary Cycle Power Plant General List of Binary Plants Binary power plant process diagram - DOE EERE 2012 Binary cycle geothermal power generation plants differ from Dry Steam and Flash Steam systems in that the water or steam from the geothermal reservoir never comes in contact with the turbine/generator units. Low to moderately heated (below 400°F) geothermal fluid and a secondary (hence, "binary") fluid with a much lower boiling point that water pass through a heat exchanger. Heat from the geothermal fluid causes the secondary fluid to flash to vapor, which then drives the turbines and subsequently, the generators. Binary cycle power plants are closed-loop systems and virtually nothing

83

"Table HC3.4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005" 4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ," Housing Units (millions)" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Space Heating Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Do Not Have Space Heating Equipment",1.2,0.6,0.3,"N","Q","Q","Q" "Have Main Space Heating Equipment",109.8,77.5,63.7,4.2,1.8,2.2,5.6

84

"Table HC3.8 Water Heating Characteristics by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

8 Water Heating Characteristics by Owner-Occupied Housing Unit, 2005" 8 Water Heating Characteristics by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Water Heating Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Number of Water Heaters" "1.",106.3,74.5,60.9,4,1.8,2.2,5.5 "2 or More",3.7,3.3,3,"Q","Q","Q","Q" "Do Not Use Hot Water",1.1,0.3,"Q","Q","N","Q","Q"

85

"Table HC3.5 Space Heating Usage Indicators by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

5 Space Heating Usage Indicators by Owner-Occupied Housing Unit, 2005" 5 Space Heating Usage Indicators by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ," Housing Units (millions)" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Space Heating Usage Indicators",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total U.S. Housing Units",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Do Not Have Heating Equipment",1.2,0.6,0.3,"N","Q","Q","Q" "Have Space Heating Equipment",109.8,77.5,63.7,4.2,1.8,2.2,5.6

86

"Table HC3.7 Air-Conditioning Usage Indicators by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

7 Air-Conditioning Usage Indicators by Owner-Occupied Housing Unit, 2005" 7 Air-Conditioning Usage Indicators by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions)" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Air Conditioning Usage Indicators",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Do Not Have Cooling Equipment",17.8,11.3,9.3,0.6,"Q",0.4,0.9 "Have Cooling Equipment",93.3,66.8,54.7,3.6,1.7,1.9,4.8 "Use Cooling Equipment",91.4,65.8,54,3.6,1.7,1.9,4.7

87

"Table HC3.11 Home Electronics Characteristics by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

1 Home Electronics Characteristics by Owner-Occupied Housing Unit, 2005" 1 Home Electronics Characteristics by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions)" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Home Electronics Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Personal Computers" "Do Not Use a Personal Computer ",35.5,20.3,14.8,1.2,0.6,0.9,2.8 "Use a Personal Computer",75.6,57.8,49.2,2.9,1.2,1.4,3 "Number of Desktop PCs"

88

"Table HC3.9 Home Appliances Characteristics by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

HC3.9 Home Appliances Characteristics by Owner-Occupied Housing Unit, 2005" HC3.9 Home Appliances Characteristics by Owner-Occupied Housing Unit, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Home Appliances Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total U.S.",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Cooking Appliances" "Conventional Ovens" "Use an Oven",109.6,77.3,63.4,4.1,1.8,2.3,5.6 "1.",103.3,71.9,58.6,3.9,1.6,2.2,5.5 "2 or More",6.2,5.4,4.8,"Q","Q","Q","Q"

89

"Table HC3.6 Air Conditioning Characteristics by Owner-Occupied Housing Units, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

6 Air Conditioning Characteristics by Owner-Occupied Housing Units, 2005" 6 Air Conditioning Characteristics by Owner-Occupied Housing Units, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Air Conditioning Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Do Not Have Cooling Equipment",17.8,11.3,9.3,0.6,"Q",0.4,0.9 "Have Cooling Equipment",93.3,66.8,54.7,3.6,1.7,1.9,4.8 "Use Cooling Equipment",91.4,65.8,54,3.6,1.7,1.9,4.7

90

"Table HC3.1 Housing Unit Characteristics by Owner-Occupied Housing Unit, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

Housing Unit Characteristics by Owner-Occupied Housing Unit, 2005" Housing Unit Characteristics by Owner-Occupied Housing Unit, 2005" " Million Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Housing Unit Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Census Region and Division" "Northeast",20.6,13.4,10.4,1.4,1,0.3,0.4 "New England",5.5,3.8,3.1,"Q",0.3,"Q","Q" "Middle Atlantic",15.1,9.6,7.3,1.3,0.6,"Q","Q"

91

DOE NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference  

Broader source: Energy.gov (indexed) [DOE]

NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference NSTB Researchers Demonstrate R&D Successes to Asset Owners at EnergySec Conference October 1, 2009 More than 150 energy sector leaders-including nearly 100 asset owners and operators-gathered at the 2009 EnergySec Annual Summit in Seattle, WA, on Sept. 23-24, where researchers from the Department of Energy's National SCADA Test Bed (NSTB) Program gave a four-hour demonstration and presentation of their Roadmap-related control systems security work. EnergySec is an information sharing forum with more than 230 utility members representing 75 energy companies across the nation. Its fifth annual conference drew asset owners, vendors, and government representatives for presentations and discussions on NERC CIP standards, collaborative industry efforts

92

"Table HC3.2 Living Space Characteristics by Owner-Occupied Housing Units, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

2 Living Space Characteristics by Owner-Occupied Housing Units, 2005" 2 Living Space Characteristics by Owner-Occupied Housing Units, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ," Housing Units (millions) " ,,,"Single-Family Units",,"Apartments in Buildings With--" "Living Space Characteristics",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Floorspace (Square Feet)" "Total Floorspace1" "Fewer than 500",3.2,1.1,"Q","Q","Q","Q",0.4 "500 to 999",23.8,7.2,3.5,0.3,0.3,0.9,2.2

93

"Table HC3.13 Lighting Usage Indicators by Owner-Occupied Housing Unit Zone, 2005"  

U.S. Energy Information Administration (EIA) Indexed Site

3 Lighting Usage Indicators by Owner-Occupied Housing Unit Zone, 2005" 3 Lighting Usage Indicators by Owner-Occupied Housing Unit Zone, 2005" " Million U.S. Housing Units" ,," Owner-Occupied Housing Units (millions)","Type of Owner-Occupied Housing Unit" ,"U.S. Housing Units (millions" ,,,"Single-Family Units",,"Apartments in Buildings With--" "Lighting Usage Indicators",,,"Detached","Attached","2 to 4 Units","5 or More Units","Mobile Homes" "Total U.S. Housing Units",111.1,78.1,64.1,4.2,1.8,2.3,5.7 "Indoor Lights Turned On During Summer" "Number of Lights Turned On" "Between 1 and 4 Hours per Day",91.8,65,54.3,3.3,1.5,1.6,4.4 "1.",28.6,17.9,14,0.9,0.6,0.7,1.7

94

Fact #856 January 19, 2015 Plug-in and Hybrid Cars Receive High Scores for Owner Satisfaction  

Broader source: Energy.gov [DOE]

The annual owner-satisfaction survey from Consumer Reports in 2014 covered 350,000 vehicles from one to three years old. They asked subscribers if they would purchase the same vehicle again knowing...

95

Binary black hole mergers in gaseous environments: 'Binary Bondi' and 'binary Bondi-Hoyle-Lyttleton' accretion  

SciTech Connect (OSTI)

Merging supermassive black hole-black hole binaries produced in galaxy mergers are promising sources of detectable gravitational waves. If such a merger takes place in a gaseous environment, there is a possibility of a simultaneous detection of electromagnetic and gravitational radiation, as the stirring, shock heating, and accretion of the gas may produce variability and enhancements in the electromagnetic flux. Such a simultaneous detection can provide a wealth of opportunities to study gravitational physics, accretion physics, and cosmology. We investigate this scenario by performing fully general-relativistic, hydrodynamic simulations of merging, equal-mass, nonspinning black hole-black hole binaries embedded in gas clouds. We evolve the metric using the Baumgarte-Shapiro-Shibata-Nakamura formulation with standard moving puncture gauge conditions and handle the hydrodynamics via a high-resolution shock-capturing scheme. We consider both 'binary Bondi accretion' in which the binary is at rest relative to the ambient gas cloud, as well as 'binary Bondi-Hoyle-Lyttleton accretion' in which the binary moves relative to the gas cloud. The gas cloud is assumed to be homogeneous far from the binary and governed by a {Gamma}-law equation of state. We vary {Gamma} between 4/3 and 5/3. For each simulation, we compute the gas flow and accretion rate and estimate the electromagnetic luminosity due to bremsstrahlung and synchrotron emission. We find evidence for significant enhancements in both the accretion rate and luminosity over values for a single black hole of the same mass as the binary. We estimate that this luminosity enhancement should be detectable by the Large Synoptic Survey Telescope for a 10{sup 6}M{sub {center_dot}}binary in a hot gas cloud of density n{approx}10 cm{sup -3} and temperature T{approx}10{sup 6} K at z=1, reaching a maximum of L{approx}3x10{sup 43} erg s{sup -1}, with the emission peaking in the visible band, and lasting for {approx}1 hour.

Farris, Brian D.; Liu, Yuk Tung; Shapiro, Stuart L. [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States)

2010-04-15T23:59:59.000Z

96

Binary Cycle Power Plant | Open Energy Information  

Open Energy Info (EERE)

Binary Cycle Power Plant Binary Cycle Power Plant (Redirected from Binary Cycle Power Plants) Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Binary Cycle Power Plant General List of Binary Plants Binary power plant process diagram - DOE EERE 2012 Binary cycle geothermal power generation plants differ from Dry Steam and Flash Steam systems in that the water or steam from the geothermal reservoir never comes in contact with the turbine/generator units. Low to moderately heated (below 400°F) geothermal fluid and a secondary (hence, "binary") fluid with a much lower boiling point that water pass through a heat exchanger. Heat from the geothermal fluid causes the secondary fluid to flash to vapor, which then drives the turbines and subsequently, the generators.

97

Searching for gravitational waves from binary coalescence  

E-Print Network [OSTI]

We describe the implementation of a search for gravitational waves from compact binary coalescences in LIGO and Virgo data. This all-sky, all-time, multidetector search for binary coalescence has been used to search data ...

Vaulin, Ruslan

98

Urey Prize Lecture: Binary Minor Planets  

E-Print Network [OSTI]

in the Kuiper belt is uncertain by an order of magnitude due to poor knowledge of albedo/density. Distribution Binary objects detected by lightcurve are not included in this chart. Over 50 binary minor planets can

Margot, Jean-Luc

99

Safety evaluation report related to Babcock and Wilcox Owners Group Plant Reassessment Program: (Final report)  

SciTech Connect (OSTI)

After the accident of Three Mile Island, Unit 2, nuclear power plant owners made a number of improvements to their nuclear facilities. Despite these improvements, the US Nuclear Regulatory Commission (NRC) staff is concerned that the number and complexity of events at Babcock and Wilcox (B and W) nuclear plants have not decreased as expected. This concern was reinforced by the June 9, 1985 total-loss-of-feedwater event at Davis-Besse Nuclear Power Station and the December 26, 1985 overcooling transient at Rancho Seco Nuclear Generating Station. By letter dated January 24, 1986, the Executive Director for Operations (EDO) informed the Chairman of the B and W Owners Group (BWOG) that a number of recent events at B and W-designed reactors have led the NRC staff to conclude that the basic requirements for B and W reactors need to be reexamined. In its February 13, 1986 response to the EDO's letter, the BWOG committed to lead an effort to define concerns relative to reducing the frequency of reactor trips and the complexity of post-trip response in B and W plants. The BWOG submitted a description of the B and W program entitled ''Safety and Performance Improvement Program'' (BAW-1919) on May 15, 1986. Five revisions to BAW-1919 have also been submitted. The NRC staff has reviewed BAW-1919 and its revisions and presents its evaluation in this report. 2 figs., 34 tabs.

Not Available

1987-11-01T23:59:59.000Z

100

Table HC3.4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005  

U.S. Energy Information Administration (EIA) Indexed Site

.4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005 .4 Space Heating Characteristics by Owner-Occupied Housing Unit, 2005 Million U.S. Housing Units Total................................................................ 111.1 78.1 64.1 4.2 1.8 2.3 5.7 Do Not Have Space Heating Equipment....... 1.2 0.6 0.3 N Q Q Q Have Main Space Heating Equipment.......... 109.8 77.5 63.7 4.2 1.8 2.2 5.6 Use Main Space Heating Equipment............ 109.1 77.2 63.6 4.2 1.8 2.1 5.6 Have Equipment But Do Not Use It.............. 0.8 0.3 Q N Q Q Q Main Heating Fuel and Equipment Natural Gas.................................................. 58.2 41.8 35.3 2.8 1.2 1.0 1.6 Central Warm-Air Furnace........................ 44.7 34.8 29.7 2.3 0.7 0.6 1.4 For One Housing Unit........................... 42.9 34.3 29.5 2.3 0.6 0.6 1.4 For Two Housing Units..........................

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101

Binary Cycle Power Plant | Open Energy Information  

Open Energy Info (EERE)

GEOTHERMAL ENERGYGeothermal Home GEOTHERMAL ENERGYGeothermal Home Binary Cycle Power Plant General List of Binary Plants Binary power plant process diagram - DOE EERE 2012 Binary cycle geothermal power generation plants differ from Dry Steam and Flash Steam systems in that the water or steam from the geothermal reservoir never comes in contact with the turbine/generator units. Low to moderately heated (below 400°F) geothermal fluid and a secondary (hence, "binary") fluid with a much lower boiling point that water pass through a heat exchanger. Heat from the geothermal fluid causes the secondary fluid to flash to vapor, which then drives the turbines and subsequently, the generators. Binary cycle power plants are closed-loop systems and virtually nothing (except water vapor) is emitted to the atmosphere. Resources below 400°F

102

Beowawe Binary Bottoming Cycle | Department of Energy  

Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

generation from the nonconventional geothermal resources of 205F by extracting waste heat from the brine to power a binary power plant. lowmcdonaldbeowawebinarybottomingc...

103

Table HC1-5a. Housing Unit Characteristics by Type of Owner-Occupied Housing Unit,  

U.S. Energy Information Administration (EIA) Indexed Site

5a. Housing Unit Characteristics by Type of Owner-Occupied Housing Unit, 5a. Housing Unit Characteristics by Type of Owner-Occupied Housing Unit, Million U.S. Households, 2001 Housing Unit Characteristics RSE Column Factor: Total Owner- Occupied Units Type of Owner-Occupied Housing Unit RSE Row Factors Single-Family Apartments in Buildings With Mobile Homes Two to Four Units Five or More Units 0.4 0.4 1.8 2.1 1.4 Total ............................................... 72.7 63.2 2.1 1.8 5.7 6.7 Census Region and Division Northeast ...................................... 13.0 10.8 1.1 0.5 0.6 11.4 New England .............................. 3.5 3.1 0.2 Q 0.1 16.9 Middle Atlantic ............................ 9.5 7.7 0.9 0.4 0.4 13.4 Midwest ......................................... 17.5 16.0 0.3 Q 1.0 10.3 East North Central ......................

104

Woodland owners' attitudes towards energy from forest biomass in a carbon-intensive jurisdiction: Case study of Nova Scotia, Canada  

Science Journals Connector (OSTI)

Abstract The use of forest biomass in thermal generation processes has been recognized by the Government of Nova Scotia (NS) as one option that could help meet its renewable electricity goals (25% by 2015 and 40% by 2020). Over half of the woodland in NS is owned by small-private woodland owners (51%), indicating that they could significantly influence the future of NS forests and its potential use for energy purposes. This paper presents the results of a survey of small-woodland owners on their attitudes towards using energy from forest biomass. 489 small-woodland owners responded to mail-out surveys and 14 rural community members participated in three focus groups. Three major findings emerged. First, it was found that the acceptability of using forest products varied depending on multiple factors the source of biomass, harvesting methods, and [predicted] end-use. Second, forest sustainability and keeping resources local were the two most important concerns amongst respondents. Finally, respondents felt that better collaboration with other stakeholders and education around the issues would be the best strategies for overcoming these concerns. The paper also highlights the barriers and drivers as perceived by the woodland owners as they relate to the possibility of using more biomass for energy in the future.

Margo MacGregor; Michelle Adams; Peter Duinker

2014-01-01T23:59:59.000Z

105

Taking an Alternative Route: A guide for fleet operators and individual owners using alternative fuels in cars and trucks  

SciTech Connect (OSTI)

Taking an Alternative Route is a 30-page guide for fleet managers and individual owners on using alternative fuels in cars and trucks. Discussed in detail are all fuels authorized for federal credits under the Energy Policy Act of 1992 (EPAct). The publication informs federal and state fleet managers about how to comply with EPAct, and provides information about the Clean Air Act Amendments.

LaRocque, T.

2001-04-18T23:59:59.000Z

106

Your University of Bristol Tier 4 Student Visa, March 2014, v5 Document Owner: International Advice and Support  

E-Print Network [OSTI]

Your University of Bristol Tier 4 Student Visa, March 2014, v5 Document Owner: International Advice a copy of these documents makes securing a replacement much easier. You should inform the police as soon as you are aware of a loss or theft of these documents, as you will also need a crime reference number

Bristol, University of

107

2009-2010 Special Projects Boellstorff: A Southern Region Well Owner Network to Safeguard Private Well and Aquifer Integrity  

E-Print Network [OSTI]

, improper well construction techniques, abandoned wells, improperly sited and functioning on-site wastewater treatment systems, and changes in land use. The aim of the proposed Southern Region Well Owner Network integrity. The SRWON will improve rural and rural-urban interface environmental management by providing

108

Group Member Names: ________________________________________________ Scenario: You are the owner of a potato plant in Idaho. You have recently won a contract  

E-Print Network [OSTI]

: ________________________________________________ ________________________________________________ ________________________________________________ Scenario: You are the owner of a potato plant in Idaho. You have recently won a contract to supply McDonald's with potatoes. McDonald's requires their suppliers to precut and freeze the potatoes before shipping to their distributing center. Your potato plant does not currently have a process for precutting and freezing potatoes

Provancher, William

109

Table HC7-5a. Home Office Equipment by Type of Owner-Occupied Housing Unit,  

U.S. Energy Information Administration (EIA) Indexed Site

5a. Home Office Equipment by Type of Owner-Occupied Housing Unit, 5a. Home Office Equipment by Type of Owner-Occupied Housing Unit, Million U.S. Households, 2001 Home Office Equipment RSE Column Factor: Total Owner- Occupied Units Type of Owner-Occupied Housing Unit RSE Row Factors Single-Family Apartments in Buildings With Mobile Home Two to Four Units Five or More Units 0.3 0.3 2.1 3.0 1.6 Total ............................................... 72.7 63.2 2.1 1.8 5.7 6.7 Households Using Office Equipment .......................... 67.5 59.0 2.0 1.7 4.8 7.0 Personal Computers 1 ................... 45.7 41.1 1.3 0.9 2.4 8.6 Number of Desktop PCs 1 .................................................. 34.1 30.5 1.0 0.7 1.9 9.7 2 or more .................................... 7.4 7.0 Q Q 0.2 18.4 Number of Laptop PCs 1 ..................................................

110

A Fast Search Technique for Binary Pulsars  

E-Print Network [OSTI]

I describe a computationally simple, efficient, and sensitive method to search long observations for pulsars in binary systems. The technique looks for orbitally induced sidebands in the power spectrum around a nominal spin frequency, enabling it to detect pulsars in high- or low-mass binaries with short orbital periods (P_orb <~ 5 h).

Scott M. Ransom

1999-11-05T23:59:59.000Z

111

Population synthesis of wide binary millisecond pulsars  

Science Journals Connector (OSTI)

......from our population synthesis code are in good agreement with those...s1, respectively. In model NS2, the maximum amount of mass...using a rapid binary evolution code based on the analytical approximation...adopted in our binary evolution code. We assume mass transfer to......

B. Willems; U. Kolb

2002-12-11T23:59:59.000Z

112

The Evolution of Compact Binary Star Systems  

E-Print Network [OSTI]

We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact binary stars are expected to be the most important sources for the forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binary stars with NS and/or black components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically important thermonuclear SN Ia. We also consider AM CVn-stars which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

Konstantin Postnov; Lev Yungelson

2014-03-21T23:59:59.000Z

113

*Intel and the Intel logo are registered trademarks of Intel Corporation. Other brands and names are the property of their respective owners The Concurrent Collections (CnC) Parallel Programming  

E-Print Network [OSTI]

are the property of their respective owners The Concurrent Collections (CnC) Parallel Programming Model and names are the property of their respective owners 8 Influence 1: Streaming ·!CnC is like Streaming

Hazelwood, Kim

114

Safety Evaluation Report related to Hydrogen Control Owners Group assessment of Mark 3 containments  

SciTech Connect (OSTI)

Title 10 of the Code of Federal Regulations (10 CFR), Section 50.44 Standards for Combustible Gas Control System in Light-Water-Cooled Power Reactors,'' requires that systems be provided to control hydrogen concentration in the containment atmosphere following an accident to ensure that containment integrity is maintained. The purpose of this report is to provide regulatory guidance to licensees with Mark III containments with regard to demonstrating compliance with 10 CFR 50.44, Section (c)(3)(vi) and (c)(3)(vii). In this report, the staff provides its evaluation of the generic methodology proposed by the Hydrogen Control Owners Group. This generic methodology is documented in Topical Report HGN-112-NP, Generic Hydrogen Control Information for BWR/6 Mark III Containments.'' In addition, the staff has recommended that the vulnerability to interruption of power to the hydrogen igniters be evaluated further on a plant-specific basis as part of the individual plant examination of the plants with Mark III containments. 10 figs., 1 tab.

Li, C.Y.; Kudrick, J.A.

1990-10-01T23:59:59.000Z

115

STEPS TO ESTABLISH A REAL-TIME TRANSMISSION MONITORING SYSTEM FOR TRANSMISSION OWNERS AND OPERATORS WITHIN THE  

Broader source: Energy.gov (indexed) [DOE]

STEPS TO ESTABLISH A REAL-TIME TRANSMISSION MONITORING STEPS TO ESTABLISH A REAL-TIME TRANSMISSION MONITORING SYSTEM FOR TRANSMISSION OWNERS AND OPERATORS WITHIN THE EASTERN AND WESTERN INTERCONNECTIONS A REPORT TO CONGRESS PURSUANT TO SECTION 1839 OF THE ENERGY POLICY ACT OF 2005 Prepared by United States Department of Energy & Federal Energy Regulatory Commission February 3, 2006 Report to Congress Joint Report by the Department of Energy and Federal Energy Regulatory Commission on Steps to Establish a Real-Time Transmission Monitoring System for Transmission Owners and Operators within the Eastern and Western Interconnections February 2006 Executive Summary In August 2003, an electrical outage in one state precipitated a cascading blackout across seven other states and as far north as a province in Canada, leaving more than 50 million

116

Binary mixture flammability characteristics for hazard assessment  

E-Print Network [OSTI]

calculations and UNIFAC, a theoretical model that does not require experimental binary interaction parameters, are employed in the mixture flash point predictions, which are validated with experimental data. MFPB is successfully predicted using the UNIFAC model...

Vidal Vazquez, Migvia del C.

2005-11-01T23:59:59.000Z

117

Black hole binary inspiral and trajectory dominance  

E-Print Network [OSTI]

Gravitational waves emitted during the inspiral, plunge and merger of a black hole binary carry linear momentum. This results in an astrophysically important recoil to the final merged black hole, a kick that can eject ...

Price, Richard H.

118

Optimization of nave dynamic binary instrumentation Tools/  

E-Print Network [OSTI]

The proliferation of dynamic program analysis tools has done much to ease the burden of developing complex software. However, creating such tools remains a challenge. Dynamic binary instrumentation frameworks such as ...

Kleckner, Reid (Reid N.)

2011-01-01T23:59:59.000Z

119

New bounds on optimal binary search trees  

E-Print Network [OSTI]

Binary search trees (BSTs) are a class of simple data structures used to store and access keys from an ordered set. They have been around for about half a century. Despite their ubiquitous use in practical programs, ...

Harmon, Dion (Dion Kane)

2006-01-01T23:59:59.000Z

120

ROTATIONAL DOPPLER BEAMING IN ECLIPSING BINARIES  

SciTech Connect (OSTI)

In eclipsing binaries the stellar rotation of the two components will cause a rotational Doppler beaming during eclipse ingress and egress when only part of the eclipsed component is covered. For eclipsing binaries with fast spinning components this photometric analog of the well-known spectroscopic Rossiter-McLaughlin effect can exceed the strength of the orbital effect. Example light curves are shown for a detached double white dwarf binary, a massive O-star binary and a transiting exoplanet case, similar to WASP-33b. Inclusion of the rotational Doppler beaming in eclipsing systems is a prerequisite for deriving the correct stellar parameters from fitting high-quality photometric light curves and can be used to determine stellar obliquities as well as, e.g., an independent measure of the rotational velocity in those systems that may be expected to be fully synchronized.

Groot, Paul J., E-mail: pgroot@astro.ru.nl [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States)

2012-01-20T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


121

This journal is c the Owner Societies 2012 Phys. Chem. Chem. Phys., 2012, 14, 675680 675 Cite this: Phys. Chem. Chem. Phys., 2012, 14, 675680  

E-Print Network [OSTI]

This journal is c the Owner Societies 2012 Phys. Chem. Chem. Phys., 2012, 14, 675­680 675 Cite this: Phys. Chem. Chem. Phys., 2012, 14, 675­680 Photodissociation of isobutene at 193 nm Gabriel M. P. Just

Neumark, Daniel M.

122

Text-Alternative Version: The L Prize-Winning LED A19 ReplacementWhat Commercial Building Owners/Operators Can Expect in 2012  

Broader source: Energy.gov [DOE]

Below is the text-alternative version of the "The L Prize-Winning LED A19 ReplacementWhat Commercial Building Owners/Operators Can Expect in 2012" webcast, held January 18, 2012.

123

Nonindustrial private forest owners' opinions to and awareness of energy wood market and forest-based bioenergy certification - results of a case study from Finnish Karelia  

Science Journals Connector (OSTI)

Nonindustrial private forest owners (NIPFs) in Finland are important stakeholders of forest management and roundwood supply decisions. Their role will also be significant to supply energy wood to meet Finland's t...

Pradipta Halder; Timo Weckroth; Qu Mei

2012-09-01T23:59:59.000Z

124

Detection Rates for Close Binaries Via Microlensing  

E-Print Network [OSTI]

Microlensing is one of the most promising methods of reconstructing the stellar mass function down to masses even below the hydrogen-burning limit. The fundamental limit to this technique is the presence of unresolved binaries, which can in principle significantly alter the inferred mass function. Here we quantify the fraction of binaries that can be detected using microlensing, considering specifically the mass ratio and separation of the binary. We find that almost all binary systems with separations greater than $b \\sim 0.4$ of their combined Einstein ring radius are detectable assuming a detection threshold of $3\\%$. For two M dwarfs, this corresponds to a limiting separation of $\\gsim 1 \\au$. Since very few observed M dwarfs have companions at separations $\\lsim 1 \\au$, we conclude that close binaries will probably not corrupt the measurements of the mass function. We find that the detectability depends only weakly on the mass ratio. For those events for which individual masses can be determined, we find that binaries can be detected down to $b \\sim 0.2$.

B. Scott Gaudi; Andrew Gould

1996-06-17T23:59:59.000Z

125

Guide to Combined Heat and Power Systems for Boiler Owners and Operators  

SciTech Connect (OSTI)

Combined heat and power (CHP) or cogeneration is the sequential production of two forms of useful energy from a single fuel source. In most CHP applications, chemical energy in fuel is converted to both mechanical and thermal energy. The mechanical energy is generally used to generate electricity, while the thermal energy or heat is used to produce steam, hot water, or hot air. Depending on the application, CHP is referred to by various names including Building Cooling, Heating, and Power (BCHP); Cooling, Heating, and Power for Buildings (CHPB); Combined Cooling, Heating, and Power (CCHP); Integrated Energy Systems (IES), or Distributed Energy Resources (DER). The principal technical advantage of a CHP system is its ability to extract more useful energy from fuel compared to traditional energy systems such as conventional power plants that only generate electricity and industrial boiler systems that only produce steam or hot water for process applications. By using fuel energy for both power and heat production, CHP systems can be very energy efficient and have the potential to produce electricity below the price charged by the local power provider. Another important incentive for applying cogeneration technology is to reduce or eliminate dependency on the electrical grid. For some industrial processes, the consequences of losing power for even a short period of time are unacceptable. The primary objective of the guide is to present information needed to evaluate the viability of cogeneration for new or existing industrial, commercial, and institutional (ICI) boiler installations and to make informed CHP equipment selection decisions. Information presented is meant to help boiler owners and operators understand the potential benefits derived from implementing a CHP project and recognize opportunities for successful application of cogeneration technology. Topics covered in the guide follow: (1) an overview of cogeneration technology with discussions about benefits of applying cogeneration technology and barriers to implementing cogeneration technology; (2) applicable federal regulations and permitting issues; (3) descriptions of prime movers commonly used in CHP applications, including discussions about design characteristics, heat-recovery options and equipment, fuels and emissions, efficiency, maintenance, availability, and capital cost; (4) electrical generators and electrical interconnection equipment; (5) cooling and dehumidification equipment; (6) thermodynamic cycle options and configurations; (7) steps for evaluating the technical and economic feasibility of applying cogeneration technology; and (8) information sources.

Oland, CB

2004-08-19T23:59:59.000Z

126

TIDAL NOVAE IN COMPACT BINARY WHITE DWARFS  

SciTech Connect (OSTI)

Compact binary white dwarfs (WDs) undergoing orbital decay due to gravitational radiation can experience significant tidal heating prior to merger. In these WDs, the dominant tidal effect involves the excitation of outgoing gravity waves in the inner stellar envelope and the dissipation of these waves in the outer envelope. As the binary orbit decays, the WDs are synchronized from outside in (with the envelope synchronized first, followed by the core). We examine the deposition of tidal heat in the envelope of a carbon-oxygen WD and study how such tidal heating affects the structure and evolution of the WD. We show that significant tidal heating can occur in the star's degenerate hydrogen layer. This layer heats up faster than it cools, triggering runaway nuclear fusion. Such 'tidal novae' may occur in all WD binaries containing a CO WD, at orbital periods between 5 minutes and 20 minutes, and precede the final merger by 10{sup 5}-10{sup 6} years.

Fuller, Jim; Lai Dong [Department of Astronomy, Cornell University, Ithaca, NY 14850 (United States)

2012-09-01T23:59:59.000Z

127

Hybrid black-hole binary initial data  

E-Print Network [OSTI]

Traditional black-hole binary puncture initial data is conformally flat. This unphysical assumption is coupled with a lack of radiation signature from the binary's past life. As a result, waveforms extracted from evolutions of this data display an abrupt jump. In Kelly et al. [Class.Quant.Grav.27:114005,2010], a new binary black-hole initial data with radiation contents derived in the post-Newtonian (PN) calculation was adapted to puncture evolutions in numerical relativity. This data satisfies the constraint equations to the 2.5PN order, and contains a transverse-traceless "wavy" metric contribution, violating the standard assumption of conformal flatness. Although the evolution contained less spurious radiation, there were undesired features; the unphysical horizon mass loss and the large initial orbital eccentricity. Introducing a hybrid approach to the initial data evaluation, we significantly reduce these undesired features.

Bruno C. Mundim; Bernard J. Kelly; Yosef Zlochower; Hiroyuki Nakano; Manuela Campanelli

2010-12-04T23:59:59.000Z

128

Understanding white dwarf binary evolution with white dwarf/main sequence binaries: first results from SEGUE  

E-Print Network [OSTI]

Close white dwarf binaries make up a wide variety of objects such as double white dwarf binaries, which are possible SN Ia progenitors, cataclysmic variables, super soft sources, or AM CVn stars. The evolution and formation of close white dwarf binaries crucially depends on the rate at which angular momentum is extracted from the binary orbit. The two most important sources of angular momentum loss are the common envelope phase and magnetic braking. Both processes are so far poorly understood. Observational population studies of white dwarf/main sequence binaries provide the potential to significantly progress with this situation and to clearly constrain magnetic braking and the CE-phase. However, the current population of white dwarf/main sequence binaries is highly incomplete and heavily biased towards young systems containing hot white dwarfs. The SDSSII/SEGUE collaboration awarded us with 5 fibers per plate pair in order to fill this gap and to identify the required unbiased sample of old white dwarf/main sequence binaries. The success rate of our selection criteria exceeds 65% and during the first 10 months we have identified 41 new systems, most of them belonging to the missed old population.

M. R. Schreiber; A. Nebot Gomez-Moran; A. D. Schwope

2006-11-15T23:59:59.000Z

129

Dynamical Tides in Rotating Binary Stars  

Science Journals Connector (OSTI)

We study the effect of rotation on the excitation of internal oscillation modes of a star by the external gravitational potential of its companion. Unlike the nonrotating case, there are difficulties with the usual mode decomposition for rotating stars because of the asymmetry between modes propagating in the direction of rotation and those propagating opposite to it. For an eccentric binary system, we derive general expressions for the energy transfer, ?Es, and the corresponding angular momentum transfer, ?Js, in a periastron passage when there is no initial oscillation present in the star. Except when a nearly precise orbital resonance occurs (i.e., the mode frequency equals multiple of the orbital frequency), ?Es is very close to the steady state mode energy in the tide in the presence of dissipation. It is shown that stellar rotation can change the strength of dynamical tide significantly. In particular, retrograde rotation with respect to the orbit increases the energy transfer by bringing lower order g-modes (or f-modes for convective stars), which couple more strongly to the tidal potential, into closer resonances with the orbital motion of the companion. We apply our general formalism to the problems of tidal capture binary formation and the orbital evolution of the PSR J0045-7319/B star binary. Stellar rotation changes the critical impact parameter for binary capture. Although the enhancement (by retrograde rotation) in the capture cross section is at most ~20%, the probability that the captured system survives disruption/merging and therefore becomes a binary can be significantly larger. It is found that in order to explain the observed rapid orbital decay of the PSR J0045-7319 binary system, retrograde rotation in the B star is required.

Dong Lai

1997-01-01T23:59:59.000Z

130

KOI-3278: A Self-Lensing Binary Star System  

Science Journals Connector (OSTI)

...eclipsing binary. By modeling the pulse as gravitational...the Quasiperiodic Automated Transit Search algorithm (17) turned...The quasiperiodic automated transit search algorithm...Eggleton P. P. , Rapid binary star evolution for N-body simulations and population synthesis...

Ethan Kruse; Eric Agol

2014-04-18T23:59:59.000Z

131

Lattice Boltzmann simulations of binary fluid flow through porous media  

Science Journals Connector (OSTI)

...V. Coveney and S. Succi Lattice Boltzmann simulations of binary fluid...D-80290 Munchen, Germany The lattice Boltzmann equation is often advocated...three-dimensional 19 velocity lattice Boltzmann model for immiscible binary...

2002-01-01T23:59:59.000Z

132

GENERATING BINARY PROCESSES WITH ALL-POLE SPECTRA Petros Boufounos  

E-Print Network [OSTI]

GENERATING BINARY PROCESSES WITH ALL-POLE SPECTRA Petros Boufounos MIT Digital signal Processing presents an algorithm to generate autoregressive random binary processes with predefined mean spectrum. The process is generated recursively using a linear combination of the previously generated

Boufounos, Petros T.

133

Geothermal Binary Power Generation System Using Unutilized Energy  

Science Journals Connector (OSTI)

Binary power generating system is based on the Rankine cycle with geothermal fluid as heating source and low boiling ... can generate electric power from low temperature (energy) source. Employing the binary powe...

Hiroaki Shibata; Hiroshi Oyama

2007-01-01T23:59:59.000Z

134

Binary Capture Rates for Massive Protostars  

E-Print Network [OSTI]

The high multiplicity of massive stars in dense, young clusters is established early in their evolution. The mechanism behind this remains unresolved. Recent results suggest that massive protostars may capture companions through disk interactions with much higher efficiency than their solar mass counterparts. However, this conclusion is based on analytic determinations of capture rates and estimates of the robustness of the resulting binaries. We present the results of coupled n-body and SPH simulations of star-disk encounters to further test the idea that disk-captured binaries contribute to the observed multiplicity of massive stars.

Nickolas Moeckel; John Bally

2007-04-09T23:59:59.000Z

135

Lattice Boltzmann model for binary mixtures  

Science Journals Connector (OSTI)

An a priori derivation of the lattice Boltzmann equations for binary mixtures is provided by discretizing the Boltzmann equations that govern the evolution of binary mixtures. The present model leads to a set of two-fluid hydrodynamic equations for the mixture. In existing models, employing the single-relaxation-time approximation, the viscosity and diffusion coefficients are coupled through the relaxation parameter ?, thus limited to unity Prandtl number and Schmidt number. In the present model the viscosity and diffusion coefficient are independently controlled by two relaxation parameters, thus enabling the modeling of mixtures with an arbitrary Schmidt number. The theoretical framework developed here can be readily applied to multiple-species mixing.

Li-Shi Luo and Sharath S. Girimaji

2002-09-27T23:59:59.000Z

136

Small geothermal binary plants in Mexico  

SciTech Connect (OSTI)

In Mexico, Comision Federal de Electricidad (CFE Federal Commission of Electricity) has identified several low enthalpy sites related with thermal water, at shallow depths. Some of those geothermal prospects are located far from the electrical national grid. In some cases, the population solve their electricity needs by internal combustion engines with very high operating costs. CFE has started a project oriented to use the energy contained in the thermal waters with off-grid binary plants. The two first projects are in the state of Chihuahua at the north of the country: San Antonio El Bravo and Maguarichic. At both places CFE will install a 300 kW, unattended binary power units.

Lopez-Diaz, M.

1996-12-31T23:59:59.000Z

137

Mastering the pilot domestic binary combined-cycle plants  

Science Journals Connector (OSTI)

Results are presented from mastering the pilot binary combined-cycle plants of Type PGU-450T (installed at...

Yu. A. Radin

2006-07-01T23:59:59.000Z

138

Binary Codes In this lesson, you will study  

E-Print Network [OSTI]

Coded Decimal (BCD), Error detection codes, Character codes 2. Coding versus binary conversion. Binary Decimal (BCD) code which corresponds to the first 10 binary representations of the decimal digits 0-9. The BCD code requires 4 bits to represent the 10 decimal digits. Since 4 bits may have up to 16 different

Bouhraoua, Abdelhafid

139

CSP for binary conservative relational structures  

E-Print Network [OSTI]

We prove that whenever A is a 3-conservative relational structure with only binary and unary relations then the algebra of polymorphisms of A either has no Taylor operation (i.e. CSP(A) is NP-complete), or generates a congruence meet semidistributive variety (i.e. CSP(A) has bounded width).

Kazda, Alexandr

2011-01-01T23:59:59.000Z

140

The electromagnetic signals of compact binary mergers  

Science Journals Connector (OSTI)

......to the dynamical ejecta of ns2 and nsbh binaries. Our study...for recent reviews. Our code is an updated version of the...earlier peak. b The canonical ns2 case. c This is the maximal signal from our runs of ns2 mergers. d nsbh merger. The......

Tsvi Piran; Ehud Nakar; Stephan Rosswog

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


141

Supermassive Black Hole Binaries: The Search Continues  

E-Print Network [OSTI]

Gravitationally bound supermassive black hole binaries (SBHBs) are thought to be a natural product of galactic mergers and growth of the large scale structure in the universe. They however remain observationally elusive, thus raising a question about characteristic observational signatures associated with these systems. In this conference proceeding I discuss current theoretical understanding and latest advances and prospects in observational searches for SBHBs.

Tamara Bogdanovic

2014-06-19T23:59:59.000Z

142

Binary Tomography with Deblurring Stefan Weber1  

E-Print Network [OSTI]

two scenarios of limited-angle binary tomography with data distorted with an unknown convolution: Either the projec- tion data are taken from a blurred object, or the projection data them- selves the projection data before reconstruction (let us call them preprocessing) and then the reconstruction

Schnörr, Christoph

143

THE ELM SURVEY. V. MERGING MASSIVE WHITE DWARF BINARIES  

SciTech Connect (OSTI)

We present the discovery of 17 low-mass white dwarfs (WDs) in short-period (P {<=} 1 day) binaries. Our sample includes four objects with remarkable log g {approx_equal} 5 surface gravities and orbital solutions that require them to be double degenerate binaries. All of the lowest surface gravity WDs have metal lines in their spectra implying long gravitational settling times or ongoing accretion. Notably, six of the WDs in our sample have binary merger times <10 Gyr. Four have {approx}>0.9 M{sub Sun} companions. If the companions are massive WDs, these four binaries will evolve into stable mass transfer AM CVn systems and possibly explode as underluminous supernovae. If the companions are neutron stars, then these may be millisecond pulsar binaries. These discoveries increase the number of detached, double degenerate binaries in the ELM Survey to 54; 31 of these binaries will merge within a Hubble time.

Brown, Warren R.; Kenyon, Scott J. [Smithsonian Astrophysical Observatory, 60 Garden St, Cambridge, MA 02138 (United States); Kilic, Mukremin; Gianninas, A. [Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks St., Norman, OK, 73019 (United States); Allende Prieto, Carlos, E-mail: wbrown@cfa.harvard.edu, E-mail: skenyon@cfa.harvard.edu, E-mail: kilic@ou.edu, E-mail: alexg@nhn.ou.edu, E-mail: callende@iac.es [Instituto de Astrofisica de Canarias, E-38205, La Laguna, Tenerife (Spain)

2013-05-20T23:59:59.000Z

144

Message from the Owner of the Improved Financial Performance Initiative of the Presidents Management Agenda:  

Broader source: Energy.gov (indexed) [DOE]

I am enthusiastic and proud to be the owner of the Improved Financial Performance initiative of the President's Management Agenda (PMA) in the Department of Energy (DOE). The Department has received clean opinions on its annual financial statements for six straight years with no material internal control weaknesses identified by the auditors. Further, DOE was successful in maintaining its clean opinion for the FY 2004 financial statements while accelerating issuance to 45 days after the end of the fiscal year. For the third quarter of FY 2004, when the Department of Energy received a Green status score on Improved Financial Performance, DOE was one of only five agencies with a Green status score on this initiative. I am enormously proud

145

Phenomenological gravitational waveforms from spinning coalescing binaries  

E-Print Network [OSTI]

An accurate knowledge of the coalescing binary gravitational waveform is crucial for experimental searches as the ones performed by the LIGO-Virgo collaboration. Following an earlier paper by the same authors we refine the construction of analytical phenomenological waveforms describing the signal sourced by generically spinning binary systems. The gap between the initial inspiral part of the waveform, described by spin-Taylor approximants, and its final ring-down part, described by damped exponentials, is bridged by a phenomenological phase calibrated by comparison with the dominant spherical harmonic mode of a set of waveforms including both numerical and phenomenological waveforms of different type. All waveforms considered describe equal mass systems. The Advanced LIGO noise-weighted overlap integral between the numerical and phenomenological waveforms presented here ranges between 0.95 and 0.99 for a wide span of mass values.

R. Sturani; S. Fischetti; L. Cadonati; G. M. Guidi; J. Healy; D. Shoemaker; A. Vicere'

2011-06-23T23:59:59.000Z

146

PRESOLICITATION Category: A. Owner: Department of Energy, Oak Ridge National Laboratory -UT Battelle LLC (DOE Contractor), Oak Ridge National Laboratory, Bethel  

E-Print Network [OSTI]

PRESOLICITATION Category: A. Owner: Department of Energy, Oak Ridge National Laboratory - UT Battelle LLC (DOE Contractor), Oak Ridge National Laboratory, Bethel Valley Road P.O. Box 2008, Oak Ridge-Battelle), the management and operating contractor for the United States Department of Energy's Oak Ridge National

Hively, Lee M.

147

2654 Phys. Chem. Chem. Phys., 2013, 15, 2654--2659 This journal is c the Owner Societies 2013 Cite this: Phys.Chem.Chem.Phys.,2013,  

E-Print Network [OSTI]

this: Phys.Chem.Chem.Phys.,2013, 15, 2654 Influence of catalyst choices on transport behaviors of In2654 Phys. Chem. Chem. Phys., 2013, 15, 2654--2659 This journal is c the Owner Societies 2013 Cite and controllable NW physical properties. The NW growths, including vapor­ liquid­solid (VLS) or vapor

Javey, Ali

148

Recent observational progress in AM CVn binaries  

E-Print Network [OSTI]

We present the results of some recent research on AM CVn systems. We present: X-ray/UV observations made using XMM-Newton; the X-ray grating spectrum of RX J1914+24; preliminary results of a search for radio emission from AM CVn binaries, and discuss the strategy and first results of the RATS project, whose main aim is to discover AM CVn systems.

G. Ramsay; C. Brocksopp; P. Groot; P. Hakala; H. Lehto; T. Marsh; R. Napiwotzki; G. Nelemans; S. Potter; B. Slee; D. Steeghs; K. Wu

2006-10-12T23:59:59.000Z

149

The binary fraction of extreme horizontal branch stars  

E-Print Network [OSTI]

(Abbreviated) We have used precise radial velocity measurements of subdwarf-B stars from the Palomar-Green catalogue to look for binary extreme horizontal branch (EHB) stars. We identify 36 EHB stars in our sample and find that at least 21 of these stars are binaries. All but one or two of these are new identifications. The minimum binary fraction for EHB stars implied by our survey is 60+-8%. Our survey is sensitive to binaries with orbital periods P less than about 10d. For reasonable assumptions concerning the period distribution and the mass ratio distribution of the binaries, we find that the mean detection efficiency of our survey over this range of orbital periods is 87%. Allowing for this estimated detection efficiency, the fraction of EHB stars which are short-period binaries ($0.03 < P <10d, approximately) is 69+-9%. The value is not strongly dependent on the period distribution below P=10d or the mean companion mass for these short-period binaries. The orbital separation of the stars in these binaries is much less than the size of the red giant from which the EHB star has formed. This is strong evidence that binary star evolution is fundamental to the formation of the majority of EHB stars. If there are also binary EHB stars whose orbital periods are more than about 10d, the fraction of EHB stars whose evolution has been affected by the presence of a companion may be much higher.

P. F. L. Maxted; U. Heber; T. R. Marsh; R. C. North

2001-03-21T23:59:59.000Z

150

Gravitational lensing in eclipsing binary stars  

E-Print Network [OSTI]

I consider the effect of the gravitational deflection of light upon the light curves of eclipsing binary stars, focussing mainly upon systems containing at least one white dwarf component. In absolute terms the effects are small, however they are strongest at the time of secondary eclipse when the white dwarf transits its companion, and act to reduce the depth of this feature. If not accounted for, this may lead to under-estimation of the radius of the white dwarf compared to that of its companion. I show that the effect is significant for plausible binary parameters, and that it leads to ~25% reduction in the transit depth in the system KPD 1930+2752. The reduction of eclipse depth is degenerate with the stellar radius ratio, and therefore cannot be used to establish the existence of lensing. A second order effect of the light bending is to steepen the ingress and egress features of the secondary eclipse relative to the primary eclipse, although it will be difficult to see this in practice. I consider also binaries containing neutron stars and black-holes. I conclude that, although relatively large effects are possible in such systems, a combination of rarity, faintness and intrinsic variability make it unlikely that lensing will be detectable in them.

T. R. Marsh

2000-12-18T23:59:59.000Z

151

A binary LP model to the facility layout problem Abstract  

E-Print Network [OSTI]

Such locations will influence material handling or distance costs and ..... binary row) and select the location which will be placed (based on the lowest value in...

Cpu

2002-04-04T23:59:59.000Z

152

Dixie Valley Bottoming Binary Cycle | Department of Energy  

Office of Energy Efficiency and Renewable Energy (EERE) Indexed Site

objective: Prove the technical and economic feasibility of utilizing the available unused heat to generate additional electric power from a binary power plant from low-temperature...

153

DESTRUCTION OF BINARY MINOR PLANETS DURING NEPTUNE SCATTERING  

SciTech Connect (OSTI)

The existence of extremely wide binaries in the low-inclination component of the Kuiper Belt provides a unique handle on the dynamical history of this population. Some popular frameworks of the formation of the Kuiper Belt suggest that planetesimals were moved there from lower semimajor axis orbits by scattering encounters with Neptune. We test the effects such events would have on binary systems and find that wide binaries are efficiently destroyed by the kinds of scattering events required to create the Kuiper Belt with this mechanism. This indicates that a binary-bearing component of the cold Kuiper Belt was emplaced through a gentler mechanism or was formed in situ.

Parker, Alex H. [Department of Astronomy, University of Victoria, BC (Canada); Kavelaars, J. J., E-mail: alexhp@uvic.c [Herzberg Institute of Astrophysics, National Research Council of Canada (Canada)

2010-10-20T23:59:59.000Z

154

Oscillating red-giant stars in eccentric binary systems  

E-Print Network [OSTI]

The unparalleled photometric data obtained by NASA's Kepler Space Telescope has led to improved understanding of red-giant stars and binary stars. We discuss the characterization of known eccentric system, containing a solar-like oscillating red-giant primary component. We also report several new binary systems that are candidates for hosting an oscillating companion. A powerful approach to study binary stars is to combine asteroseimic techniques with light curve fitting. Seismology allows us to deduce the properties of red giants. In addition, by modeling the ellipsoidal modulations we can constrain the parameters of the binary system. An valuable independent source are ground-bases, high-resolution spectrographs.

Beck, P G; Vos, J; Kallinger, T; Garcia, R A; Mathur, S; Houmani, K

2014-01-01T23:59:59.000Z

155

The influence of energy audits on the energy efficiency investments of private owner-occupied households in the Netherlands  

Science Journals Connector (OSTI)

Abstract Energy audits are promoted as an effective tool to drive investment in energy efficiency measures in the residential sector. Despite operating in many countries for several decades details of the impact of audits are mixed. The aim of research presented here is to explore the role of audits on investment in energy efficiency measures by private owner-occupied householders in the Netherlands. Results showed that the main influence of the energy audit was to confirm information held by householders. A significant portion of audit recommendations was ignored, the main reason being that householders considered their dwellings to be adequately energy efficient. A comparison of audit recipients to non-recipients showed that audit recipients did not adopt, plan to adopt or invest in more energy efficiency measures than non-recipients. In fact non-recipients adopted more and invested more in measures. It is concluded that energy based renovation is driven by householder perception of comfort and acceptable outlay on energy bills and not necessarily to expert technical tailored information on the potential to reduce CO2 emissions and environmental impact. Results support arguments for minimum energy efficiency standards and performance based incentives.

Lorraine Murphy

2014-01-01T23:59:59.000Z

156

Nonlinear Tides in Close Binary Systems  

Science Journals Connector (OSTI)

We study the excitation and damping of tides in close binary systems, accounting for the leading-order nonlinear corrections to linear tidal theory. These nonlinear corrections include two distinct physical effects: three-mode nonlinear interactions, i.e., the redistribution of energy among stellar modes of oscillation, and nonlinear excitation of stellar normal modes by the time-varying gravitational potential of the companion. This paper, the first in a series, presents the formalism for studying nonlinear tides and studies the nonlinear stability of the linear tidal flow. Although the formalism we present is applicable to binaries containing stars, planets, and/or compact objects, we focus on non-rotating solar-type stars with stellar or planetary companions. Our primary results include the following: (1) The linear tidal solution almost universally used in studies of binary evolution is unstable over much of the parameter space in which it is employed. More specifically, resonantly excited internal gravity waves in solar-type stars are nonlinearly unstable to parametric resonance for companion masses M' 10-100 M ? at orbital periods P ? 1-10 days. The nearly static "equilibrium" tidal distortion is, however, stable to parametric resonance except for solar binaries with P 2-5 days. (2) For companion masses larger than a few Jupiter masses, the dynamical tide causes short length scale waves to grow so rapidly that they must be treated as traveling waves, rather than standing waves. (3) We show that the global three-wave treatment of parametric instability typically used in the astrophysics literature does not yield the fastest-growing daughter modes or instability threshold in many cases. We find a form of parametric instability in which a single parent wave excites a very large number of daughter waves (N ? 103[P/10 days] for a solar-type star) and drives them as a single coherent unit with growth rates that are a factor of ?N faster than the standard three-wave parametric instability. These are local instabilities viewed through the lens of global analysis; the coherent global growth rate follows local rates in the regions where the shear is strongest. In solar-type stars, the dynamical tide is unstable to this collective version of the parametric instability for even sub-Jupiter companion masses with P a month. (4) Independent of the parametric instability, the dynamical and equilibrium tides excite a wide range of stellar p-modes and g-modes by nonlinear inhomogeneous forcing; this coupling appears particularly efficient at draining energy out of the dynamical tide and may be more important than either wave breaking or parametric resonance at determining the nonlinear dissipation of the dynamical tide.

Nevin N. Weinberg; Phil Arras; Eliot Quataert; Josh Burkart

2012-01-01T23:59:59.000Z

157

E-Print Network 3.0 - accuracy binary black Sample Search Results  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

binary search tree with one extra bit of storage per node... of the tree. A binary search tree is a ... Source: Belohlavek, Radim - Department of Computer Science, Palack...

158

Binary Black Hole Accretion Flows From a Misaligned Circumbinary Disk  

Science Journals Connector (OSTI)

......mass-accretion-rate variation per binary...because each black hole passes across the circumbinary...mass-accretion-rate variation per binary...holes|black hole physics|Galaxies: nuclei...because each black hole passes across the circumbinary...the mass accretion rates is also independent......

Kimitake Hayasaki; Hideki Saito; Shin Mineshige

2013-08-25T23:59:59.000Z

159

k-PROTECTED VERTICES IN BINARY SEARCH TREES MIKLOS BONA  

E-Print Network [OSTI]

k-PROTECTED VERTICES IN BINARY SEARCH TREES MIKL´OS B´ONA Abstract. We show that for every k, the probability that a randomly selected vertex of a random binary search tree on n nodes is at distance k - 1. In another model, leaves may represent end-users (customers) of a company, and in that case, it may

Bona, Miklos

160

Layered Binary-Dielectrics for Energy Applications: Limitations and Potentials  

SciTech Connect (OSTI)

In this Letter, an attempt is made to illustrate how performance of an electrically insulating material, a dielectric, can be improved by constructing a layered binary-dielectric structure that employs a weak insulator with high dielectric permittivity. It is shown that layered binary-dielectrics could have a signicant impact on energy storage and electrical insulation.

Tuncer, Enis [ORNL

2012-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


161

On Binary Methods Kim Bruce, Luca Cardelli, Giuseppe Castagna,  

E-Print Network [OSTI]

On Binary Methods Kim Bruce, Luca Cardelli, Giuseppe Castagna, The Hopkins Objects Group, Gary T 50011­1040, USA #12; On Binary Methods Kim Bruce \\Lambda Department of Computer Science, Williams­ dations of Object­Oriented Languages, which was spon­ sored by NSF and ESPRIT and held in Paris in June

Trifonov, Valery

162

Surface tension in a reactive binary mixture of incompressible fluids  

E-Print Network [OSTI]

Surface tension in a reactive binary mixture of incompressible fluids Henning Struchtrup Institute with a distributed form of surface tension. The model describes chemistry, diffusion, viscosity and heat transfer tension at the front. Keywords: Binary mixtures, Surface tension, Irreversible thermodynamics, Hele

Struchtrup, Henning

163

ccsd00004127, ON THE SURFACE TENSIONS OF BINARY MIXTURES  

E-Print Network [OSTI]

ccsd­00004127, version 1 ­ 2 Feb 2005 ON THE SURFACE TENSIONS OF BINARY MIXTURES JEAN RUIZ Abstract tensions and the concentrations are brie y reviewed. Key Words: Surface tensions, binary mixtures the corresponding surface tension depends on the composition of the mixture. Some relationship is expected which

164

Note on the size of binary Armstrong codes Aart Blokhuis  

E-Print Network [OSTI]

Note on the size of binary Armstrong codes Aart Blokhuis , Andries Brouwer, Attila Sali April 19, 2012 Abstract We show for binary Armstrong codes Arm(2, k, n) that asymptotically n/k 1.224, while) for all admissible n. Keywords: coding theory; databases; Armstrong codes AMS subject classification: 94B

Brouwer, Andries E.

165

Note on the size of binary Armstrong codes Aart Blokhuis  

E-Print Network [OSTI]

Note on the size of binary Armstrong codes Aart Blokhuis , Andries Brouwer, Attila Sali February 20, 2012 Abstract We show for binary Armstrong codes Arm(2, k, n) that asymptotically n/k 1.224, while) for all admissible n. Keywords: coding theory; databases; Armstrong codes AMS subject classification: 94B

Brouwer, Andries E.

166

Modeling Spatial-Temporal Binary Data Using Markov Random Fields  

E-Print Network [OSTI]

Modeling Spatial-Temporal Binary Data Using Markov Random Fields Jun Zhu Department of Statistics to the autologistic model for spatial-temporal binary data. The model we propose is a Markov chain across time, where discuss the generality of our approach for modeling other types of spatial-temporal lattice data. Keywords

Huang, Su-Yun

167

A Combined Decimal and Binary Floating-point Divider  

E-Print Network [OSTI]

to most recent decimal divider designs, which are based on the Binary Coded Decimal (BCD) encoding, our Integer Decimal (BID) encoding. DPD is a compressed form of the Binary Coded Decimal (BCD) encoding on the BCD encoding [3],[4],[5], using the DPD encoding for floating-point and the BCD encoding for fixed

Nannarelli, Alberto

168

Advanced binary cycles: Optimum working fluids  

SciTech Connect (OSTI)

A computer model (Cycle Analysis Simulation Tool, CAST) and a methodology have been developed to perform value analysis for small, low- to moderate-temperature binary geothermal power plants. The value analysis method allows for incremental changes in the levelized electricity cost (LEC) to be determined between a baseline plant and a modified plant. Thermodynamic cycle analyses and component sizing are carried out in the model followed by economic analysis which provides LEC results. The emphasis of the present work is on evaluating the effect of mixed working fluids instead of pure fluids on the LEC of a geothermal binary plant that uses a simple Organic Rankine Cycle. Four resources were studied spanning the range of 265 F to 375 F. A variety of isobutane and propane based mixtures, in addition to pure fluids, were used as working fluids. This study shows that the use of propane mixtures at a 265 F resource can reduce the LEC by 24% when compared to a base case value that utilizes commercial isobutane as its working fluid. The cost savings drop to 6% for a 375 F resource, where an isobutane mixture is favored. Supercritical cycles were found to have the lowest cost at all resources.

Gawlik, K.; Hassani, V. [National Renewable Energy Lab., Golden, CO (United States)

1997-12-31T23:59:59.000Z

169

Thermodynamics of magnetized binary compact objects  

SciTech Connect (OSTI)

Binary systems of compact objects with electromagnetic field are modeled by helically symmetric Einstein-Maxwell spacetimes with charged and magnetized perfect fluids. Previously derived thermodynamic laws for helically symmetric perfect-fluid spacetimes are extended to include the electromagnetic fields, and electric currents and charges; the first law is written as a relation between the change in the asymptotic Noether charge {delta}Q and the changes in the area and electric charge of black holes, and in the vorticity, baryon rest mass, entropy, charge and magnetic flux of the magnetized fluid. Using the conservation laws of the circulation of magnetized flow found by Bekenstein and Oron for the ideal magnetohydrodynamic fluid, and also for the flow with zero conducting current, we show that, for nearby equilibria that conserve the quantities mentioned above, the relation {delta}Q=0 is satisfied. We also discuss a formulation for computing numerical solutions of magnetized binary compact objects in equilibrium with emphasis on a first integral of the ideal magnetohydrodynamic-Euler equation.

Uryu, Koji [Department of Physics, University of the Ryukyus, Senbaru, Nishihara, Okinawa 903-0213 (Japan); Gourgoulhon, Eric [Laboratoire Univers et Theories, UMR 8102 du CNRS, Observatoire de Paris, Universite Paris Diderot, F-92190 Meudon (France); Markakis, Charalampos [Department of Physics, University of Wisconsin-Milwaukee, Post Office Box 413, Milwaukee, Wisconsin 53201 (United States)

2010-11-15T23:59:59.000Z

170

Binary classification of items of interest in a repeatable process  

DOE Patents [OSTI]

A system includes host and learning machines in electrical communication with sensors positioned with respect to an item of interest, e.g., a weld, and memory. The host executes instructions from memory to predict a binary quality status of the item. The learning machine receives signals from the sensor(s), identifies candidate features, and extracts features from the candidates that are more predictive of the binary quality status relative to other candidate features. The learning machine maps the extracted features to a dimensional space that includes most of the items from a passing binary class and excludes all or most of the items from a failing binary class. The host also compares the received signals for a subsequent item of interest to the dimensional space to thereby predict, in real time, the binary quality status of the subsequent item of interest.

Abell, Jeffrey A.; Spicer, John Patrick; Wincek, Michael Anthony; Wang, Hui; Chakraborty, Debejyo

2014-06-24T23:59:59.000Z

171

A Flashing Binary Combined Cycle For Geothermal Power Generation | Open  

Open Energy Info (EERE)

Flashing Binary Combined Cycle For Geothermal Power Generation Flashing Binary Combined Cycle For Geothermal Power Generation Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Journal Article: A Flashing Binary Combined Cycle For Geothermal Power Generation Details Activities (0) Areas (0) Regions (0) Abstract: The performance of a flashing binary combined cycle for geothermal power generation is analysed. It is proposed to utilize hot residual brine from the separator in flashing-type plants to run a binary cycle, thereby producing incremental power. Parametric variations were carried out to determine the optimum performance of the combined cycle. Comparative evaluation with the simple flashing plant was made to assess its thermodynamic potential and economic viability. Results of the analyses indicate that the combined cycle can generate 13-28% more power than the

172

Automated analysis of eclipsing binary lightcurves. I. EBAS -- a new Eclipsing Binary Automated Solver with EBOP  

E-Print Network [OSTI]

We present a new algorithm -- Eclipsing Binary Automated Solver (EBAS), to analyse lightcurves of eclipsing binaries. The algorithm is designed to analyse large numbers of lightcurves, and is therefore based on the relatively fast EBOP code. To facilitate the search for the best solution, EBAS uses two parameter transformations. Instead of the radii of the two stellar components, EBAS uses the sum of radii and their ratio, while the inclination is transformed into the impact parameter. To replace human visual assessment, we introduce a new 'alarm' goodness-of-fit statistic that takes into account correlation between neighbouring residuals. We perform extensive tests and simulations that show that our algorithm converges well, finds a good set of parameters and provides reasonable error estimation.

Omer Tamuz; Tsevi Mazeh; Pierre North

2006-01-10T23:59:59.000Z

173

Reliability Standards Owner  

Broader source: Energy.gov [DOE]

This position is located in the Internal Operations and Asset Management group of Planning and Asset Management (TP). A successful candidate in this position will serve as the Reliability Standards...

174

From binary breakup to multifragmentation: Computer simulation  

Science Journals Connector (OSTI)

A semiclassical model developed for the computer simulation of nuclear reactions is applied to the problem of fragmentation in proton and heavy ion induced reactions. Simulations based on the model are used to follow the time evolution of the reactions in both coordinate and phase space as well as to calculate correlations for quantities such as fragment positions and masses. Three reactions are selected for detailed study: p+Ag at 300 MeV, and Ca+Ca at 25 and 50 MeV/nucleon bombarding energy. It is shown that the behavior expected for these reactions from the mechanical instability properties of nuclear matter is supported by the simulations. An experimental measure of the change from binary breakup to multifragmentation is shown to be the two-particle correlation function in mass.

David H. Boal and James N. Glosli

1988-01-01T23:59:59.000Z

175

Mapping the peculiar binary GP Com  

E-Print Network [OSTI]

We present high resolution spectra of the AM CVn helium binary GP Com at two different wavelength ranges. The spectra show the same flaring behaviour observed in previous UV and optical data. We find that the central spike contributes to the flare spectra indicating that its origin is probably the compact object. We also detect that the central spike moves with orbital phase following an S-wave pattern. The radial velocity semiamplitude of the S-wave is \\~10 km/s which indicates its origin is near the centre of mass of the system, which in this case lies very close to the white dwarf. The Stark effect seems to affect significantly the central spike of some of the lines suggesting that it forms in a high electron density region. This again favours the idea that the central spike originates in the white dwarf. We present Doppler maps obtained for the emission lines which show three clear emission regions.

L. Morales-Rueda; T. R. Marsh; R. C. North

2000-08-29T23:59:59.000Z

176

NONLINEAR TIDES IN CLOSE BINARY SYSTEMS  

SciTech Connect (OSTI)

We study the excitation and damping of tides in close binary systems, accounting for the leading-order nonlinear corrections to linear tidal theory. These nonlinear corrections include two distinct physical effects: three-mode nonlinear interactions, i.e., the redistribution of energy among stellar modes of oscillation, and nonlinear excitation of stellar normal modes by the time-varying gravitational potential of the companion. This paper, the first in a series, presents the formalism for studying nonlinear tides and studies the nonlinear stability of the linear tidal flow. Although the formalism we present is applicable to binaries containing stars, planets, and/or compact objects, we focus on non-rotating solar-type stars with stellar or planetary companions. Our primary results include the following: (1) The linear tidal solution almost universally used in studies of binary evolution is unstable over much of the parameter space in which it is employed. More specifically, resonantly excited internal gravity waves in solar-type stars are nonlinearly unstable to parametric resonance for companion masses M' {approx}> 10-100 M{sub Circled-Plus} at orbital periods P Almost-Equal-To 1-10 days. The nearly static 'equilibrium' tidal distortion is, however, stable to parametric resonance except for solar binaries with P {approx}< 2-5 days. (2) For companion masses larger than a few Jupiter masses, the dynamical tide causes short length scale waves to grow so rapidly that they must be treated as traveling waves, rather than standing waves. (3) We show that the global three-wave treatment of parametric instability typically used in the astrophysics literature does not yield the fastest-growing daughter modes or instability threshold in many cases. We find a form of parametric instability in which a single parent wave excites a very large number of daughter waves (N Almost-Equal-To 10{sup 3}[P/10 days] for a solar-type star) and drives them as a single coherent unit with growth rates that are a factor of Almost-Equal-To N faster than the standard three-wave parametric instability. These are local instabilities viewed through the lens of global analysis; the coherent global growth rate follows local rates in the regions where the shear is strongest. In solar-type stars, the dynamical tide is unstable to this collective version of the parametric instability for even sub-Jupiter companion masses with P {approx}< a month. (4) Independent of the parametric instability, the dynamical and equilibrium tides excite a wide range of stellar p-modes and g-modes by nonlinear inhomogeneous forcing; this coupling appears particularly efficient at draining energy out of the dynamical tide and may be more important than either wave breaking or parametric resonance at determining the nonlinear dissipation of the dynamical tide.

Weinberg, Nevin N. [Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States); Arras, Phil [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Quataert, Eliot; Burkart, Josh, E-mail: nevin@mit.edu [Astronomy Department and Theoretical Astrophysics Center, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)

2012-06-01T23:59:59.000Z

177

The binary properties of the pulsating subdwarf B eclipsing binary PG 1336-018 (NY Vir)  

E-Print Network [OSTI]

We present an unbiased orbit solution and mass determination of the components of the eclipsing binary NY Vir as a critical test for the formation scenarios of subdwarf B stars. We obtained high-resolution time series VLT/UVES spectra and high-speed multicolour VLT/ULTRACAM photometric observations of NY Vir, a rapidly pulsating subdwarf B star in a short period eclipsing binary. Combining the radial velocity curve obtained from the VLT/UVES spectra with the VLT/ULTRACAM multicolour lightcurves, we determined numerical orbital solutions for this eclipsing binary. Due to the large number of free parameters and their strong correlations, no unique solution could be found, only families of solutions. We present three solutions of equal statistical significance, two of which are compatible with the primary having gone through a core He-flash and a common-envelope phase described by the $\\alpha$-formalism. These two models have an sdB primary of 0.466 \\msol and 0.389 \\msol, respectively. Finally, we report the detection of the Rossiter-McLaughlin effect for NY Vir.

M. Vu?kovi?; C. Aerts; R. stensen; G. Nelemans; H. Hu; C. S. Jeffery; V. S. Dhillon; T. R. Marsh

2007-06-22T23:59:59.000Z

178

Collision of two identical hypersonic stellar winds in binary systems  

E-Print Network [OSTI]

We investigate the hydrodynamics of two identical hypersonic stellar winds in a binary system. The interaction of these winds manifests itself in the form of two shocks and a contact surface between them. We neglect the binary rotation and assume that the gas flow ahead of the shocks is spherically symmetrical. In this case the contact surface that separates the gas emanated from the different stars coincides with the midplane of the binary components. In the shock the gas is heated and flows away nearly along the contact surface. We find the shock shape and the hot gas parameters in the shock layer between the shock and the contact surface.

Nikolay N. Pilyugin; Vladimir V. Usov

2006-10-13T23:59:59.000Z

179

Collision of two identical hypersonic stellar winds in binary systems  

E-Print Network [OSTI]

We investigate the hydrodynamics of two identical hypersonic stellar winds in a binary system. The interaction of these winds manifests itself in the form of two shocks and a contact surface between them. We neglect the binary rotation and assume that the gas flow ahead of the shocks is spherically symmetrical. In this case the contact surface that separates the gas emanated from the different stars coincides with the midplane of the binary components. In the shock the gas is heated and flows away nearly along the contact surface. We find the shock shape and the hot gas parameters in the shock layer between the shock and the contact surface.

Pilyugin, N N; Pilyugin, Nikolay N.; Usov, Vladimir V.

2006-01-01T23:59:59.000Z

180

Light and Life: Exotic Photosynthesis in Binary Star Systems  

E-Print Network [OSTI]

The potential for hosting photosynthetic life on Earth-like planets within binary/multiple stellar systems was evaluated by modelling the levels of photosynthetically active radiation (PAR) such planets receive. Combinations of M and G stars in: (i) close-binary systems; (ii) wide-binary systems and (iii) three-star systems were investigated and a range of stable radiation environments found to be possible. These environmental conditions allow for the possibility of familiar, but also more exotic forms of photosynthetic life, such as infrared photosynthesisers and organisms specialised for specific spectral niches.

O'Malley-James, J T; Cockell, C S; Greaves, J S

2011-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


181

Synthesis of binary images from band-limited functions  

Science Journals Connector (OSTI)

Binary images usually are produced by clipping band-limited images generated through physical systems. We examine the conditions under which a prescribed image can be formed by this...

Nashold, Karen M; Rudin, Walter; Saleh, Bahaa E A; Bucklew, James A

1989-01-01T23:59:59.000Z

182

A Binary Linear Programming Approach for LCA System Boundary Identification  

Science Journals Connector (OSTI)

One of the very first steps in conducting life cycle assessment (LCA) is system boundaries identification. A binary ... boundary between significant and insignificant processes in a LCA study. The proposed model ...

Feri Afrinaldi; Hong-Chao Zhang

2013-01-01T23:59:59.000Z

183

A Molecular-Thermodynamic Lattice Model for Binary Mixtures  

SciTech Connect (OSTI)

Using a method originally proposed for describing a continuum-space polymer fluid, a new expression for the Helmholtz energy of mixing is proposed for a binary lattice mixture. Molecular size asymmetry and nonrandomness due to segment-segment interactions are taken into account. An expression proposed by Yan, Liu and Hu for a binary lattice mixture of monomers, based on the Ising model, is used as a reference system. Calculated critical constants and liquid-liquid coexistence curves are in good agreement with Monte Carlo simulations for lattice mixtures with modest size asymmetry. Because lattice spacing rises with increasing temperature, comparison of calculated binary liquid-liquid equilibria with experiment requires that calculations take into account that the interchange energy falls as temperature rises. While the new expression for the Helmholtz energy of mixing provides much improvement over the Flory-Huggins equation, calculated liquid-liquid equilibria for three binary systems are similar to those from Guggenheim's quasi-chemical theory.

Qin, Yuan; Prausnitz, John M.

2005-04-29T23:59:59.000Z

184

Green's functions and hydrodynamics for isotopic binary diffusion  

E-Print Network [OSTI]

We study classical binary fluid mixtures in which densities vary on very short time (ps) and length (nm) scales, such that hydrodynamics does not apply. In a pure fluid with a localized heat pulse the breakdown of hydrodynamics was overcome using Green's functions which connect the initial densities to those at later times. Numerically it appeared that for long times the results from the Green's functions would approach hydrodynamics. In this paper we extend the Green's functions theory to binary mixtures. For the case of isothermal isobaric mutual diffusion in isotopic binary mixtures and ideal binary mixtures, which is easier to handle than heat conduction yet still non-trivial, we show analytically that in the Green's function approach one recovers hydrodynamic behaviour at long time scales provided the system reaches local equilibrium at long times. This is a first step toward giving the Green's function theory a firmer basis because it can for this case be considered as an extension of hydrodynamics.

R. van Zon; E. G. D. Cohen

2005-08-10T23:59:59.000Z

185

Topologies and approximation operators induced by binary relations  

E-Print Network [OSTI]

Rough set theory is an important mathematical tool for dealing with uncertain or vague information. This paper studies some new topologies induced by a binary relation on universe with respect to neighborhood opera- tors. Moreover, the relations among them are studied. In additionally, lower and upper approximations of rough sets using the binary relation with respect to neighborhood operators are studied and examples are given.

Nurettin Bagirmaz; A. Fatih Ozcan Hatice Tasbozan; Ilhan Icen

2014-05-09T23:59:59.000Z

186

Crossed diagrams for transport in substitutional binary alloys  

Science Journals Connector (OSTI)

We have adapted the method of summing crossed diagrams to the case of substitutional binary alloys. The summation is done by explicitly uncrossing the diagrams to look like ladders. Details are presented for the case of a single-band model of a simple-cubic lattice with nearest-neighbor hopping. The critical concentration at which the conductivity goes to zero is estimated. Some aspects of the generalization of this method to realistic models of binary alloys are discussed.

S. M. Chitanvis

1985-03-15T23:59:59.000Z

187

Phase Transformations in Binary Colloidal Monolayers  

E-Print Network [OSTI]

Phase transformations can be difficult to characterize at the microscopic level due to the inability to directly observe individual atomic motions. Model colloidal systems, by contrast, permit the direct observation of individual particle dynamics and of collective rearrangements, which allows for real-space characterization of phase transitions. Here, we study a quasi-two-dimensional, binary colloidal alloy that exhibits liquid-solid and solid-solid phase transitions, focusing on the kinetics of a diffusionless transformation between two crystal phases. Experiments are conducted on a monolayer of magnetic and nonmagnetic spheres suspended in a thin layer of ferrofluid and exposed to a tunable magnetic field. A theoretical model of hard spheres with point dipoles at their centers is used to guide the choice of experimental parameters and characterize the underlying materials physics. When the applied field is normal to the fluid layer, a checkerboard crystal forms; when the angle between the field and the normal is sufficiently large, a striped crystal assembles. As the field is slowly tilted away from the normal, we find that the transformation pathway between the two phases depends strongly on crystal orientation, field strength, and degree of confinement of the monolayer. In some cases, the pathway occurs by smooth magnetostrictive shear, while in others it involves the sudden formation of martensitic plates.

Ye Yang; Lin Fu; Catherine Marcoux; Joshua E. S. Socolar; Patrick Charbonneau; Benjamin B. Yellen

2015-02-10T23:59:59.000Z

188

Measuring tides and binary parameters from gravitational wave data and eclipsing timings of detached white dwarf binaries  

E-Print Network [OSTI]

The discovery of the most compact detached white dwarf (WD) binary SDSS J065133.33+284423.3 has been discussed in terms of probing the tidal effects in white dwarfs. This system is also a verification source for the space-based gravitational wave (GW) detector, evolved Laser Interferometer Space Antenna (eLISA) which will observe short-period compact Galactic binaries with $P_{orb}\\lesssim 5$ hrs. We address the prospects of doing tidal studies using eLISA binaries by showing the fractional uncertainties in the orbital decay rate and the rate of that decay, $\\dot{f}, \\ddot{f}$ expected from both the GW and EM data for some of the high-$f$ binaries. We find that $\\dot{f}$ and $\\ddot{f}$ can be measured using GW data only for the most massive WD binaries observed at high-frequencies. Form timing the eclipses for $\\sim 10$ years, we find that $\\dot{f}$ can be known to $\\sim 0.1% $ for J0651. We find that from GW data alone, measuring the effects of tides in binaries is (almost) impossible. We also investigate th...

Shah, Sweta

2014-01-01T23:59:59.000Z

189

A DEEPLY ECLIPSING DETACHED DOUBLE HELIUM WHITE DWARF BINARY  

SciTech Connect (OSTI)

Using Liverpool Telescope+RISE photometry we identify the 2.78 hr period binary star CSS 41177 as a detached eclipsing double white dwarf binary with a 21,100 K primary star and a 10,500 K secondary star. This makes CSS 41177 only the second known eclipsing double white dwarf binary after NLTT 11748. The 2 minute long primary eclipse is 40% deep and the secondary eclipse 10% deep. From Gemini+GMOS spectroscopy, we measure the radial velocities of both components of the binary from the H{alpha} absorption line cores. These measurements, combined with the light curve information, yield white dwarf masses of M{sub 1} = 0.283 {+-} 0.064 M{sub sun} and M{sub 2} = 0.274 {+-} 0.034 M{sub sun}, making them both helium core white dwarfs. As an eclipsing, double-lined spectroscopic binary, CSS 41177 is ideally suited to measuring precise, model-independent masses and radii. The two white dwarfs will merge in roughly 1.1 Gyr to form a single sdB star.

Parsons, S. G.; Marsh, T. R.; Gaensicke, B. T. [Department of Physics, University of Warwick, Coventry, CV4 7AL (United Kingdom); Drake, A. J. [California Institute of Technology, 1200 E. California Blvd, CA 91225 (United States); Koester, D. [Institut fuer Theoretische Physik und Astrophysik, Universitaet Kiel (Germany)

2011-07-10T23:59:59.000Z

190

DOUBLE-LINED SPECTROSCOPIC BINARY STARS IN THE RAVE SURVEY  

SciTech Connect (OSTI)

We devise a new method for the detection of double-lined binary stars in a sample of the Radial Velocity Experiment (RAVE) survey spectra. The method is both tested against extensive simulations based on synthetic spectra and compared to direct visual inspection of all RAVE spectra. It is based on the properties and shape of the cross-correlation function, and is able to recover {approx}80% of all binaries with an orbital period of order 1 day. Systems with periods up to 1 yr are still within the detection reach. We have applied the method to 25,850 spectra of the RAVE second data release and found 123 double-lined binary candidates, only eight of which are already marked as binaries in the SIMBAD database. Among the candidates, there are seven that show spectral features consistent with the RS CVn type (solar type with active chromosphere) and seven that might be of W UMa type (over-contact binaries). One star, HD 101167, seems to be a triple system composed of three nearly identical G-type dwarfs. The tested classification method could also be applicable to the data of the upcoming Gaia mission.

Matijevic, G.; Zwitter, T. [Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana (Slovenia); Munari, U.; Siviero, A. [INAF Osservatorio Astronomico di Padova, Asiago (Italy); Bienayme, O.; Siebert, A. [Observatorie de Strasbourg, Strasbourg (France); Binney, J. [Rudolf Pierls Center for Theoretical Physics, University of Oxford, Oxford (United Kingdom); Bland-Hawthorn, J. [Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney (Australia); Boeche, C.; Steinmetz, M. [Astrophysikalisches Institut Potsdam, Potsdam (Germany); Campbell, R. [Western Kentucky University, Bowling Green, KY (United States); Freeman, K. C. [RSAA, Australian National University, Camberra (Australia); Gibson, B. [University of Central Lancashire, Preston (United Kingdom); Gilmore, G. [Institute of Astronomy, Cambridge (United Kingdom); Grebel, E. K. [Astronomisches Rechen-Institut, Zentrum fuer Astronomie der Universitaet Heidelberg, Heidelberg (Germany); Helmi, A. [Kapteyn Astronomical Institute, University of Groningen, Groningen (Netherlands); Navarro, J. F. [University of Victoria, Victoria (Canada); Parker, Q. A. [Macquarie University, Sydney (Australia); Seabroke, G. M. [e2v Centre for Electronic Imaging, Planetary and Space Sciences Research Institute, Open University, Walton Hall, Milton Keynes (United Kingdom); Watson, F. G., E-mail: gal.matijevic@fmf.uni-lj.s [Anglo-Australian Observatory, Sydney (Australia)

2010-07-15T23:59:59.000Z

191

PERIOD ERROR ESTIMATION FOR THE KEPLER ECLIPSING BINARY CATALOG  

SciTech Connect (OSTI)

The Kepler Eclipsing Binary Catalog (KEBC) describes 2165 eclipsing binaries identified in the 115 deg{sup 2} Kepler Field based on observations from Kepler quarters Q0, Q1, and Q2. The periods in the KEBC are given in units of days out to six decimal places but no period errors are provided. We present the PEC (Period Error Calculator) algorithm, which can be used to estimate the period errors of strictly periodic variables observed by the Kepler Mission. The PEC algorithm is based on propagation of error theory and assumes that observation of every light curve peak/minimum in a long time-series observation can be unambiguously identified. The PEC algorithm can be efficiently programmed using just a few lines of C computer language code. The PEC algorithm was used to develop a simple model that provides period error estimates for eclipsing binaries in the KEBC with periods less than 62.5 days: log {sigma}{sub P} Almost-Equal-To - 5.8908 + 1.4425(1 + log P), where P is the period of an eclipsing binary in the KEBC in units of days. KEBC systems with periods {>=}62.5 days have KEBC period errors of {approx}0.0144 days. Periods and period errors of seven eclipsing binary systems in the KEBC were measured using the NASA Exoplanet Archive Periodogram Service and compared to period errors estimated using the PEC algorithm.

Mighell, Kenneth J. [National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719 (United States); Plavchan, Peter [NASA Exoplanet Science Institute, California Institute of Technology, Pasadena, CA 91125 (United States)

2013-06-15T23:59:59.000Z

192

Planetary Microlensing Perturbations: True Planets or Binary Sources?  

E-Print Network [OSTI]

A planetary microlensing event is characterized by a short-lived perturbation to the standard Paczy\\'nski curve. Planetary perturbations typically last from a few hours to a day, and have maximum amplitudes, $\\dmax$, of $5-20%$ of the standard curve. There exist a subset of binary-source events that can reproduce these main features, and thus masquerade as planetary events. These events require a binary source with a small flux ratio, $\\epsil \\sim 10^{-2}-10^{-4}$, and a small impact parameter for the fainter source, $\\beta_2 \\lsim \\epsil / \\dmax$. The detection probability of events of this type is $\\sim \\beta_2$, and can be as high as $\\sim 30%$; this is comparable to planetary detection rates. Thus a sample of planetary-like perturbations could be seriously contaminated by binary-source events, and there exists the possibility that completely meaningless physical parameters would be derived for any given perturbation. Here I derive analytic expressions for a binary-source event in the extreme flux ratio limit, and use these to demonstrate the basic degeneracy between binary source and planet perturbations. I describe how the degeneracy can be broken by dense and accurate sampling of the perturbation, optical/infrared photometry, or spectroscopic measurements.

B. Scott Gaudi

1997-06-26T23:59:59.000Z

193

Beowawe Bottoming Binary Project Geothermal Project | Open Energy  

Open Energy Info (EERE)

Beowawe Bottoming Binary Project Geothermal Project Beowawe Bottoming Binary Project Geothermal Project Jump to: navigation, search Last modified on July 22, 2011. Project Title Beowawe Bottoming Binary Project Project Type / Topic 1 Recovery Act: Geothermal Technologies Program Project Type / Topic 2 Geothermal Energy Production from Low Temperature Resources, Coproduced Fluids from Oil and Gas Wells, and Geopressured Resources Project Type / Topic 3 Low Temperature Resources Project Description The proposed two-year project supports the DOE GTP's goal of promoting the development and commercial application of energy production from low-temperature geothermal fluids, i.e., between 150°F and 300°F. State Nevada Objectives Demonstrate the technical and economic feasibility of electricity generation from nonconventional geothermal resources of 205°F using the first commercial use of a cycle at a geothermal power plant inlet temperature of less than 300°F.

194

Russell Hulse, the First Binary Pulsar, and Science Education  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Russell Hulse, the First Binary Pulsar, and Science Education Russell Hulse, the First Binary Pulsar, and Science Education Resources with Additional Information 'Dr. Russell A. Hulse of Princeton University, the discoverer of the first binary pulsar and co-recipient of the 1993 Nobel Prize in physics, will affiliate with The University of Texas at Dallas (UTD) as a visiting professor of physics and of science and math education, beginning in January 2004. Russell Hulse Courtesy Princeton Plasma Physics Laboratory Hulse will be involved with developing innovative science and mathematics education programs for primary and secondary schools, including those in several Texas school districts, as well as with developing activities in more informal settings, such as libraries. During his appointment at UTD, Hulse will retain his affiliation with Princeton University, where he is a principal research physicist at the U.S. Department of Energy's Princeton Plasma Physics Laboratory.

195

Subdwarf B binaries in the Edinburgh-Cape Survey  

E-Print Network [OSTI]

We give an update of the results of a campaign to obtain orbital solutions of subdwarf B stars from the Edinburgh-Cape survey (Stobie et al. 1997). To date we have obtained blue spectra of 40 subdwarf B stars from the Edinburgh-Cape catalogue using the grating spectrograph at the 1.9m Radcliffe telescope at the South African Astronomical Observatory. We find that 17 out of these 40 are certain binaries with a few other objects showing radial velocity variations of small amplitude. The binary fraction found in our sample, after correcting for our binary detection efficiency, is 48%. We have secured the orbital parameters for 4 of the 17 systems and narrowed down the orbits of another 7 to a small range of periods.

L. Morales-Rueda; P. F. L. Maxted; T. R. Marsh; D. Kilkenny; D. O'Donoghue

2005-09-12T23:59:59.000Z

196

The orbital period distribution of subdwarf B binaries  

E-Print Network [OSTI]

We present the results of a 3.5 year long campaign to measure orbital periods of subdwarf B (sdB) star binaries. We directly compare our observed orbital period distribution with that predicted by using binary population synthesis. Up to now, most of our systems seem to have been formed through two of the formation channels discussed by Han et al.(2003), i.e. the first and the second common envelope ejection (CE) channels. At this point, thanks to the long baseline of our observations, we are starting to detect also very long orbital period systems. These have probably come from a complete different formation path, the first stable Roche Lobe overflow (RLOF) channel in which the first mass transfer phase is stable. This channel is expected to lead to the formation of very wide binaries with orbital periods ranging between 0.5 to 2000 days.

L. Morales-Rueda; P. F. L. Maxted; T. R. Marsh

2003-09-03T23:59:59.000Z

197

Magnetic fields of neutron stars in X-ray binaries  

E-Print Network [OSTI]

A substantial fraction of the known neutron stars resides in X-ray binaries -- systems in which one compact object accretes matter from a companion star. Neutron stars in X-ray binaries have magnetic fields among the highest found in the Universe, spanning at least the range from $\\sim10^8$ to several 10$^{13}$ G. The magnetospheres around these neutron stars have a strong influence on the accretion process, which powers most of their emission. The magnetic field intensity and geometry, are among the main factors responsible for the large variety of spectral and timing properties observed in the X-ray energy range, making these objects unique laboratories to study the matter behavior and the radiation processes in magnetic fields unaccessible on Earth. In this paper we review the main observational aspects related to the presence of magnetic fields in neutron star X-ray binaries and some methods that are used to estimate their strength.

Revnivtsev, Mikhail

2014-01-01T23:59:59.000Z

198

Determining the Porosity and Saturated Hydraulic Conductivity of Binary Mixtures  

SciTech Connect (OSTI)

Gravels and coarse sands make up significant portions of some environmentally important sediments, while the hydraulic properties of the sediments are typically obtained in the laboratory using only the fine fraction (e.g., <2 mm or 4.75 mm). Researchers have found that the content of gravel has significant impacts on the hydraulic properties of the bulk soils. Laboratory experiments were conducted to measure the porosity and the saturated hydraulic conductivity of binary mixtures with different fractions of coarse and fine components. We proposed a mixing-coefficient model to estimate the porosity and a power-averaging method to determine the effective particle diameter and further to predict the saturated hydraulic conductivity of binary mixtures. The proposed methods could well estimate the porosity and saturated hydraulic conductivity of the binary mixtures for the full range of gravel contents and was successfully applied to two data sets in the literature.

Zhang, Z. F.; Ward, Anderson L.; Keller, Jason M.

2009-09-27T23:59:59.000Z

199

COMPACT BINARY PROGENITORS OF SHORT GAMMA-RAY BURSTS  

SciTech Connect (OSTI)

In recent years, detailed observations and accurate numerical simulations have provided support to the idea that mergers of compact binaries containing either two neutron stars (NSs) or an NS and a black hole (BH) may constitute the central engine of short gamma-ray bursts (SGRBs). The merger of such compact binaries is expected to lead to the production of a spinning BH surrounded by an accreting torus. Several mechanisms can extract energy from this system and power the SGRBs. Here we connect observations and numerical simulations of compact binary mergers, and use the current sample of SGRBs with measured energies to constrain the mass of their powering tori. By comparing the masses of the tori with the results of fully general-relativistic simulations, we are able to infer the properties of the binary progenitors that yield SGRBs. By assuming a constant efficiency in converting torus mass into jet energy, {epsilon}{sub jet} = 10%, we find that most of the tori have masses smaller than 0.01 M{sub Sun }, favoring 'high-mass' binary NSs mergers, i.e., binaries with total masses {approx}> 1.5 the maximum mass of an isolated NS. This has important consequences for the gravitational wave signals that may be detected in association with SGRBs, since 'high-mass' systems do not form a long-lived hypermassive NS after the merger. While NS-BH systems cannot be excluded to be the engine of at least some of the SGRBs, the BH would need to have an initial spin of {approx}0.9 or higher.

Giacomazzo, Bruno [JILA, University of Colorado and National Institute of Standards and Technology, Boulder, CO 80309 (United States); Perna, Rosalba [JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States); Rezzolla, Luciano [Max-Planck-Institut fuer Gravitationsphysik, Albert-Einstein-Institut, Potsdam D-14476 (Germany); Troja, Eleonora [NASA Goddard Space Flight Center, Greenbelt, MD 20771 (United States); Lazzati, Davide [Department of Physics, NC State University, 2401 Stinson Drive, Raleigh, NC 27695-8202 (United States)

2013-01-10T23:59:59.000Z

200

Binary fish passage models for uniform and nonuniform flows  

SciTech Connect (OSTI)

Binary fish passage models are considered by many fisheries managers to be the best 21 available practice for culvert inventory assessments and for fishway and barrier design. 22 Misunderstandings between different binary passage modeling approaches often arise, 23 however, due to differences in terminology, application and presentation. In this paper 24 one-dimensional binary fish passage models are reviewed and refined to clarify their 25 origins and applications. For uniform flow, a simple exhaustion-threshold (ET) model 26 equation is derived that predicts the flow speed threshold in a fishway or velocity barrier 27 that causes exhaustion at a given maximum distance of ascent. Flow speeds at or above 28 the threshold predict failure to pass (exclusion). Flow speeds below the threshold predict 29 passage. The binary ET model is therefore intuitive and easily applied to predict passage 30 or exclusion. It is also shown to be consistent with the distance-maximizing model. The 31 ET model s limitation to uniform flow is addressed by deriving a passage model that 32 accounts for nonuniform flow conditions more commonly found in the field, including 33 backwater profiles and drawdown curves. Comparison of these models with 34 experimental observations of volitional passage for Gambusia affinis in uniform and 35 nonuniform flows indicates reasonable prediction of binary outcomes (passage or 36 exclusion) if the flow speed is not near the threshold flow velocity. More research is 37 needed on fish behavior, passage strategies under nonuniform flow regimes and 38 stochastic methods that account for individual differences in swimming performance at or 39 near the threshold flow speed. Future experiments should track and measure ground 40 speeds of ascending fish to test nonuniform flow passage strategies and to improve model 41 predictions. Stochastic models, such as Monte-Carlo techniques, that account for 42 different passage performance among individuals and allow prediction of the percentage 43 of fish passing would be particularly useful near flow speed thresholds where binary 44 passage models are clearly limited.

Neary, Vincent S [ORNL

2011-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


201

Search for gravitational waves from binary black hole inspiral, merger, and ringdown  

E-Print Network [OSTI]

We present the first modeled search for gravitational waves using the complete binary black-hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched ...

Barnum, Sam

202

E-Print Network 3.0 - accreting x-ray binaries Sample Search...  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

Collection: Physics 27 Broad-band spectral properties of accreting X-ray binary pulsars Mauro Orlandini * Summary: Broad-band spectral properties of accreting X-ray binary pulsars...

203

E-Print Network 3.0 - accreting low-mass binary Sample Search...  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

C channel to form the Galactic low mass BH binaries... , and for the occurrence of gamma-ray bursts from collapsars in binaries. Rotational eects in accreting white dwarfs......

204

Estimation of the error for small-sample optimal binary filter design using prior knowledge  

E-Print Network [OSTI]

Optimal binary filters estimate an unobserved ideal quantity from observed quantities. Optimality is with respect to some error criterion, which is usually mean absolute error MAE (or equivalently mean square error) for the binary values. Both...

Sabbagh, David L

1999-01-01T23:59:59.000Z

205

Numerical studies of hypersonic binary gas-mixture flows near a sphere  

E-Print Network [OSTI]

Numerical studies of hypersonic binary gas-mixture flows near a sphere V.V. Riabov 1 Diffusive] to study the flow. In the present study, diffusive effects in hypersonic flows of binary gas-mixtures near

Riabov, Vladimir V.

206

Subdwarf B Binaries from the Edinburgh--Cape Survey  

E-Print Network [OSTI]

We present the first results of a campaign to obtain orbital solutions of subdwarf B (sdB) stars from the Edinburgh-Cape survey. We have obtained blue spectra of 35 sdBs, 20 of which have been observed in more than two epochs. 15 out of the 35 are certain binaries with a few other objects showing radial velocity variations with small amplitude, possibly long period sdB binaries. We have secured the orbital parameters for 2 of the 15 systems and narrowed down the orbits of another one to a small range of periods. These preliminary results only use data taken up to December 2003.

L. Morales-Rueda; P. F. L. Maxted; T. R. Marsh; D. Kilkenny; D. O'Donoghue

2004-10-11T23:59:59.000Z

207

Implementation of a low power adaptive binary encoder  

E-Print Network [OSTI]

encoder is the BinaryEncoder block. This is the block which contains the most original design and the key to the adaptive portion for 30 P robability aout[5:0] bout[5:0] cout[5:0] dout[5:0] eout[5:0] fout[5:0] gout[5:0] newprob ttl& O'U 8 u- 0) I C... FIGURE 19 Probability symbol next countertotal d D countera counterb counterc counterd aout bout cout dout countere counterl counter tout gout FIGURE 20 Probability schematic 31 this adaptive binary encoder. Figure 21 shows the input...

Herrin, Scott W

2012-06-07T23:59:59.000Z

208

Particle acceleration in the colliding winds binary WR140  

E-Print Network [OSTI]

Massive WR+O star systems produce high-temperature, shock-heated plasma where the wind of the WR star and that of its binary companion collide - the wind-collision region (WCR). The WCR is a source of thermal (e.g. hard X-rays) and non-thermal (e.g. synchrotron) emission, the latter arising from electrons and ions accelerated to relativistic energies. These colliding wind binaries provide an excellent laboratory for the study of particle acceleration at higher mass, photon and magnetic energy densities than exist in SNRs. Recent models of the non-thermal emission from WR 140 have provided insight into this process.

J. M. Pittard; S. M. Dougherty

2007-03-23T23:59:59.000Z

209

Radio emission from Colliding-Wind Binaries: Observations and Models  

E-Print Network [OSTI]

We have developed radiative transfer models of the radio emission from colliding-wind binaries (CWB) based on a hydrodynamical treatment of the wind-collision region (WCR). The archetype of CWB systems is the 7.9-yr period binary WR140, which exhibits dramatic variations at radio wavelengths. High-resolution radio observations of WR140 permit a determination of several system parameters, particularly orbit inclination and distance, that are essential for any models of this system. A model fit to data at orbital phase 0.9 is shown, and some short comings of our model described.

S. M. Dougherty; J. M. Pittard; E. P. O'Connor

2005-10-18T23:59:59.000Z

210

A characterisation of the complexity of forbidding subproblems in binary Max-CSP  

Science Journals Connector (OSTI)

Tractable classes of binary CSP and binary Max-CSP have recently been discovered by studying classes of instances defined by excluding subproblems. In this paper we characterise the complexity of all classes of binary Max-CSP instances defined by forbidding ...

Martin C. Cooper; Guillaume Escamocher; Stanislav ivn

2012-10-01T23:59:59.000Z

211

ATLAS Binary Readout IC (ABC) Specification V5.01 21Jul1999 Project Specification  

E-Print Network [OSTI]

ATLAS Binary Readout IC (ABC) Specification V5.01 21­Jul­1999 Project Specification Project Name: ATLAS ATLAS Binary Readout IC (ABC) Specification V5.01 21­Jul­1999 Table of Contents 1. SCOPE . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 7 1.1. ATLAS BINARY FRONT END READOUT ARCHITECTURE

California at Santa Cruz, University of

212

ATLAS Binary Readout IC (ABC) Specification V5.01 21-Jul-1999 Project Specification  

E-Print Network [OSTI]

Page 1 ATLAS Binary Readout IC (ABC) Specification V5.01 21-Jul-1999 Project Specification Project Name: ATLAS Binary Chip (ABC) Version: 5.01 Revision History Revision Change Description, Pages Revised and formatting. M. French 21-Jul-99 #12;Page 2 ATLAS Binary Readout IC (ABC) Specification V5.01 21-Jul-1999

California at Santa Cruz, University of

213

Accurate and efficient waveforms for compact binaries on eccentric orbits  

E-Print Network [OSTI]

Compact binaries that emit gravitational waves in the sensitivity band of ground-based detectors can have non-negligible eccentricities just prior to merger, depending on the formation scenario. We develop a purely analytic, frequency-domain model for gravitational waves emitted by compact binaries on orbits with small eccentricity, which reduces to the quasi-circular post-Newtonian approximant TaylorF2 at zero eccentricity and to the post-circular approximation of Yunes et al. (2009) at small eccentricity. Our model uses a spectral approximation to the (post-Newtonian) Kepler problem to model the orbital phase as a function of frequency, accounting for eccentricity effects up to ${\\cal{O}}(e^8)$ at each post-Newtonian order. Our approach accurately reproduces an alternative time-domain eccentric waveform model for eccentricities $e\\in [0, 0.4]$ and binaries with total mass less than 12 solar masses. As an application, we evaluate the signal amplitude that eccentric binaries produce in different networks of existing and forthcoming gravitational waves detectors. Assuming a population of eccentric systems containing black holes and neutron stars that is uniformly distributed in co-moving volume, we estimate that second generation detectors like Advanced LIGO could detect approximately 0.1-10 events per year out to redshift $z\\sim 0.2$, while an array of Einstein Telescope detectors could detect hundreds of events per year to redshift $z \\sim 2.3$.

E. A. Huerta; Prayush Kumar; Sean T. McWilliams; Richard O'Shaughnessy; Nicolas Yunes

2014-08-14T23:59:59.000Z

214

MULTIWAVELENGTH OBSERVATIONS OF THE RUNAWAY BINARY HD 15137  

SciTech Connect (OSTI)

HD 15137 is an intriguing runaway O-type binary system that offers a rare opportunity to explore the mechanism by which it was ejected from the open cluster of its birth. Here, we present recent blue optical spectra of HD 15137 and derive a new orbital solution for the spectroscopic binary and physical parameters of the O star primary. We also present the first XMM-Newton observations of the system. Fits of the EPIC spectra indicate soft, thermal X-ray emission consistent with an isolated O star. Upper limits on the undetected hard X-ray emission place limits on the emission from a proposed compact companion in the system, and we rule out a quiescent neutron star (NS) in the propeller regime or a weakly accreting NS. An unevolved secondary companion is also not detected in our optical spectra of the binary, and it is difficult to conclude that a gravitational interaction could have ejected this runaway binary with a low mass optical star. HD 15137 may contain an elusive NS in the ejector regime or a quiescent black hole with conditions unfavorable for accretion at the time of our observations.

McSwain, M. Virginia; Aragona, Christina; Marsh, Amber N.; Roettenbacher, Rachael M. [Department of Physics, Lehigh University, Bethlehem, PA 18015 (United States); De Becker, Michael [Institut d'Astrophysique et Geophysique, Universite de Liege, FNRS (Belgium); Roberts, Mallory S. E. [Eureka Scientific, Inc., Oakland, CA 94602-3017 (United States); Boyajian, Tabetha S.; Gies, Douglas R. [Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30302-4106 (United States); Grundstrom, Erika D. [Physics and Astronomy Department, Vanderbilt University, Nashville, TN 37235 (United States)], E-mail: mcswain@lehigh.edu, E-mail: cha206@lehigh.edu, E-mail: anm506@lehigh.edu, E-mail: rmr207@lehigh.edu, E-mail: debecker@astro.ulg.ac.be, E-mail: malloryr@gmail.com, E-mail: tabetha@chara.gsu.edu, E-mail: gies@chara.gsu.edu, E-mail: erika.grundstrom@vanderbilt.edu

2010-03-15T23:59:59.000Z

215

Synthesis and characterization of nanocrystalline binary and ternary intermetallic compounds  

E-Print Network [OSTI]

nanocrystalline powders. Using this process, I was able to access several binary and ternary intermetallics, including two new phases: AuCuSn2 and AuNiSn2. These compounds were isolated as nanocrystals using low temperature solution synthesis techniques, which had...

Leonard, Brian Matthew

2009-05-15T23:59:59.000Z

216

Exploiting the relationships among several binary classifiers via data transformation  

Science Journals Connector (OSTI)

The structural resemblance among several existing classifiers has motivated us to investigate their underlying relationships. By exploring into the mapping solutions of these classifiers, we found that they can be linked by simple feature data scaling. ... Keywords: Area under the ROC curve, Binary classification, Deterministic methods, Linear estimation methods

Kar-Ann Toh; Geok-Choo Tan

2014-03-01T23:59:59.000Z

217

Capture Formed Binaries via Encounters with Massive Protostars  

E-Print Network [OSTI]

Most massive stars are found in the center of dense clusters, and have a companion fraction much higher than their lower mass siblings; the massive stars of the Trapezium core in Orion have ~ 1.5 companions each. This high multiplicity could be a consequence of formation via a capture scenario, or it could be due to fragmentation of the cores that form the massive stars. During stellar formation circumstellar disks appear to be nearly ubiquitous. Their large radii compared to stellar sizes increase the interaction radius significantly, suggesting that disk interactions with neighboring stars could assist in capturing binary companions. This mechanism has been studied for stars of approximately solar mass and found to be inefficient. In this paper we present simulations of interactions between a 22 Msun star-disk system and less massive impactors, to study the disk-assisted capture formation of binaries in a regime suited to massive stars. The formation of binaries by capture is found to be much more efficient for massive capturers. We discuss the effects of a mass dependent velocity dispersion and mass segregation on the capture rates, and consider the long term survival of the resultant binaries in a dense cluster.

Nickolas Moeckel; John Bally

2006-10-20T23:59:59.000Z

218

Invertible Symmetric 3 3 Binary Matrices and GQ(2, 4)  

E-Print Network [OSTI]

Invertible Symmetric 3 ? 3 Binary Matrices and GQ(2, 4) Andrea Blunck,1 P´eter L´evay,2 Metod of 27 (disregarding the identity) invertible symmetric 3 ? 3 matrices over GF(2) and the points of invertible symmetric 3 ? 3 matrices over the field GF(2) has 28 elements. The elements different from

Paris-Sud XI, Université de

219

A detection pipeline for galactic binaries in LISA data  

E-Print Network [OSTI]

The Galaxy is suspected to contain hundreds of millions of binary white dwarf systems, a large fraction of which will have sufficiently small orbital period to emit gravitational radiation in band for space-based gravitational wave detectors such as the Laser Interferometer Space Antenna (LISA). LISA's main science goal is the detection of cosmological events (supermassive black hole mergers, etc.) however the gravitational signal from the galaxy will be the dominant contribution to the data -- including instrumental noise -- over approximately two decades in frequency. The catalogue of detectable binary systems will serve as an unparalleled means of studying the Galaxy. Furthermore, to maximize the scientific return from the mission, the data must be "cleansed" of the galactic foreground. We will present an algorithm that can accurately resolve and subtract >10000 of these sources from simulated data supplied by the Mock LISA Data Challenge Task Force. Using the time evolution of the gravitational wave frequency, we will reconstruct the position of the recovered binaries and show how LISA will sample the entire compact binary population in the Galaxy.

Tyson B. Littenberg

2011-06-30T23:59:59.000Z

220

Optimization Methods for Binary Sequences The Merit Factor Problem  

E-Print Network [OSTI]

Optimization Methods for Binary Sequences ­ The Merit Factor Problem Ron Ferguson, Joshua Knauer SFU MOCAA Project Leader: Peter Borwein MITACS 6th Annual Conference, May, 2005 Abstract Optimization of much interest in combinatorial optimization, communications engineering, and analytic number theory

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


221

Dixie Valley Binary Cycle Production Data 2013 YTD  

SciTech Connect (OSTI)

Proving the technical and economic feasibility of utilizing the available unused heat to generate additional electric power from a binary power plant from the low-temperature brine at the Dixie Valley Geothermal Power Plant. Monthly data for Jan 2013-September 2013

Lee, Vitaly

2013-10-18T23:59:59.000Z

222

COMPARISON OF KERNELBASED MODELS FOR BINARY CLASSIFICATION OF ENVIRONMENTAL DATA  

E-Print Network [OSTI]

1 COMPARISON OF KERNEL­BASED MODELS FOR BINARY CLASSIFICATION OF ENVIRONMENTAL DATA V. Polishchuk ABSTRACT The task of real­world environmental data classification was approached with different models simulation -- which arise in environmental modeling, classification between two classes may be considered

223

Addendum to Heat and matter transport in binary liquid mixtures  

Science Journals Connector (OSTI)

We recently presented nonequilibrium molecular dynamics simulations of coupled heat and matter transport in a binary liquid mixture. While these simulations were carried out exactly as indicated, the relations given between the microscopic and macroscopic formalism were strictly wrong. Here we correct these errors and indicate how they limit the possibilities for comparison of our simulation results with experiment.

Denis J. Evans and David MacGowan

1987-07-15T23:59:59.000Z

224

Production and Injection data for NV Binary facilities  

DOE Data Explorer [Office of Scientific and Technical Information (OSTI)]

Excel files are provided with well production and injection data for binary facilities in Nevada. The files contain the data that reported montly to the Nevada Bureau of Mines and Geology (NBMG) by the facility operators. this data has been complied into Excel spreadsheets for each of the facilities given on the NBMG web site.

Mines, Greg

225

Landscape statistics of the low autocorrelated binary string problem  

E-Print Network [OSTI]

Landscape statistics of the low autocorrelated binary string problem Fernando F. Ferreiraa , Jos, NM 87501, USA Abstract. The statistical properties of the energy landscape of the low autocorrelated disordered models. Using two global measures of landscape structure which have been introduced

Stadler, Peter F.

226

Landscape statistics of the low autocorrelated binary string problem  

E-Print Network [OSTI]

Landscape statistics of the low autocorrelated binary string problem Fernando F. Ferreira a , Jos, NM 87501, USA Abstract. The statistical properties of the energy landscape of the low autocorrelated disordered models. Using two global measures of landscape structure which have been introduced

Stadler, Peter F.

227

Vacancy mediated substitutional diffusion in binary crystalline solids  

E-Print Network [OSTI]

Vacancy mediated substitutional diffusion in binary crystalline solids Anton Van der Ven a,*, Hui coefficients of substi- tutional alloys from first principles. The focus is restricted to vacancy mediated and grain boundaries that can act as vacancy sources) and diffusion in a solid containing a continuous

Ceder, Gerbrand

228

COLLISIONAL EVOLUTION OF ULTRA-WIDE TRANS-NEPTUNIAN BINARIES  

SciTech Connect (OSTI)

The widely separated, near-equal mass binaries hosted by the cold classical Kuiper Belt are delicately bound and subject to disruption by many perturbing processes. We use analytical arguments and numerical simulations to determine their collisional lifetimes given various impactor size distributions and include the effects of mass loss and multiple impacts over the lifetime of each system. These collisional lifetimes constrain the population of small (R {approx}> 1 km) objects currently residing in the Kuiper Belt and confirm that the size distribution slope at small size cannot be excessively steep-likely q {approx}< 3.5. We track mutual semimajor axis, inclination, and eccentricity evolution through our simulations and show that it is unlikely that the wide binary population represents an evolved tail of the primordially tight binary population. We find that if the wide binaries are a collisionally eroded population, their primordial mutual orbit planes must have preferred to lie in the plane of the solar system. Finally, we find that current limits on the size distribution at small radii remain high enough that the prospect of detecting dust-producing collisions in real time in the Kuiper Belt with future optical surveys is feasible.

Parker, Alex H. [Department of Astronomy, University of Victoria, Victoria BC (Canada); Kavelaars, J. J., E-mail: alexhp@uvic.ca [Herzberg Institute of Astrophysics, National Research Council of Canada, Saanich BC (Canada)

2012-01-10T23:59:59.000Z

229

SPECTROSCOPIC METALLICITY DETERMINATIONS FOR W UMa-TYPE BINARY STARS  

SciTech Connect (OSTI)

This study is the first attempt to determine the metallicities of W UMa-type binary stars using spectroscopy. We analyzed about 4500 spectra collected at the David Dunlap Observatory. To circumvent problems caused by the extreme spectral line broadening and blending and by the relatively low quality of the data, all spectra were subject to the same broadening function (BF) processing to determine the combined line strength in the spectral window centered on the Mg I triplet between 5080 A and 5285 A. All individual integrated BFs were subsequently orbital-phase averaged to derive a single line-strength indicator for each star. The star sample was limited to 90 W UMa-type (EW) binaries with the strict phase-constancy of colors and without spectral contamination by spectroscopic companions. The best defined results were obtained for an F-type sub-sample (0.32 < (B - V){sub 0} < 0.62) of 52 binaries for which integrated BF strengths could be interpolated in the model atmosphere predictions. The logarithmic relative metallicities, [M/H], for the F-type sub-sample indicate metal abundances roughly similar to the solar metallicity, but with a large scatter which is partly due to combined random and systematic errors. Because of the occurrence of a systematic color trend resulting from inherent limitations in our approach, we were forced to set the absolute scale of metallicities to correspond to that derived from the m{sub 1} index of the Stroemgren uvby photometry for 24 binaries of the F-type sub-sample. The trend-adjusted metallicities [M/H]{sub 1} are distributed within -0.65 < [M/H]{sub 1} < +0.50, with the spread reflecting genuine metallicity differences between stars. One half of the F-sub-sample binaries have [M/H]{sub 1} within -0.37 < [M/H]{sub 1} < +0.10, a median of -0.04 and a mean of -0.10, with a tail toward low metallicities, and a possible bias against very high metallicities. A parallel study of kinematic data, utilizing the most reliable and recently obtained proper motion and radial velocity data for 78 binaries of the full sample, shows that the F-type sub-sample binaries (44 stars with both velocities and metallicity determinations) have similar kinematic properties to solar-neighborhood, thin-disk dwarfs with space velocity component dispersions: {sigma}U = 33 km s{sup -1}, {sigma}V = 23 km s{sup -1} and {sigma}W = 14 km s{sup -1}. FU Dra with a large spatial velocity, V{sub tot} = 197 km s{sup -1} and [M/H]{sub 1} = -0.6 {+-} 0.2, appears to be the only thick-disk object in the F-type sub-sample. The kinematic data indicate that the F-type EW binaries are typical, thin-disk population stars with ages about 3-5.5 Gyr. The F-type binaries that appear to be older than the rest tend to have systematically smaller mass ratios than most of the EW binaries of the same period.

Rucinski, Slavek M. [Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4 (Canada); Pribulla, Theodor; Budaj, Jan, E-mail: rucinski@astro.utoronto.ca, E-mail: pribulla@ta3.sk, E-mail: budaj@ta3.sk [Astronomical Institute, Slovak Academy of Sciences, 059 60 Tatranska Lomnica (Slovakia)

2013-09-15T23:59:59.000Z

230

Training a Binary Classifier with the Quantum Adiabatic Algorithm  

E-Print Network [OSTI]

This paper describes how to make the problem of binary classification amenable to quantum computing. A formulation is employed in which the binary classifier is constructed as a thresholded linear superposition of a set of weak classifiers. The weights in the superposition are optimized in a learning process that strives to minimize the training error as well as the number of weak classifiers used. No efficient solution to this problem is known. To bring it into a format that allows the application of adiabatic quantum computing (AQC), we first show that the bit-precision with which the weights need to be represented only grows logarithmically with the ratio of the number of training examples to the number of weak classifiers. This allows to effectively formulate the training process as a binary optimization problem. Solving it with heuristic solvers such as tabu search, we find that the resulting classifier outperforms a widely used state-of-the-art method, AdaBoost, on a variety of benchmark problems. Moreover, we discovered the interesting fact that bit-constrained learning machines often exhibit lower generalization error rates. Changing the loss function that measures the training error from 0-1 loss to least squares maps the training to quadratic unconstrained binary optimization. This corresponds to the format required by D-Wave's implementation of AQC. Simulations with heuristic solvers again yield results better than those obtained with boosting approaches. Since the resulting quadratic binary program is NP-hard, additional gains can be expected from applying the actual quantum processor.

Hartmut Neven; Vasil S. Denchev; Geordie Rose; William G. Macready

2008-11-04T23:59:59.000Z

231

BOWLING GREEN STATE UNIVERSITY is the owner of all rights, title and interest in and to the following Indicia, which includes trademarks, service marks, trade names, designs, logos, seals and symbols.  

E-Print Network [OSTI]

APPENDIX B BOWLING GREEN STATE UNIVERSITY is the owner of all rights, title and interest GREEN STATE UNIVERSITY shall be deemed to be additions to the Indicia as though shown above and shall 1126 BLACK WHITE RA TBD RA 2273 BLACK WHITE NOTE: The marks of Bowling Green State University

Moore, Paul A.

232

Motion compensation method for moving pictures with binary shape  

Science Journals Connector (OSTI)

This paper describes a motion compensation method for arbitrarily shaped moving visual objects. To utilise both the inter-frame correlation and the texture-shape correlation, we use macroblock-based motion compensation for binary shape coding as well as texture coding. To efficiently achieve motion compensation for a moving binary shape, we introduce extra motion vectors for the shape coding in addition to the texture motion vectors, where the shape motion vectors are coded by referring to the texture motion vectors. The proposed method can successfully save more than 50% of the number of bits in comparison with the intra-only method. The effectiveness of the proposed method has been established through MPEG4 standardisation activity, and the proposed motion-compensation framework has been adopted by the MPEG-4 visual coding standard (ISO 14496-2).

Shinya Kadono; Choong Seng Boon; Minoru Etoh

2000-01-01T23:59:59.000Z

233

General Relativistic Binary Merger Simulations and Short Gamma Ray Bursts  

E-Print Network [OSTI]

The recent localization of some short-hard gamma ray bursts (GRBs) in galaxies with low star formation rates has lent support to the suggestion that these events result from compact object binary mergers. We discuss how new simulations in general relativity are helping to identify the central engine of short-hard GRBs. Motivated by our latest relativistic black hole-neutron star merger calculations, we discuss a scenario in which these events may trigger short-hard GRBs, and compare this model to competing relativistic models involving binary neutron star mergers and the delayed collapse of hypermassive neutron stars. Distinguishing features of these models may help guide future GRB and gravitational wave observations to identify the nature of the sources.

Joshua A. Faber; Thomas W. Baumgarte; Stuart L. Shapiro; Keisuke Taniguchi

2006-03-10T23:59:59.000Z

234

Supersaturated Turbine Expansions for Binary Geothermal Power Plants  

SciTech Connect (OSTI)

The Heat Cycle Research project is developing the technology base that will permit a much greater utilization of the moderate-temperature, liquid-dominated geothermal resources, particularly for the generation of electrical power. The emphasis in the project has been the improvement of the performance of binary power cycles. The investigations have been examining concepts projected to improve the brine utilization by 20% relative to a ''Heber-type'' binary plant; these investigations are nearing completion. preparations are currently underway in the project to conduct field investigations of the condensation behavior of supersaturated turbine expansions. These investigations will evaluate whether the projected additional 8% to 10% improvement in brine utilization can be realized by allowing these expansions. Future program efforts will focus on the problems associated with heat rejection and on the transfer of the technology being developed to industry.

Bliem, C.J.; Mines, G.L.

1992-03-24T23:59:59.000Z

235

Vibrated polar disks: spontaneous motion, binary collisions, and collective dynamics  

E-Print Network [OSTI]

We study the spontaneous motion, binary collisions, and collective dynamics of "polar disks", i.e. purpose-built particles which, when vibrated between two horizontal plates, move coherently along a direction strongly correlated to their intrinsic polarity. The motion of our particles, although nominally three-dimensional and complicated, is well accounted for by a two-dimensional persistent random walk. Their binary collisions are spatiotemporally extended events during which multiple actual collisions happen, yielding a weak average effective alignment. We show that this well-controlled, "dry active matter" system can display collective motion with orientationally-ordered regions of the order of the system size. We provide evidence of strong number density in the most ordered regimes observed. These results are discussed in the light of the limitations of our system, notably those due to the inevitable presence of walls.

Julien Deseigne; Sbastien Lonard; Olivier Dauchot; Hugues Chat

2012-01-29T23:59:59.000Z

236

Short Gamma-Ray Bursts from Binary Neutron Star Mergers  

E-Print Network [OSTI]

We present the results from new relativistic hydrodynamic simulations of binary neutron star mergers using realistic non-zero temperature equations of state. We vary several unknown parameters in the system such as the neutron star (NS) masses, their spins and the nuclear equation of state. The results are then investigated with special focus on the post-merger torus-remnant system. Observational implications on the Gamma-ray burst (GRB) energetics are discussed and compared with recent observations.

Roland Oechslin; Thomas Janka

2006-04-27T23:59:59.000Z

237

Coal liquefaction process using pretreatment with a binary solvent mixture  

DOE Patents [OSTI]

An improved process for thermal solvent refining or hydroliquefaction of non-anthracitic coal at elevated temperatures under hydrogen pressure in a hydrogen donor solvent comprises pretreating the coal with a binary mixture of an aromatic hydrocarbon and an aliphatic alcohol at a temperature below 300 C before the hydroliquefaction step. This treatment generally increases both conversion of coal and yields of oil. 1 fig.

Miller, R.N.

1986-10-14T23:59:59.000Z

238

Gravitational-wave modes from precessing black-hole binaries  

E-Print Network [OSTI]

Gravitational waves from precessing black-hole binaries exhibit features that are absent in nonprecessing systems. The most prominent of these is a parity-violating asymmetry that beams energy and linear momentum preferentially along or opposite to the orbital angular momentum, leading to recoil of the binary. The asymmetry will appear as amplitude and phase modulations at the orbital frequency. For strongly precessing systems, it accounts for at least 3% amplitude modulation for binaries in the sensitivity band of ground-based gravitational-wave detectors, and can exceed 50% for massive systems. Such asymmetric features are also clearly visible when the waves are decomposed into modes of spin-weighted spherical harmonics, and are inherent in the waves themselves---rather than resulting from residual eccentricity in numerical simulations, or from mode-mixing due to precession. In particular, there is generically no instantaneous frame for which the mode decomposition will have any symmetry. We introduce a method to simplify the expressions for waveforms given in analytical relativity, which can be used to combine existing high-order waveforms for nonprecessing systems with expressions for the precessing contributions, leading to improved accuracy and a unified treatment of precessing and nonprecessing binaries. Using this method, it is possible to clarify the nature and the origins of the asymmetries and show the effects of asymmetry on recoils more clearly. We present post-Newtonian (PN) expressions for the waveform modes that include these terms, complete to the relative 2PN level in spin (proportional to $v^4/c^4$ times a certain combination of the spins). Comparing the results of those expressions to numerical results, we find good qualitative agreement. We also demonstrate how these expressions can be used to efficiently calculate waveforms for gravitational-wave astronomy.

Michael Boyle; Lawrence E. Kidder; Serguei Ossokine; Harald P. Pfeiffer

2014-09-15T23:59:59.000Z

239

The Binary Nature of PSR J2032+4127  

E-Print Network [OSTI]

PSR J2032+4127 is a gamma-ray and radio-emitting pulsar which has been regarded as a young luminous isolated neutron star. However, its recent spin-down rate has extraordinarily increased by a factor of two. We present evidence that this is due to its motion as a member of a highly-eccentric binary system with a 15-solar-mass Be star, MT91~213. Timing observations show that, not only are the positions of the two stars coincident within 0.4 arcsec, but timing models of binary motion of the pulsar fit the data much better than a model of a young isolated pulsar. MT91~213, and hence the pulsar, lie in the Cyg~OB2 stellar association, which is at a distance of only 1.4-1.7 kpc. The pulsar is currently on the near side of, and accelerating towards, the Be star, with an orbital period of 20-30 years. The next periastron is well-constrained to occur in early 2018, providing an opportunity to observe enhanced high-energy emission as seen in other Be-star binary systems.

Lyne, Andrew; Keith, Michael; Ray, Paul; Kerr, Matthew; Camilo, Fernando; Johnson, Tyrel

2015-01-01T23:59:59.000Z

240

NuSTAR Observations of X-Ray Binaries  

E-Print Network [OSTI]

As of 2014 August, the Nuclear Spectroscopic Telescope Array (NuSTAR) had observed ~30 X-ray binaries either as part of the planned program, as targets of opportunity, or for instrument calibration. The main science goals for the observations include probing the inner part of the accretion disk and constraining black hole spins via reflection components, providing the first observations of hard X-ray emission from quiescent Low Mass X-ray Binaries (LMXBs), measuring cyclotron lines from accreting pulsars, and studying type I X-ray bursts from neutron stars. Here, we describe the science objectives in more depth and give an overview of the NuSTAR observations that have been carried out to achieve the objectives. These include observation of four "IGR" High Mass X-ray Binaries (HMXBs) discovered by INTEGRAL. We also summarize the results that have been obtained and their implications. Among the IGR HMXBs, we focus on the discovery of a cyclotron line in the spectrum of IGR J17544-2619.

Tomsick, John A; Fuerst, Felix; Harrison, Fiona; Miyasaka, Hiromasa; Tendulkar, Shriharsh; Bhalerao, Varun; Chakrabarty, Deepto; King, Ashley; Miller, Jon M; Natalucci, Lorenzo; Stern, Daniel

2015-01-01T23:59:59.000Z

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241

Terra-Gen Power and TAS Celebrate Innovative Binary Geothermal Technology |  

Open Energy Info (EERE)

and TAS Celebrate Innovative Binary Geothermal Technology and TAS Celebrate Innovative Binary Geothermal Technology Jump to: navigation, search OpenEI Reference LibraryAdd to library Web Site: Terra-Gen Power and TAS Celebrate Innovative Binary Geothermal Technology Abstract N/A Authors Terra-Gen Power and LLC Published Publisher Not Provided, Date Not Provided DOI Not Provided Check for DOI availability: http://crossref.org Online Internet link for Terra-Gen Power and TAS Celebrate Innovative Binary Geothermal Technology Citation Terra-Gen Power, LLC. Terra-Gen Power and TAS Celebrate Innovative Binary Geothermal Technology [Internet]. [updated 2011;cited 2011]. Available from: http://www.terra-genpower.com/News/TERRA-GEN-POWER-AND-TAS-CELEBRATE-INNOVATIVE-BINAR.aspx Retrieved from "http://en.openei.org/w/index.php?title=Terra-Gen_Power_and_TAS_Celebrate_Innovative_Binary_Geothermal_Technology&oldid=682514

242

Bubble-Point Measurements of Eight Binary Mixtures for Organic Rankine Cycle Applications  

Science Journals Connector (OSTI)

Bubble-Point Measurements of Eight Binary Mixtures for Organic Rankine Cycle Applications ... These mixtures are of interest as working fluids in organic Rankine power cycles. ...

Stephanie L. Outcalt; Eric W. Lemmon

2013-05-24T23:59:59.000Z

243

GridRun: A lightweight packaging and execution environment forcompact, multi-architecture binaries  

SciTech Connect (OSTI)

GridRun offers a very simple set of tools for creating and executing multi-platform binary executables. These ''fat-binaries'' archive native machine code into compact packages that are typically a fraction the size of the original binary images they store, enabling efficient staging of executables for heterogeneous parallel jobs. GridRun interoperates with existing distributed job launchers/managers like Condor and the Globus GRAM to greatly simplify the logic required launching native binary applications in distributed heterogeneous environments.

Shalf, John; Goodale, Tom

2004-02-01T23:59:59.000Z

244

Star Cluster Ecology: VII The evolution of young dense star clusters containing primordial binaries  

E-Print Network [OSTI]

We study the first 100Myr of the evolution of isolated star clusters initially containing 144179 stars, including 13107 (10%) primordial hard binaries. Our calculations include the effects of both stellar and binary evolution. Gravitational interactions among the stars are computed by direct N-body integration using high precision GRAPE-6 hardware. The evolution of the core radii and central concentrations of our simulated clusters are compared with the observed sample of young (about 100Myr) star clusters in the large Magellanic cloud. Even though our simulations start with a rich population of primordial binaries, core collapse during the early phase of the cluster evolution is not prevented. Throughout the simulations, the fraction of binaries remains roughly constant (about 10%). Due to the effects of mass segregation the mass function of intermediate-mass main-sequence stars becomes as flat as $\\alpha=-1.8$ in the central part of the cluster (where the initial Salpeter mass function had $\\alpha=-2.35$). About 6--12% of the neutron stars were retained in our simulations; the fraction of retained black holes is 40--70%. In each simulation about three neutron stars become members of close binaries with a main-sequence companion. Such a binary will eventually become an x-ray binary, when the main-sequence star starts to fill its Roche lobe. Black holes are found more frequently in binaries; in each simulated cluster we find about 11 potential x-ray binaries containing a black hole. Abstract abbreviated....

Simon Portegies Zwart; Steve McMillan; Jun Makino

2006-09-27T23:59:59.000Z

245

Robust Audio Watermarking Algorithm Based on Audio Binary Halftone Pre-process  

Science Journals Connector (OSTI)

Conventional audio watermarking method has the following deficiencies: the ... simple which reduce the security; the embedded audio watermarking is meaningless binary sequence. To address these problems, we propo...

Huan Li; Zheng Qin; XuanPing Zhang; Xu Wang

2011-01-01T23:59:59.000Z

246

Identification of Owners Project Value Interests  

E-Print Network [OSTI]

, schedule and engineering specifications that must be met; but there are other attributes of a project that are not always immediately evident; yet, when implemented, can add significant value. A delivered project that meets cost, schedule, engineering... ........................................................................ 27 Table 4 Description of Case Study Project ............................................................ 36 Table 5 Sensitivity of Meet the Cost Objective ..................................................... 37 Table 6 Sensitivity of Meet...

Gunby, Molly Gaynell

2011-02-22T23:59:59.000Z

247

Compact binary evolutions with the Z4c formulation  

Science Journals Connector (OSTI)

Numerical relativity simulations of compact binaries with the Z4c and Baumgarte-Shapiro-Shibata-Nakamura-Oohara-Kojima (BSSNOK) formulations are compared. The Z4c formulation is advantageous in every case considered. In simulations of nonvacuum spacetimes, the constraint violations due to truncation errors are between 1 and 3 orders of magnitude lower in the Z4c evolutions. Improvements are also found in the accuracy of the computed gravitational radiation. For equal-mass irrotational binary neutron star evolutions, we find that the absolute errors in phase and amplitude of the waveforms can be up to a factor of 4 smaller. The quality of the Z4c numerical data is also demonstrated by a remarkably accurate computation of the Arnowitt-Deser-Misner mass from surface integrals. For equal-mass nonspinning binary puncture black hole evolutions, we find that the absolute errors in phase and amplitude of the waveforms can be up to a factor of 2 smaller. In the same evolutions, we find that away from the punctures the Hamiltonian constraint violation is reduced by between 1 and 2 orders of magnitude. Furthermore, the utility of gravitational radiation controlling, constraint preserving boundary conditions for the Z4c formulation is demonstrated. The evolution of spacetimes containing a single compact object confirms earlier results in spherical symmetry. The boundary conditions avoid spurious and nonconvergent effects present in high resolution runs with either formulation with a more naive boundary treatment. We conclude that Z4c is preferable to BSSNOK for the numerical solution of the 3+1 Einstein equations with the puncture gauge.

David Hilditch; Sebastiano Bernuzzi; Marcus Thierfelder; Zhoujian Cao; Wolfgang Tichy; Bernd Brgmann

2013-10-30T23:59:59.000Z

248

THE AGE AND STELLAR PARAMETERS OF THE PROCYON BINARY SYSTEM  

SciTech Connect (OSTI)

The Procyon AB binary system (orbital period 40.838 yr, a newly refined determination) is near and bright enough that the component radii, effective temperatures, and luminosities are very well determined, although more than one possible solution to the masses has limited the claimed accuracy. Preliminary mass determinations for each component are available from Hubble Space Telescope imaging, supported by ground-based astrometry and an excellent Hipparcos parallax; we use these for our preferred solution for the binary system. Other values for the masses are also considered. We have employed the TYCHO stellar evolution code to match the radius and luminosity of the F5 IV-V primary star to determine the system's most likely age as 1.87 {+-} 0.13 Gyr. Since prior studies of Procyon A found its abundance indistinguishable from solar, the solar composition of Asplund, Grevesse, and Sauval (Z = 0.014) is assumed for the Hertzsprung-Russell diagram fitting. An unsuccessful attempt to fit using the older solar abundance scale of Grevesse and Sauval (Z = 0.019) is also reported. For Procyon B, 11 new sequences for the cooling of non-DA white dwarfs have been calculated to investigate the dependences of the cooling age on (1) the mass, (2) core composition, (3) helium layer mass, and (4) heavy-element opacities in the helium envelope. Our calculations indicate a cooling age of 1.19 {+-} 0.11 Gyr, which implies that the progenitor mass of Procyon B was 2.59{sub -0.26}{sup +0.44} M{sub Sun }. In a plot of initial versus final mass of white dwarfs in astrometric binaries or star clusters (all with age determinations), the Procyon B final mass lies several {sigma} below a straight line fit.

Liebert, James; Arnett, David [Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States); Fontaine, Gilles [Departement de Physique, Universite de Montreal, C.P. 6128, Succ. Centre-Ville, Montreal, Quebec H3C 3J7 (Canada); Young, Patrick A. [School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287 (United States); Williams, Kurtis A., E-mail: jamesliebert@gmail.com, E-mail: darnett@as.arizona.edu, E-mail: fontaine@astro.umontreal.ca, E-mail: pyoung.3@asu.edu, E-mail: Kurtis.Williams@tamuc.edu [Texas A and M University, Commerce, TX 75429 (United States)

2013-05-20T23:59:59.000Z

249

Investigating Binary Black Hole Mergers with Principal Component Analysis  

E-Print Network [OSTI]

Despite recent progress in numerical simulations of the coalescence of binary black hole systems, highly asymmetric spinning systems and the construction of accurate physical templates remain challenging and computationally expensive. We explore the feasibility of a prompt and robust test of whether the signals exhibit evidence for generic features that can educate new simulations. We form catalogs of numerical relativity waveforms with distinct physical effects and compute the relative probability that a gravitational wave signal belongs to each catalog. We introduce an algorithm designed to perform this task for coalescence signals using principal component analysis of waveform catalogs and Bayesian model selection and demonstrate its effectiveness.

James Clark; Laura Cadonati; James Healy; Ik Siong Heng; Josh Logue; Nicholas Mangini; Lionel London; Larne Pekowsky; Deirdre Shoemaker

2014-06-20T23:59:59.000Z

250

The Spectroscopic Orbits of Five Solar Type, Single Lined Binaries  

E-Print Network [OSTI]

We have determined spectroscopic orbits for five single-lined spectroscopic binaries, HD 100167, HD 135991, HD 140667, HD 158222, HD 217924. Their periods range from 60.6 to 2403 days and the eccentricities, from 0.20 to 0.84. Our spectral classes for the stars confirm that they are of solar type, F9 to G5, and all are dwarfs. Their [Fe/H] abundances, determined spectroscopically, are close to the solar value and on average are 0.12 greater than abundances from a photometric calibration. Four of the five stars are rotating faster than their predicted pseudosynchronous rotational velocities.

Fekel, Francis C; Muterspaugh, Matthew W; Williamson, Michael H

2014-01-01T23:59:59.000Z

251

Plastic flow in polycrystal states in a binary mixture  

E-Print Network [OSTI]

Using molecular dynamics simulation we examine dynamics in sheared polycrystal states in a binary mixture containing 10% larger particles in two dimensions. We find large stress fluctuations arising from sliding motions of the particles at the grain boundaries, which occur cooperatively to release the elastic energy stored. These dynamic processes are visualized with the aid of a sixfold angle $\\alpha_j(t)$ representing the local crystal orientation and a disorder variable $D_j(t)$ representing a deviation from the hexagonal order for particle $j$.

Toshiyuki Hamanaka; Akira Onuki

2007-09-05T23:59:59.000Z

252

Binary and multifragment decay of very hot nuclei  

SciTech Connect (OSTI)

Compound binary emission of complex fragments is illustrated for a variety of reactions. Complex fragment emission from 35 and 40 MeV/N {sup 139}La + {sup 12}C, {sup 27}Al, {sup 40}Ca and {sup 51}V reactions has been studied. Multifragment events from these reactions were assigned to sources characterized by their energy and mass through the incomplete-fusion-model kinematics. Excitation functions for the various multifragment channels appear to be nearly independent of the system and bombarding energy. Preliminary comparisons of the data with sequential-statistical-decay calculations are discussed. 14 refs., 7 figs.

Moretto, L.G.; Blumenfeld, Y.; Charity, R.J.; Wozniak, G.J.

1990-05-01T23:59:59.000Z

253

IUPAC-NIST Solubility Data Series. 78. Acetonitrile Binary Systems  

Science Journals Connector (OSTI)

The mutual solubilities and liquidliquid equilibria of acetonitrile binary systems with different compounds exhaustively and critically are reviewed. The compounds include water inorganic compounds and a variety of organic compounds (hydrocarbons halogenated hydrocarbons alcohols carboxylic acids and esters nitrogen and sulfur compounds). A total of 353 systems reported in the primary literature through 2000 are compiled. For 25 systems sufficient data are available to allow critical evaluation. All data are expressed as mass and mole fractions as well as the originally reported units. Similar reviews of gas liquid and solid solubilities for other systems are published in the of Solubility Data Series. This is the 78th volume of this series.

Valerii P. Sazonov; David G. Shaw; Valerii P. Sazonov; Nikolai V. Sazonov; Adam Skrzecz; Valerii P. Sazonov; Nikolai V. Sazonov; Nikolai I. Lisov

2002-01-01T23:59:59.000Z

254

Radial velocities of population II binary stars. II  

E-Print Network [OSTI]

Here we publish the second list of radial velocities for 91 Hipparcos stars, mostly high transverse velocity binaries without previous radial velocity measurements. The measurements of radial velocities are done with a CORAVEL-type radial velocity spectrometer with an accuracy better than 1 km/s. We also present the information on eight new radial velocity variables - HD 29696, HD 117466AB, BD +28 4035AB, BD +30 2129A, BD +39 1828AB, BD +69 230A, BD +82 565A and TYC 2267-1300-1 - found from our measurements. Two stars (HD 27961AB and HD 75632AB) are suspected as possible radial velocity variables.

A. Bartkevicius; J. Sperauskas

2006-01-10T23:59:59.000Z

255

Adaptive filters for detection of gravitational waves from coalescing binaries  

SciTech Connect (OSTI)

In this work we propose use of infinite impulse response adaptive line enhancer (IIR ALE) filters for detection of gravitational waves from coalescing binaries. We extend our previous work and define an adaptive matched filter structure. Filter performance is analyzed in terms of the tracking capability and determination of filter parameters. Furthermore, following the Neyman-Pearson strategy, receiver operating characteristics are derived, with closedform expressions for detection threshold, false alarm, and detection probability. Extensive tests demonstrate the effectiveness of adaptive filters both in terms of small computational cost and robustness.

Eleuteri, Antonio; Milano, Leopoldo; De Rosa, Rosario; Garufi, Fabio; Acernese, Fausto; Barone, Fabrizio; Giordano, Lara; Pardi, Silvio [Dip. di Scienze Fisiche, Universita di Napoli 'Federico II', via Cintia, I-80126 Naples (Italy) and INFN sez. Napoli, via Cintia, I-80126 Naples (Italy); Dip. di Scienze Farmaceutiche, Universita di Salerno, via Ponte Don Melillo, 84084 Fisciano (Saudi Arabia) (IT) and INFN sez. Napoli, via Cintia, I-80126 Naples (Italy); Dip. di Matematica ed Applicazioni, Universita di Napoli 'Federico II', via Cintia, I-80126 Naples (Italy) and INFN sez. Napoli, via Cintia, I-80126 Naples (Italy)

2006-06-15T23:59:59.000Z

256

Lack of energy equipartition in homogeneous heated binary granular mixtures  

E-Print Network [OSTI]

We consider the problem of determining the granular temperatures of the components of a homogeneous binary heated mixture of inelastic hard spheres, in the framework of Enskog kinetic theory. Equations are derived for the temperatures of each species and their ratio, which is different from unity, as may be expected since the system is out of equilibrium. We focus on the particular heating mechanism where the inelastic energy loss is compensated by an injection through a random external force (``stochastic thermostat''). The influence of various parameters and their possible experimental relevance is discussed.

A. Barrat; E. Trizac

2002-05-21T23:59:59.000Z

257

Compact Stars in low-mass X-ray binaries  

E-Print Network [OSTI]

We propose a model for compact stars in low-mass X-ray binaries(LMXBs) namely KS 1731-260, EXO 1745-248 and 4U 1608-52. Here we investigate the physical phenomena of a compact star in the LMXBs. Using our model, we have calculated central density, surface density, mass(M) and red-shift for the above mentioned compact stars, which is very much consistent with the reported data. We also obtain the possible equation of state(EOS) of the stars which is physically acceptable.

Sk. Monowar Hossein; Sajahan Molla; Md. Abdul Kayum Jafry; Mehedi Kalam

2014-08-13T23:59:59.000Z

258

Owner Valuation of Rabies Vaccination  

E-Print Network [OSTI]

similar protocols. Each campaign covered the same 3 city quarters, which had high- density dog populations an estimated 55,000 hu- man deaths each year; 23,750 (43%) of which occur in Africa (1). To eliminate rabies virus in dog populations, and thus reduce the risk for human rabies, the World Health Organization (WHO

Richner, Heinz

259

Ultrasonic studies in binary solutions of pyridine with water, methanol, and ethanol  

Science Journals Connector (OSTI)

The velocity and absorption of ultrasound at 19.5 MHz were studied as a function of the concentration in binary solutions of pyridine with water methanol and ethanol. In addition the compressibility and volume viscosity were calculated. Molecular processes are suggested to explain the variation of the ultrasonic properties of these binary solutions with respect to concentration.

K. N. Thomas; F. B. Stumpf

1973-01-01T23:59:59.000Z

260

Lattice Boltzmann model for binary mixtures Li-Shi Luo1,  

E-Print Network [OSTI]

Lattice Boltzmann model for binary mixtures Li-Shi Luo1, * and Sharath S. Girimaji2, 1 ICASE, Mail 2002 An a priori derivation of the lattice Boltzmann equations for binary mixtures is provided The lattice Boltzmann equation LBE 1­6 is emerging as an effective computational method based on fundamental

Luo, Li-Shi

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


261

Hypersonic acoustic excitations in binary colloidal crystals: Big versus small hard sphere control  

E-Print Network [OSTI]

Hypersonic acoustic excitations in binary colloidal crystals: Big versus small hard sphere control January 2007 The phononic band structure of two binary colloidal crystals, at hypersonic frequencies of light photonic crystals 2 and sound at hypersonic frequencies.3 The propa- gation of phonons

Schofield, Andrew B.

262

Binary and nonbinary description of hypointensity for search and retrieval of brain MR images  

E-Print Network [OSTI]

Binary and nonbinary description of hypointensity for search and retrieval of brain MR images. In a previous study based on binary description of hypointensity in the brain, it was shown that brain iron accumulation shape provides additional information to the shape-insensitive features, such as the total brain

Yanikoglu, Berrin

263

Binary Join Trees for Computing Marginals in the Shenoy-Shafer Architecture  

E-Print Network [OSTI]

The main goal of this paper is to describe a data structure called binary join trees that are useful in computing multiple marginals efficiently in the Shenoy-Shafer architecture. We define binary join trees, describe their utility, and describe a...

Shenoy, Prakash P.

1997-08-01T23:59:59.000Z

264

HOT WHITE DWARFS IN DETACHED BINARIES FROM THE ROSAT WFC ALL SKY SURVEY  

E-Print Network [OSTI]

HOT WHITE DWARFS IN DETACHED BINARIES FROM THE ROSAT WFC ALL SKY SURVEY Thesis submitted 1997 #12; HOT WHITE DWARFS IN DETACHED BINARIES FROM THE ROSAT WFC ALL SKY SURVEY Matthew R. Burleigh ABSTRACT White dwarfs in unresolved pairs with normal stars (spectral type K or earlier) are invisible

Burleigh, Matt

265

The effect of cluster formation on mass separation in binary molecular beams  

E-Print Network [OSTI]

The effect of cluster formation on mass separation in binary molecular beams Wei Li,a) M. J composition of a skimmed supersonic binary molecular beam originally consisting of a 20% neon/80% xenon. © 2000 American Institute of Physics. S0021-9606 00 01806-7 I. INTRODUCTION Supersonic molecular beam

Sibener, Steven

266

Division Unit for Binary Integer Decimals Tomas Lang and Alberto Nannarelli  

E-Print Network [OSTI]

) for significands. Recent decimal division designs are all based on the Binary Coded Decimal (BCD) encoding. We. The conversion from declet to Binary Coded Decimal (BCD) format, and vice versa, can be implemented with simple in standard cell technology. The implementation of the proposed BID division unit is compared to that of a BCD

Nannarelli, Alberto

267

Bubble and droplet motion in binary mixtures: Evaporation-condensation mechanism and Marangoni effect  

E-Print Network [OSTI]

Bubble and droplet motion in binary mixtures: Evaporation-condensation mechanism and Marangoni 2009; published 14 April 2009 Bubble and droplet motion in binary mixtures is studied in weak heat a crossover concentration c inversely proportional to the radius R of the bubble or droplet. Here c is usually

268

X-ray Pulsations in the Supersoft X-ray Binary CAL 83  

E-Print Network [OSTI]

X-ray data reveal that the supersoft X-ray binary CAL 83 exhibits 38.4 minute pulsations at some epochs. These X-ray variations are similar to those found in some novae and are likely to be caused by nonradial pulsations the white dwarf. This is the first detection of pulsations in a classical supersoft X-ray binary.

P. C. Schmidtke; A. P. Cowley

2005-09-28T23:59:59.000Z

269

Hypercritical Accretion, Induced Gravitational Collapse, and Binary-Driven Hypernovae  

E-Print Network [OSTI]

The induced gravitational collapse (IGC) paradigm has been successfully applied to the explanation of the concomitance of gamma-ray bursts (GRBs) with supernovae (SNe) Ic. The progenitor is a tight binary system composed by a carbon-oxygen (CO) core and a neutron star (NS) companion. The explosion of the SN leads to hypercritical accretion onto the NS companion which reaches the critical mass, hence inducing its gravitational collapse to a black hole (BH) with consequent emission of the GRB. The first estimates of this process were based on a simplified model of the binary parameters and the Bondi-Hoyle-Lyttleton accretion rate. We present here the first full numerical simulations of the IGC phenomenon. We simulate the core-collapse and SN explosion of CO stars to obtain the density and ejection velocity of the SN ejecta. We follow the hydrodynamic evolution of the accreting material falling into the Bondi-Hoyle surface of the NS all the way up to its incorporation to the NS surface. The simulations go up to ...

Fryer, Chris L; Ruffini, Remo

2014-01-01T23:59:59.000Z

270

FORMATION OF STABLE MAGNETARS FROM BINARY NEUTRON STAR MERGERS  

SciTech Connect (OSTI)

By performing fully general relativistic magnetohydrodynamic simulations of binary neutron star mergers, we investigate the possibility that the end result of the merger is a stable magnetar. In particular, we show that, for a binary composed of two equal-mass neutron stars (NSs) of gravitational mass M {approx} 1.2 M{sub Sun} and equation of state similar to Shen et al. at high densities, the merger product is a stable NS. Such NS is found to be differentially rotating and ultraspinning with spin parameter J/M{sup 2} {approx} 0.86, where J is its total angular momentum, and it is surrounded by a disk of Almost-Equal-To 0.1 M{sub Sun }. While in our global simulations the magnetic field is amplified by about two orders of magnitude, local simulations have shown that hydrodynamic instabilities and the onset of the magnetorotational instability could further increase the magnetic field strength up to magnetar levels. This leads to the interesting possibility that, for some NS mergers, a stable and magnetized NS surrounded by an accretion disk could be formed. We discuss the impact of these new results for the emission of electromagnetic counterparts of gravitational wave signals and for the central engine of short gamma-ray bursts.

Giacomazzo, Bruno [JILA, University of Colorado and National Institute of Standards and Technology, Boulder, CO 80309 (United States); Perna, Rosalba [JILA and Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 80309 (United States)

2013-07-10T23:59:59.000Z

271

Characterizing spinning black hole binaries in eccentric orbits with LISA  

SciTech Connect (OSTI)

The Laser Interferometer Space Antenna (LISA) is designed to detect gravitational wave signals from astrophysical sources, including those from coalescing binary systems of compact objects such as black holes. Colliding galaxies have central black holes that sink to the center of the merged galaxy and begin to orbit one another and emit gravitational waves. Some galaxy evolution models predict that the binary black hole system will enter the LISA band with significant orbital eccentricity, while other models suggest that the orbits will already have circularized. Using a full 17 parameter waveform model that includes the effects of orbital eccentricity, spin precession, and higher harmonics, we investigate how well the source parameters can be inferred from simulated LISA data. Defining the reference eccentricity as the value one year before merger, we find that for typical LISA sources, it will be possible to measure the eccentricity to an accuracy of parts in a thousand. The accuracy with which the eccentricity can be measured depends only very weakly on the eccentricity, making it possible to distinguish circular orbits from those with very small eccentricities. LISA measurements of the orbital eccentricity can help constraints theories of galaxy mergers in the early universe. Failing to account for the eccentricity in the waveform modeling can lead to a loss of signal power and bias the estimation of parameters such as the black hole masses and spins.

Key, Joey Shapiro; Cornish, Neil J. [Department of Physics, Montana State University, Bozeman, Montana 59717 (United States)

2011-04-15T23:59:59.000Z

272

Improved Moving Puncture Gauge Conditions for Compact Binary Evolutions  

E-Print Network [OSTI]

Robust gauge conditions are critically important to the stability and accuracy of numerical relativity (NR) simulations involving compact objects. Most of the NR community use the highly robust---though decade-old---moving-puncture (MP) gauge conditions for such simulations. It has been argued that in binary black hole (BBH) evolutions adopting this gauge, noise generated near adaptive-mesh-refinement (AMR) boundaries does not converge away cleanly with increasing resolution, severely limiting gravitational waveform accuracy at computationally feasible resolutions. We link this noise to a sharp (short-wavelength), initial outgoing gauge wave crossing into progressively lower resolution AMR grids, and present improvements to the standard MP gauge conditions that focus on stretching, smoothing, and more rapidly settling this outgoing wave. Our best gauge choice greatly reduces gravitational waveform noise during inspiral, yielding less fluctuation in convergence order and $\\sim 40%$ lower waveform phase and amplitude errors at typical resolutions. Noise in other physical quantities of interest is also reduced, and constraint violations drop by more than an order of magnitude. We expect these improvements will carry over to simulations of all types of compact binary systems, as well as other $N$+1 formulations of gravity for which MP-like gauge conditions can be chosen.

Zachariah B. Etienne; John G. Baker; Vasileios Paschalidis; Bernard J. Kelly; Stuart L. Shapiro

2014-10-06T23:59:59.000Z

273

The Age and Stellar Parameters of the Procyon Binary System  

E-Print Network [OSTI]

The Procyon AB binary system (orbital period 40.838 years, a newly-refined determination), is near and bright enough that the component radii, effective temperatures, and luminosities are very well determined, although more than one possible solution to the masses has limited the claimed accuracy. Preliminary mass determinations for each component are available from HST imaging, supported by ground-based astrometry and an excellent Hipparcos parallax; we use these for our preferred solution for the binary system. Other values for the masses are also considered. We have employed the TYCHO stellar evolution code to match the radius and luminosity of the F5 IV-V primary star to determine the system's most likely age as 1.87 +/- 0.13 Gyr. Since prior studies of Procyon A found its abundance indistinguishable from solar, the solar composition of Asplund, Grevesse & Sauval (Z=0.014) is assumed for the HR Diagram flitting. An unsuccessful attempt to fit using the older solar abundance scale of Grevesse & Sau...

Liebert, James; Young, Patrick A; Williams, Kurtis A; Arnett, David

2013-01-01T23:59:59.000Z

274

Long term evolution of an interacting binary system  

E-Print Network [OSTI]

We describe a new code to simulate the stellar evolution of a close interacting binary system. It is then used to calculate the evolution of a classical nova system composed of a 1.25 Msun Main-Sequence (MS) star and a 1.0 Msun white dwarf (WD) companion. The system begins as a well separated non-interacting binary system. Initially, the two stars evolve independently of each other. However, Roche lobe overflow begins as the MS star expands on its way to become a Red Giant. We follow the mass accreted onto the WD and the ensuing nuclear runaways for several thousand flashes. The main finding is that the Roche-Lobe mass transfer rate is modulated by oscillations in the MS star, with a period that is somewhat shorter than the thermal time scale of the star. This periodically modulates the rate of thermonuclear flashes on the WD, between once every 12000 yrs, such that the WD can cool, to once every 300 yrs, such that it cannot. The system is further complicated by the secular drift in the secondary modulation. ...

Shaviv, Giora; Shaviv, Nir J

2014-01-01T23:59:59.000Z

275

Theoretical X-ray Line Profiles from Colliding Wind Binaries  

E-Print Network [OSTI]

We present theoretical X-ray line profiles from a range of model colliding wind systems. In particular, we investigate the effects of varying the stellar mass-loss rates, the wind speeds, and the viewing orientation. We find that a wide range of theoretical line profile shapes is possible, varying with orbital inclination and phase. At or near conjunction, the lines have approximately Gaussian profiles, with small widths (HWHM ~ 0.1 v_\\infty) and definite blue- or redshifts (depending on whether the star with the weaker wind is in front or behind). When the system is viewed at quadrature, the lines are generally much broader (HWHM ~ v_\\infty), flat-topped and unshifted. Local absorption can have a major effect on the observed profiles - in systems with mass-loss rates of a few times 10^{-6} Msol/yr the lower energy lines (E wind of the primary. The orbital variation of the line widths and shifts is reduced in a low inclination binary. The extreme case is a binary with i = 0 degrees, for which we would expect no line profile variation.

D. B. Henley; I. R. Stevens; J. M. Pittard

2003-06-23T23:59:59.000Z

276

Ultrashort-period MS eclipsing systems. New observations and light curve solutions of six NSVS binaries  

E-Print Network [OSTI]

We carried out photometric and low-resolution spectral observations of six eclipsing ultrashort-period binaries with MS components. The light curve solutions of the Rozhen observations show that all targets are overcontact systems. We found well-defined empirical relation "period -- semi-major axis" for the short-period binaries and used it for estimation of the global parameters of the targets. Our results revealed that NSVS 925605 is quite interesting target: (a) it is one of a few contact binaries with M components; (b) it exhibits high activity (emission in H$\\alpha$ line, X-ray emission, large cool spots, non-Planck energy distribution); (c) its components differ in temperature by 700 K. All appearances of high magnetic activity and huge fillout factor (0.7) of NSVS 925605 might be assumed as a precursor of the predicted merging of close magnetic binaries. Another unusual binary is NSVS 2700153 which reveals considerable long-term variability.

Dimitrov, Dinko

2015-01-01T23:59:59.000Z

277

Robust parameter estimation for compact binaries with ground-based gravitational-wave observations using LALInference  

E-Print Network [OSTI]

The Advanced LIGO and Advanced Virgo gravitational wave (GW) detectors will begin operation in the coming years, with compact binary coalescence events a likely source for the first detections. The gravitational waveforms emitted directly encode information about the sources, including the masses and spins of the compact objects. Recovering the physical parameters of the sources from the GW observations is a key analysis task. This work describes the LALInference software library for Bayesian parameter estimation of compact binary coalescence (CBC) signals, which builds on several previous methods to provide a well-tested toolkit which has already been used for several studies. We are able to show using three independent sampling algorithms that our implementation consistently converges on the same results, giving confidence in the parameter estimates thus obtained. We demonstrate this with a detailed comparison on three compact binary systems: a binary neutron star, a neutron star-black hole binary and a bin...

Veitch, John; Farr, Benjamin; Farr, Will M; Graff, Philip; Vitale, Salvatore; Aylott, Ben; Blackburn, Kent; Christensen, Nelson; Coughlin, Michael; Del Pozzo, Walter; Feroz, Farhan; Gair, Jonathan; Haster, Carl-Johan; Kalogera, Vicky; Littenberg, Tyson; Mandel, Ilya; O'Shaughnessy, Richard; Pitkin, Matthew; Rodriguez, Carl; Rver, Christian; Sidery, Trevor; Smith, Rory; Van Der Sluys, Marc; Vecchio, Alberto; Vousden, Will; Wade, Leslie

2014-01-01T23:59:59.000Z

278

Short Gamma Ray Bursts as possible electromagnetic counterpart of coalescing binary systems  

E-Print Network [OSTI]

Coalescing binary systems, consisting of two collapsed objects, are among the most promising sources of high frequency gravitational waves signals detectable, in principle, by ground-based interferometers. Binary systems of Neutron Star or Black Hole/Neutron Star mergers should also give rise to short Gamma Ray Bursts, a subclass of Gamma Ray Bursts. Short-hard-Gamma Ray Bursts might thus provide a powerful way to infer the merger rate of two-collapsed object binaries. Under the hypothesis that most short Gamma Ray Bursts originate from binaries of Neutron Star or Black Hole/Neutron Star mergers, we outline here the possibility to associate short Gamma Ray Bursts as electromagnetic counterpart of coalescing binary systems.

S. Capozziello; M. De Laurentis; I. De Martino; M. Formisano

2010-04-27T23:59:59.000Z

279

Linking the fate of massive black hole binaries to the active galactic nuclei luminosity function  

E-Print Network [OSTI]

Massive black hole binaries are naturally predicted in the context of the hierarchical model of structure formation. The binaries that manage to lose most of their angular momentum can coalesce to form a single remnant. In the last stages of this process, the holes undergo an extremely loud phase of gravitational wave emission, possibly detectable by current and future probes. The theoretical effort towards obtaining a coherent physical picture of the binary path down to coalescence is still underway. In this paper, for the first time, we take advantage of observational studies of active galactic nuclei evolution to constrain the efficiency of gas-driven binary decay. Under conservative assumptions we find that gas accretion toward the nuclear black holes can efficiently lead binaries of any mass forming at high redshift (> 2) to coalescence within the current time. The observed "downsizing" trend of the accreting black hole luminosity function further implies that the gas inflow is sufficient to drive light ...

Dotti, Massimo; Montuori, Carmen

2015-01-01T23:59:59.000Z

280

Vacancies in ordered and disordered binary alloys treated with the cluster expansion A. Van der Ven and G. Ceder  

E-Print Network [OSTI]

Vacancies in ordered and disordered binary alloys treated with the cluster expansion A. Van der Ven far neglected the presence of vacancies. Here, we invoke a local cluster expansion as a perturbation to the standard binary cluster expansion to model the equilibrium vacancy concentration in a binary alloy

Ceder, Gerbrand

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


281

Hawaii/Geothermal | Open Energy Information  

Open Energy Info (EERE)

Hawaii/Geothermal Hawaii/Geothermal < Hawaii Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Print PDF Hawaii Geothermal General Regulatory Roadmap Geothermal Power Projects Under Development in Hawaii Developer Location Estimated Capacity (MW) Development Phase Geothermal Area Geothermal Region Haleakala SW Rift Zone Exploration Ormat Technologies Inc , US Department of Energy Haleakala Southwest Rift Zone Haleakala Volcano Geothermal Area Hawaii Geothermal Region Puna Geothermal Venture Ormat Technologies Inc Pahoa, Hawaii 38 MW38,000 kW 38,000,000 W 38,000,000,000 mW 0.038 GW 3.8e-5 TW Kilauea East Rift Geothermal Area Hawaii Geothermal Region Add a geothermal project. Operational Geothermal Power Plants in Hawaii Owner Facility Type Capacity (MW) Commercial Online

282

Low velocity ion stopping in binary ionic mixtures  

SciTech Connect (OSTI)

Attention is focused on the low ion velocity stopping mechanisms in multicomponent and dense target plasmas built of quasiclassical electron fluids neutralizing binary ionic mixtures, such as, deuterium-tritium of current fusion interest, proton-heliumlike iron in the solar interior or proton-helium ions considered in planetology, as well as other mixtures of fiducial concern in the heavy ion beam production of warm dense matter at Bragg peak conditions. The target plasma is taken in a multicomponent dielectric formulation a la Fried-Conte. The occurrence of projectile ion velocities (so-called critical) for which target electron slowing down equals that of given target ion components is also considered. The corresponding multiquadrature computations, albeit rather heavy, can be monitored analytical through a very compact code operating a PC cluster. Slowing down results are systematically scanned with respect to target temperature and electron density, as well as ion composition.

Tashev, Bekbolat; Baimbetov, Fazylkhan [Department of Physics, Kazakh National University, Tole Bi 96, Almaty 480012 (Kazakhstan); Deutsch, Claude [LPGP (UMR-CNRS 8578), Universite Paris XI, 91405 Orsay (France); Fromy, Patrice [Direction de l'Informatique, Universite Paris XI, 91405 Orsay (France)

2008-10-15T23:59:59.000Z

283

Beowawe Bottoming Binary Unit - Final Technical Report for EE0002856  

SciTech Connect (OSTI)

This binary plant is the first high-output refrigeration based waste heat recovery cycle in the industry. Its working fluid is environmentally friendly and as such, the permits that would be required with a butane based cycle are not necessary. The unit is modularized, meaning that the units individual skids were assembled in another location and were shipped via truck to the plant site. This project proves the technical feasibility of using low temperature brine The development of the unit led to the realization of low temperature, high output, and environmentally friendly heat recovery systems through domestic research and engineering. The project generates additional renewable energy for Nevada, resulting in cleaner air and reduced carbon dioxide emissions. Royalty and tax payments to governmental agencies will increase, resulting in reduced financial pressure on local entities. The major components of the unit were sourced from American companies, resulting in increased economic activity throughout the country.

McDonald, Dale Edward

2013-02-12T23:59:59.000Z

284

A brown dwarf mass donor in an accreting binary  

E-Print Network [OSTI]

A long standing and unverified prediction of binary star evolution theory is the existence of a population of white dwarfs accreting from sub-stellar donor stars. Such systems ought to be common, but the difficulty of finding them, combined with the challenge of detecting the donor against the light from accretion means that no donor star to date has a measured mass below the hydrogen burning limit. Here we apply a technique which allows us to reliably measure the mass of the unseen donor star in eclipsing systems. We are able to identify a brown dwarf donor star, with a mass of 0.052+/-0.002 Msun. The relatively high mass of the donor star for its orbital period suggests that current evolutionary models may underestimate the radii of brown dwarfs.

S. P. Littlefair; V. S. Dhillon; T. R. Marsh; Boris T. Gaensicke; John Southworth; C. A. Watson

2006-12-08T23:59:59.000Z

285

Heating mechanism affects equipartition in a binary granular system  

E-Print Network [OSTI]

Two species of particles in a binary granular system typically do not have the same mean kinetic energy, in contrast to the equipartition of energy required in equilibrium. We investigate the role of the heating mechanism in determining the extent of this non-equipartition of kinetic energy. In most experiments, different species of particle are unequally heated at the boundaries. We show by event-driven simulations that this differential heating at the boundary influences the level of non-equipartition even in the bulk of the system. This conclusion is fortified by studying a numerical model and a solvable stochastic model without spatial degrees of freedom. In both cases, even in the limit where heating events are rare compared to collisions, the effect of the heating mechanism persists.

Hong-Qiang Wang; Narayanan Menon

2007-10-19T23:59:59.000Z

286

Very hot nuclear systems and their binary and multifragment decay  

SciTech Connect (OSTI)

Compound emission of complex fragments in the reaction {sup 63}Cu + {sup 12}C is used to determine the associated ridge-line potential. Compound binary emission of complex fragments at higher energies is illustrated for a variety of reactions. Complex fragment emission from 18, 26, 31, 35, 45 and 55 MeV/N {sup 139}La/{sup 129}Xe + {sup 12}C, {sup 27}Al, {sup 40}Ca, {sup 51}V, {sup nat}Cu and {sup 139}La reactions has been studied. Multifragment events from these reactions were assigned to sources characterized by their energy and mass through the incomplete-fusion-model kinematics. Excitation functions for the various multifragment channels appear to be nearly independent of the system and bombarding energy. Preliminary comparisons of the data with sequential-statistical-decay calculations are discussed. 16 refs., 9 figs.

Moretto, L.G.; Blumenfeld, Y.; Delis, D.; Wozniak, G.J.

1990-10-01T23:59:59.000Z

287

Free energy of surface segregation in binary alloys  

Science Journals Connector (OSTI)

The pair-bond approximation and the mean-field approach are used to derive an expression for the free energy of surface segregation in binary alloys. It is suggested that a correction term, in addition to the surface energy term and the heat of solution, should be included in the free energy of segregation in order to obtain a better quantitative agreement between theory and experiment. This correction term is a concentration-dependent quantity and therefore cannot be obtained from pure-metal properties. The theory is applied to Cu-Ni alloy, and if the correction term is properly chosen, then a good quantitative agreement with experiment is found for all in-depth surface compositions. The free energy of segregation obtained by this method is in qualitative agreement with that calculated on surface core-level shifts. This is not the case if the correction term is not considered.

Yi-Chen Cheng; C. J. Wu; R. C. Chiang

1985-09-15T23:59:59.000Z

288

Instabilities in granular binary mixtures at moderate densities  

Science Journals Connector (OSTI)

A linear stability analysis of the Navier-Stokes (NS) granular hydrodynamic equations is performed to determine the critical length scale for the onset of vortices and clusters instabilities in granular dense binary mixtures. In contrast to previous attempts, our results (which are based on the solution to the inelastic Enskog equation to NS order) are not restricted to nearly elastic systems since they take into account the complete nonlinear dependence of the NS transport coefficients on the coefficients of restitution ?ij. The theoretical predictions for the critical length scales are compared to molecular dynamics (MD) simulations in flows of strong dissipation (?ij?0.7) and moderate solid volume fractions (??0.2). We find excellent agreement between MD and kinetic theory for the onset of velocity vortices, indicating the applicability of NS hydrodynamics to polydisperse flows even for strong inelasticity, finite density, and particle dissimilarity.

Peter P. Mitrano; Vicente Garz; Christine M. Hrenya

2014-02-10T23:59:59.000Z

289

Absolute Properties of the Eclipsing Binary Star AP Andromedae  

E-Print Network [OSTI]

AP And is a well-detached F5 eclipsing binary star for which only a very limited amount of information was available before this publication. We have obtained very extensive measurements of the light curve (19097 differential V magnitude observations) and a radial velocity curve (83 spectroscopic observations) which allow us to fit orbits and determine the absolute properties of the components very accurately: masses of 1.277 +/- 0.004 and 1.251 +/- 0.004 solar masses, radii of 1.233 +/- 0.006 and 1.1953 +/- 0.005 solar radii, and temperatures of 6565 +/- 150 K and 6495 +/- 150 K. The distance to the system is about 400 +/- 30 pc. Comparison with the theoretical properties of the stellar evolutionary models of the Yonsei-Yale series of Yi et al. shows good agreement between the observations and the theory at an age of about 500 Myr and a slightly sub-solar metallicity.

Lacy, Claud H Sandberg; Fekel, Francis C; Muterspaugh, Matthew W

2014-01-01T23:59:59.000Z

290

AA Dor - An Eclipsing sdOB - Brown Dwarf Binary  

E-Print Network [OSTI]

AA Dor is an eclipsing, close, post common-envelope binary consisting of a sdOB primary star and an unseen secondary with an extraordinary small mass - formally a brown dwarf. The brown dwarf may have been a former planet which survived a common envelope phase and has even gained mass. A recent determination of the components' masses from results of NLTE spectral analysis and subsequent comparison to evolutionary tracks shows a discrepancy to masses derived from radial-velocity and the eclipse curves. Phase-resolved high-resolution and high-SN spectroscopy was carried out in order to investigate on this problem. We present results of a NLTE spectral analysis of the primary, an analysis of its orbital parameters, and discuss possible evolutionary scenarios.

Thomas Rauch

2003-11-25T23:59:59.000Z

291

SPECTRAL PROPERTIES OF X-RAY BINARIES IN CENTAURUS A  

SciTech Connect (OSTI)

We present a spectral investigation of X-ray binaries (XBs) in NGC 5128 (Cen A), using six 100 ks Chandra observations taken over two months in 2007. We divide our sample into thermally and non-thermally dominated states based on the behavior of the fitted absorption column N{sub H}, and present the spectral parameters of sources with L{sub x} {approx}> 2 Multiplication-Sign 10{sup 37} erg s{sup -1}. The majority of sources are consistent with being neutron star low-mass X-ray binaries (NS LMXBs) and we identify three transient black hole (BH) LMXB candidates coincident with the dust lane, which is the remnant of a small late-type galaxy. Our results also provide tentative support for the apparent 'gap' in the mass distribution of compact objects between {approx}2-5 M{sub Sun }. We propose that BH LMXBs are preferentially found in the dust lane, and suggest this is because of the younger stellar population. The majority ({approx}70%-80%) of potential Roche lobe filling donors in the Cen A halo are {approx}> 12 Gyr old, while BH LMXBs require donors {approx}> 1 M{sub Sun} to produce the observed peak luminosities. This requirement for more massive donors may also explain recent results that claim a steepening of the X-ray luminosity function with age at L{sub x} {>=} 5 Multiplication-Sign 10{sup 38} erg s{sup -1} for the XB population of early-type galaxies; for older stellar populations, there are fewer stars {approx}> 1 M{sub Sun }, which are required to form the more luminous sources.

Burke, Mark J.; Raychaudhury, Somak [School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT (United Kingdom)] [School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT (United Kingdom); Kraft, Ralph P.; Forman, William R.; Jones, Christine; Murray, Stephen S.; Birkinshaw, Mark; Evans, Daniel A.; Jordan, Andres [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)] [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Maccarone, Thomas J.; Croston, Judith H. [School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ (United Kingdom)] [School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ (United Kingdom); Brassington, Nicola J.; Hardcastle, Martin J.; Goodger, Joanna L. [School of Physics, Astronomy, and Mathematics, University of Hertfordshire, Hatfield AL10 9AB (United Kingdom)] [School of Physics, Astronomy, and Mathematics, University of Hertfordshire, Hatfield AL10 9AB (United Kingdom); Kainulainen, Jouni [Max-Planck-Institute for Astronomy, Koenigstuhl 17, D-69117 Heidelberg (Germany)] [Max-Planck-Institute for Astronomy, Koenigstuhl 17, D-69117 Heidelberg (Germany); Woodley, Kristin A. [Department of Physics and Astronomy, University of British Columbia, Vancouver BC V6T 1Z1 (Canada)] [Department of Physics and Astronomy, University of British Columbia, Vancouver BC V6T 1Z1 (Canada); Sivakoff, Gregory R. [Department of Physics, University of Alberta, Edmonton, Alberta T6G 2E1 (Canada)] [Department of Physics, University of Alberta, Edmonton, Alberta T6G 2E1 (Canada); Gilfanov, Marat [Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85741, Garching (Germany)] [Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85741, Garching (Germany); Sarazin, Craig L. [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States)] [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Voss, Rasmus, E-mail: mburke@star.sr.bham.ac.uk [Department of Astrophysics/IMAPP, Radboud, University Nijmegen, P.O. Box 9010, NL-6500 GL Nijmegen (Netherlands)] [Department of Astrophysics/IMAPP, Radboud, University Nijmegen, P.O. Box 9010, NL-6500 GL Nijmegen (Netherlands); and others

2013-04-01T23:59:59.000Z

292

THE INTERACTING EARLY-TYPE BINARY V382 Cyg  

SciTech Connect (OSTI)

We analyze photometric and spectroscopic data and study the orbital period of the early-type interacting binary system V382 Cyg by using all the available data. We obtain a simultaneous light and radial velocity curve solution. The derived physical parameters of the primary and secondary stellar components are M{sub 1} = 27.9(5) M{sub Sun }, M{sub 2} = 20.8(4) M{sub Sun }, R{sub 1} = 9.7(2) R{sub Sun }, R{sub 2} = 8.5(2) R{sub Sun }, log ({sub 1}/L{sub Sun }) = 5.152(20), and log (L{sub 2}/L{sub Sun }) = 4.954(19) while the separation of the components is a = 23.4 R{sub Sun }. Newly obtained parameters yield the distance of the system to be 1466(76) pc. Analyses of the mid-eclipse times indicate a period increase of dP/dt = 4.2(1) Multiplication-Sign 10{sup -7} days yr{sup -1} that can be interpreted in terms of the high-mass transfer (dM/dt 6.1(5) Multiplication-Sign 10{sup -6} M{sub Sun} yr{sup -1}) from the less massive component to the more massive component. Finally, we model the evolution of the components using non-conservative codes and discuss the results obtained. The age of the binary system is estimated to be 3.85 Myr.

Yasarsoy, B.; Yakut, K. [Department of Astronomy and Space Sciences, University of Ege, 35100 Bornova-Izmir (Turkey)

2013-01-01T23:59:59.000Z

293

Very Wide Binary Stars as the Primary Source of Stellar Collisions in the Galaxy  

Science Journals Connector (OSTI)

We present numerical simulations modeling the orbital evolution of very wide binaries, pairs of stars separated by over ~103AU. Due to perturbations from other passing stars and the Milky Way's tide, the orbits of very wide binary stars occasionally become extremely eccentric, which forces close encounters between the companion stars. We show that this process causes a stellar collision between very wide binary companion stars once every 1000-7500yr on average in the Milky Way. One of the main uncertainties in this collision rate is the amount of energy dissipated by dynamic tides during close (but not collisional) periastron passages. This dissipation presents a dynamical barrier to stellar collisions and can instead transform very wide binaries into close or contact binaries. However, for any plausible tidal dissipation model, very wide binary stars are an unrealized, and potentially the dominant, source of stellar collisions in our Galaxy. Such collisions should occur throughout the thin disk of the Milky Way. Stellar collisions within very wide binaries should yield a small population of single, Li-depleted, rapidly rotating massive stars.

Nathan A. Kaib; Sean N. Raymond

2014-01-01T23:59:59.000Z

294

Close Binary White Dwarfs, Neutron Stars, Black Holes: Formation, Evolution, and Related Phenomena  

E-Print Network [OSTI]

We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact binary stars are expected to be the most important sources for the forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binary stars with NS and/or black components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically important thermonuclear SN~Ia. We also consider AM~CVn-stars which are thought to be the bes...

Postnov, Konstantin

2014-01-01T23:59:59.000Z

295

The Evolution of the Multiplicity of Embedded Protostars II: Binary Separation Distribution & Analysis  

E-Print Network [OSTI]

We present the Class I protostellar binary separation distribution based on the data tabulated in the companion paper. We verify the excess of Class I binary stars over solar-type main-sequence stars, especially at separations beyond 500 AU. Although our sources are in nearby star forming regions distributed across the entire sky (including Orion), none of our objects are in a high stellar density environment. The binary separation distribution changes significantly during the Class I phase, and the binary frequency at separations greater than 1000 AU declines steadily with respect to spectral index. Despite these changes, the binary frequency remains constant until the end of the Class I phase, when it drops sharply. We propose a scenario to account for the changes in the Class I binary separation distribution. This scenario postulates that companions with a separation greater than ~1000 AU were ejected during the Class 0 phase, but remain gravitationally bound due to the mass of the envelope. As the envelope dissipates, these companions become unbound and the binary frequency at wide separations declines. This scenario predicts that a large number of Class 0 objects should be non-hierarchical multiple systems, and that many Class I YSOs with a widely separated companion should also have a very close companion. We also find that Class I protostars are not dynamically pristine, and have experienced dynamical evolution before they are visible as Class I objects. For the first time, evidence is presented showing that the Class I binary frequency and the binary separation distribution strongly depend on the star forming environment. The reason for this dependence remains unclear.

Michael Connelley; Bo Reipurth; Alan Tokunaga

2008-03-07T23:59:59.000Z

296

Formalism for the construction of binary neutron stars with arbitrary circulation  

SciTech Connect (OSTI)

Most numerical models of binary stars - in particular neutron stars in compact binaries - assume the companions to be either corotational or irrotational. Either one of these assumptions leads to a significant simplification in the hydrodynamic equations of stationary equilibrium. In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational. Generalizing the equations for irrotational flow we cast the Euler equation, which is an algebraic equation in the case of corotational or irrotational fluid flow, as an elliptic equation for a new auxiliary quantity. We also suggest a parametrized decomposition of the fluid flow that allows for a variation of the stellar circulation.

Baumgarte, Thomas W. [Department of Physics and Astronomy, Bowdoin College, Brunswick, Maine 04011 (United States); Shapiro, Stuart L. [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States)

2009-09-15T23:59:59.000Z

297

BINARIES DISCOVERED BY THE MUCHFUSS PROJECT: SDSS J08205+0008-AN ECLIPSING SUBDWARF B BINARY WITH A BROWN DWARF COMPANION  

SciTech Connect (OSTI)

Hot subdwarf B stars (sdBs) are extreme horizontal branch stars believed to originate from close binary evolution. Indeed about half of the known sdB stars are found in close binaries with periods ranging from a few hours to a few days. The enormous mass loss required to remove the hydrogen envelope of the red-giant progenitor almost entirely can be explained by common envelope ejection. A rare subclass of these binaries are the eclipsing HW Vir binaries where the sdB is orbited by a dwarf M star. Here, we report the discovery of an HW Vir system in the course of the MUCHFUSS project. A most likely substellar object ({approx_equal}0.068 M{sub sun}) was found to orbit the hot subdwarf J08205+0008 with a period of 0.096 days. Since the eclipses are total, the system parameters are very well constrained. J08205+0008 has the lowest unambiguously measured companion mass yet found in a subdwarf B binary. This implies that the most likely substellar companion has not only survived the engulfment by the red-giant envelope, but also triggered its ejection and enabled the sdB star to form. The system provides evidence that brown dwarfs may indeed be able to significantly affect late stellar evolution.

Geier, S.; Schaffenroth, V.; Drechsel, H.; Heber, U.; Kupfer, T.; Tillich, A. [Dr. Remeis-Observatory and ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuernberg, Sternwartstr. 7, 96049 Bamberg (Germany); Oestensen, R. H.; Smolders, K.; Degroote, P. [Institute of Astronomy, K.U. Leuven, Celestijnenlaan 200D, B-3001 Heverlee (Belgium); Maxted, P. F. L. [Astrophysics Group, Keele University, Staffordshire, ST5 5BG (United Kingdom); Barlow, B. N. [Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255 (United States); Gaensicke, B. T.; Marsh, T. R. [Department of Physics, University of Warwick, Conventry CV4 7AL (United Kingdom); Napiwotzki, R., E-mail: geier@sternwarte.uni-erlangen.de [Centre of Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB (United Kingdom)

2011-04-20T23:59:59.000Z

298

Supercomputers Crack Sixty-Trillionth Binary Digit of Pi-Squared |  

Broader source: Energy.gov (indexed) [DOE]

Supercomputers Crack Sixty-Trillionth Binary Digit of Pi-Squared Supercomputers Crack Sixty-Trillionth Binary Digit of Pi-Squared Supercomputers Crack Sixty-Trillionth Binary Digit of Pi-Squared April 28, 2011 - 11:28am Addthis David H. Bailey | Photo Courtesy of Lawrence Berkely National Lab David H. Bailey | Photo Courtesy of Lawrence Berkely National Lab Linda Vu What are the key facts? Australian researchers have found the sixty-trillionth binary digit of Pi-squared. The calculation would have taken a single computer processor unit (CPU) 1,500 years to calculate, but it took just a few months on IBM's "BlueGene/P" supercomputer, which is designed to run continuously at one quadrillion calculations per second. Pi is one of the most mysterious numbers in mathematics and can never be expressed as a finite decimal number -- humanity will never have

299

Probability distribution function for inclinations of merging compact binaries detected by gravitational wave interferometers  

E-Print Network [OSTI]

We analytically discuss probability distribution function (PDF) for inclinations of merging compact binaries whose gravitational waves are coherently detected by a network of ground based interferometers. The PDF would be useful for studying prospects of (1) simultaneously detecting electromagnetic signals (such as gamma-ray-bursts) associated with binary mergers and (2) statistically constraining the related theoretical models from the actual observational data of multi-messenger astronomy. Our approach is similar to Schutz (2011), but we explicitly include the dependence of the polarization angles of the binaries, based on the concise formulation given in Cutler and Flanagan (1994). We find that the overall profiles of the PDFs are similar for any networks composed by the second generation detectors (Advanced-LIGO, Advanced-Virgo, KAGRA, LIGO-India). For example, 5.1% of detected binaries would have inclination angle less than 10 degree with at most 0.1% differences between the potential networks. A perturb...

Seto, Naoki

2014-01-01T23:59:59.000Z

300

Non-Oberbeck-Boussinesq effects and barodiffusion in binary mixtures with small thermodiffusion ratio  

Science Journals Connector (OSTI)

For a binary-fluid layer heated from below, we evaluate the effects of the temperature and concentration dependence of the thermodiffusion ratio kT as well as the influence of barodiffusion on the conductive state and its stability.

S. J. Linz and M. Lcke

1987-10-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


301

E-Print Network 3.0 - adc x-ray binary Sample Search Results  

Broader source: All U.S. Department of Energy (DOE) Office Webpages (Extended Search)

-Planck code and its applications . . . 63 3.6.7 Observation of X-ray binaries with Simbol... for the hard X-ray emission of accreting black holes sources (both in Seyfert...

302

First all-sky search for continuous gravitational waves from unknown sources in binary systems  

E-Print Network [OSTI]

We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect ...

Aggarwal, Nancy

303

Parameter estimation for compact binary coalescence signals with the first generation gravitational-wave detector network  

E-Print Network [OSTI]

Compact binary systems with neutron stars or black holes are one of the most promising sources for ground-based gravitational-wave detectors. Gravitational radiation encodes rich information about source physics; thus ...

Barsotti, Lisa

304

X-ray spectroscopy of neutron star low-mass X-ray binaries  

E-Print Network [OSTI]

In this thesis, I present work spanning a variety of topics relating to neutron star lowmass X-ray binaries (LMXBs) and utilize spectral information from X-ray observations to further our understanding of these sources. ...

Krauss, Miriam Ilana

2007-01-01T23:59:59.000Z

305

On the rarity of x-ray binaries with Wolf-Rayet donors  

DOE Public Access Gateway for Energy & Science Beta (PAGES Beta)

The paucity of High mass X-Ray binaries (HMXB) consisting of a neutron star (NS) accretor and Wolf-Rayet (WR) donor has long been at odds with expectations from population synthesis studies indicating that these systems should survive as the evolved offspring of the observed HMXB population. This tension is particularly troubling in light of recent observations uncovering a preponderance of HMXBs containing loosely bound Be donors which would be expected to naturally evolve into WR-HMXBs. Reconciling the unexpectedly large population of Be-HMXBs with the lack of observed WR-HMXB sources thus serves to isolate the dynamics of CE physics from other binary evolution parameters. Here, we find that binary mergers during CE events must be common in order to resolve tension between these observed populations. Furthermore, future observations which better constrain the background population of loosely bound O/B-NS binaries are likely to place significant constraints on the efficiency of CE removal.

Linden, T; Valsecchi, F; Kalogera, V

2012-03-06T23:59:59.000Z

306

Hydrodynamic Model with Binary Particle Diameters to Predict Axial Voidage Profile in a CFB Combustor  

Science Journals Connector (OSTI)

A hydrodynamic model with binary particle diameters was developed to better predict axial voidage profile in a CFB combustor. In the model, the CFB is regarded as a superposition of two ... field data of voidage ...

J. J. Li; H. Zhang; H. R. Yang; Y. X. Wu

2010-01-01T23:59:59.000Z

307

The Binary Cooling Tower Process: An Energy Conserving Water Reuse Technology  

E-Print Network [OSTI]

The Binary Cooling Tower (BCT) harnesses cooling system waste heat to accomplish concentration of waste and process streams. The BCT can also be integrated to isolate and improve the efficiency of critical cooling loops. This paper describes the BCT...

Lancaster, R. L.; Sanderson, W. G.; Cooke, R. L., Jr.

1981-01-01T23:59:59.000Z

308

Observational and evolutionary studies of neutron star X-ray binaries  

E-Print Network [OSTI]

In this thesis, we present our observational and evolutionary studies of neutron stars in X-ray binary systems. A variety of topics are discussed, which are all related by a single scientific theme, namely, helping to set ...

Lin, Jinrong, Ph. D. Massachusetts Institute of Technology

2011-01-01T23:59:59.000Z

309

Adsorption and desorption of binary mixtures of volatile organic contaminants on soil  

E-Print Network [OSTI]

, the potential theory and the ideal adsorbed solution theory for mixture adsorption were also evaluated for prediction of the experimental results for binary adsorption. All models failed for prediction of the BET type III isotherms when methanol was present...

Guo, Yang

2012-06-07T23:59:59.000Z

310

The Volatility and the Thermal Storage Performance of Binary Polyalcohol Systems Used in the Wall  

E-Print Network [OSTI]

In this paper, the volatility of binary systems, consisting of neopentylglycol(NPG), pentaerythritol(PE) and trihytdroxy methyl-aminomethane(TAM) with different components, was studied experimentally. In the solid -solid phase change process...

Yan, Q.

2006-01-01T23:59:59.000Z

311

Textural Characterization of Pilc Montmorillonite Pillared with Binary Oxides LaNiOx  

Science Journals Connector (OSTI)

Montmorillonite pillared clay was synthesized by intercalation of binuclear complex of the form NiLa(fsaen)NO3 and subsequent calcination at 500C. The binary oxides of the form NiLaOx thus created inside the lay...

S. P. Skaribas; P. J. Pomonis; P. Grange

1993-01-01T23:59:59.000Z

312

A Static Birthmark of Binary Executables Based on API Call Structure  

Science Journals Connector (OSTI)

A software birthmark is a unique characteristic of a program that can be used as a software theft detection. In this paper we suggest and empirically evaluate a static birthmark of binary executables based on API

Seokwoo Choi; Heewan Park; Hyun-il Lim

2007-01-01T23:59:59.000Z

313

Effect of eccentricity on binary neutron star searches in Advanced LIGO  

E-Print Network [OSTI]

Binary neutron stars (BNSs) are the primary source of gravitational waves for the Laser Interferometer Gravitational-Wave Observatory (LIGO) and its international partners Virgo and KAGRA. Current BNS searches target field binaries whose orbits will have circularized by radiation reaction before their gravitational waves enter the Advanced LIGO sensitive band at 15 Hz. It has been suggested that a population of BNSs may form by n-body interactions near supermassive black holes or in globular clusters and that these systems may have non-negligible eccentricity in the Advanced LIGO band. We show that for BNS systems with total mass of 2.4 (6.0) solar masses, the effect of eccentricity e search is effectual for these binaries. For eccentricities up to e = 0.4, we investigate the selection bias caused by neglecting eccentricity in BNS searches. If such high eccentricity systems exist, searches that specifically target eccentric binaries will be needed in Advanced LIGO and Virgo.

E. A. Huerta; Duncan A. Brown

2013-06-07T23:59:59.000Z

314

RADIAL VELOCITIES OF GALACTIC O-TYPE STARS. II. SINGLE-LINED SPECTROSCOPIC BINARIES  

SciTech Connect (OSTI)

We report on new radial velocity measurements of massive stars that are either suspected binaries or lacking prior observations. This is part of a survey to identify and characterize spectroscopic binaries among O-type stars with the goal of comparing the binary fraction of field and runaway stars with those in clusters and associations. We present orbits for HDE 308813, HD 152147, HD 164536, BD-16 Degree-Sign 4826, and HDE 229232, Galactic O-type stars exhibiting single-lined spectroscopic variation. By fitting model spectra to our observed spectra, we obtain estimates for effective temperature, surface gravity, and rotational velocity. We compute orbital periods and velocity semiamplitudes for each system and note the lack of photometric variation for any system. These binaries probably appear single-lined because the companions are faint and because their orbital Doppler shifts are small compared to the width of the rotationally broadened lines of the primary.

Williams, S. J.; Gies, D. R. [Center for High Angular Resolution Astronomy and Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106 (United States); Hillwig, T. C. [Department of Physics and Astronomy, Valparaiso University, Valparaiso, IN 46383 (United States); McSwain, M. V. [Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015 (United States); Huang, W., E-mail: swilliams@chara.gsu.edu, E-mail: gies@chara.gsu.edu, E-mail: todd.hillwig@valpo.edu, E-mail: mcswain@lehigh.edu, E-mail: hwenjin@astro.washington.edu [Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195-1580 (United States)

2013-02-01T23:59:59.000Z

315

Binary Restoration of Thin Objects in Multidimensional Imagery Jeffrey E. Boyd  

E-Print Network [OSTI]

Binary Restoration of Thin Objects in Multidimensional Imagery Jeffrey E. Boyd Department becomes trivial. Such is the case #12; Boyd and Meloche, PAMI, Vol. 20, No. 6, p647--651, June 98. 2 (a

Boyd, Jeffrey E.

316

Heat Pipe Performance Enhancement with Binary Mixture Fluids that Exhibit Strong Concentration Marangoni Effects  

E-Print Network [OSTI]

on a flat-plate solar heat collector with integrated solarBinary Mixture Nucleate Boiling Heat Transfer CorrelationsG.E. , 1965, A study of heat transfer in nucleate pool

Armijo, Kenneth Miguel

2011-01-01T23:59:59.000Z

317

Report on the first binary black hole inspiral search in LIGO data  

E-Print Network [OSTI]

The LIGO Scientific Collaboration is currently engaged in the first search for binary black hole inspiral signals in real data. We are using the data from the second LIGO science run and we focus on inspiral signals coming from binary systems with component masses between 3 and 20 solar masses. We describe the analysis methods used and report on preliminary estimates for the sensitivities of the LIGO instruments during the second science run.

Eirini Messaritaki; for the LIGO Scientific Collaboration

2005-04-14T23:59:59.000Z

318

An experimental investigation of binary solidification in a vertical channel with thermal and solutal mixed convection  

SciTech Connect (OSTI)

Experimental measurements and photographic observations are presented for the solidification of a binary, aqueous ammonium chloride solution in a vertical channel. Transient liquidus front progressions and temperature measurements are used to characterize the influences of flow rate, superheat, composition, and chill wall temperature on binary phase-change behavior. Experimental results are compared with previously reported model predictions and discrepancies are used to critically assess model assumptions and limitations.

Bennon, W.D. (Aluminum Company of America, Alcoa Center, PA 15069 (USA)); Incropera, F.P. (Heat Transfer Laboratory, School of Mechanical Engineering, Purdue University, West Lafayette, IN 47907 (USA))

1989-08-01T23:59:59.000Z

319

Gravitational Waves from Coalescing Binary Black Holes: Theoretical and Experimental Challenges  

ScienceCinema (OSTI)

A network of ground-based interferometric gravitational wave detectors (LIGO/VIRGO/GEO/...) is currently taking data near its planned sensitivity. Coalescing black hole binaries are among the most promising, and most exciting, gravitational wave sources for these detectors. The talk will review the theoretical and experimental challenges that must be met in order to successfully detect gravitational waves from coalescing black hole binaries, and to be able to reliably measure the physical parameters of the source (masses, spins, ...).

None

2011-10-06T23:59:59.000Z

320

The detectability of eccentric compact binary coalescences with advanced gravitational-wave detectors  

E-Print Network [OSTI]

Compact binary coalescences are a promising source of gravitational waves for second-generation interferometric gravitational-wave detectors such as advanced LIGO and advanced Virgo. While most binaries are expected to possess circular orbits, some may be eccentric, for example, if they are formed through dynamical capture. Eccentric orbits can create difficulty for matched filtering searches due to the challenges of creating effective template banks to detect these signals. In previous work, we showed how seedless clustering can be used to detect low-mass ($M_\\text{total}\\leq10M_\\odot$) compact binary coalescences for both spinning and eccentric systems, assuming a circular post-Newtonian expansion. Here, we describe a parameterization that is designed to maximize sensitivity to low-eccentricity ($0\\leq\\epsilon\\leq0.6$) systems, derived from the analytic equations. We show that this parameterization provides a robust and computationally efficient method for detecting eccentric low-mass compact binaries. Based on these results, we conclude that advanced detectors will have a chance of detecting eccentric binaries if optimistic models prove true. However, a null observation is unlikely to firmly rule out models of eccentric binary populations.

Michael Coughlin; Patrick Meyers; Eric Thrane; Jialun Luo; Nelson Christensen

2014-12-19T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


321

A simple model of complete precessing black-hole-binary gravitational waveforms  

E-Print Network [OSTI]

The construction of a model of the gravitational-wave (GW) signal from generic configurations of spinning-black-hole binaries, through inspiral, merger and ringdown, is one of the most pressing theoretical problems in the build-up to the era of GW astronomy. We present the first such model in the frequency domain, "PhenomP", which captures the basic phenomenology of the seven-dimensional parameter space of binary configurations with only three key physical parameters. Two of these (the binary's mass ratio and an effective total spin parallel to the orbital angular momentum, which determines the inspiral rate) define an underlying non-precessing-binary model. The non-precessing-binary waveforms are then "twisted up" with approximate expressions for the precessional motion, which require only one additional physical parameter, an effective precession spin, $\\chi_p$. All other parameters (total mass, sky location, orientation and polarisation, and initial phase) can be specified trivially. The model is constructed in the frequency domain, which will be essential for efficient GW searches and source measurements. We have tested the model's fidelity for GW applications by comparison against hybrid post-Newtonian-numerical-relativity waveforms at a variety of configurations --although we did not use these numerical simulations in the construction of the model. Our model can be used to develop GW searches, to study the implications for astrophysical measurements, and as a simple conceptual framework to form the basis of generic-binary waveform modelling in the advanced-detector era.

Mark Hannam; Patricia Schmidt; Alejandro Boh; Leila Haegel; Sascha Husa; Frank Ohme; Geraint Pratten; Michael Prrer

2014-09-19T23:59:59.000Z

322

LBQS 0103-2753 A 0.3 Arcsec Binary Quasar  

E-Print Network [OSTI]

Imaging and spectroscopy with HST show that LBQS 0103-2753 (V = 17.8, z = 0.848) is a binary quasar with a separation of 0.3 arcsec or 2.3 kpc. This is by far the smallest separation binary quasar reported to date. The two components have very different spectra, including the presence of strong broad absorption lines (BALs) in component A only. The emission-line redshifts, based on the broad high ionization C IV lines, are z_A = 0.834 and z_B = 0.858; their difference is 3900 km/s in velocity units. The broad C IV lines, however, are probably not a good indicator of systemic redshift; and LBQS 0103-2753 A and B could have a much smaller systemic redshift difference, like the other known binary quasars. If the systemic redshift difference is small, then LBQS 0103-2753 would most likely be a galaxy merger that has led to a binary supermassive black hole. There is now one known 0.3 arcsec binary among roughly 500 QSOs that have been observed in a way that would reveal such a close binary. This suggests that QSO ...

Junkkarinen, V T; Beaver, E A; Burbidge, Eleanor Margaret; Cohen, R D; Hamann, F W; Lyons, R W

2001-01-01T23:59:59.000Z

323

How does a thermal binary crystal break under shear?  

E-Print Network [OSTI]

When exposed to strong shearing, the particles in a crystal will rearrange and ultimately, the crystal will break by forming large nonaffine defects. Even for the initial stage of this process, only little effort has been devoted to the understanding of the breaking process on the scale of the individual particle size for thermalized mixed crystals. Here, we explore the shear-induced breaking for an equimolar two-dimensional binary model crystal with a high interaction asymmetry between the two different species such that the initial crystal has an intersecting square sublattice of the two constituents. Using Brownian dynamics computer simulations, we show that the combination of shear and thermal fluctuations leads to a characteristic hierarchical breaking scenario where initially, the more strongly coupled particles are thermally distorted, paving the way for the weakly coupled particles to escape from their cage. This in turn leads to mobile defects which may finally merge, proliferating a cascade of defects, which triggers the final breakage of the crystal. This scenario is in marked contrast to the breakage of one-component crystals close to melting. Moreover, we explore the orientational dependence of the initial shear direction relative to the crystal orientation and compare this to the usual melting scenario without shear. Our results are verifiable in real-space experiments of superparamagnetic colloidal mixtures at a pending air-water interface in an external magnetic field where the shear can be induced by an external laser field.

Tobias Horn; Hartmut Lwen

2014-11-21T23:59:59.000Z

324

Magnetospheric Eclipses in the Binary Pulsar J0737-3039  

E-Print Network [OSTI]

(Abridged) In the binary radio pulsar system J0737-3039, the faster pulsar A is eclipsed once per orbit. We construct a simple geometric model which successfully reproduces the eclipse light curves, based on the idea that the radio pulses are attenuated by synchrotron absorption on the closed magnetic field lines of pulsar B. The model explains most of the properties of the eclipse: its asymmetric form, the nearly frequency-independent duration, and the modulation of the brightness of pulsar A at both once and twice the rotation frequency of pulsar B in different parts of the eclipse. This detailed agreement confirms the dipolar structure of the star's poloidal magnetic field. The model makes clear predictions for the degree of linear polarization of the transmitted radiation. The weak frequency dependence of the eclipse duration implies that the absorbing plasma is relativistic, with a density much larger than the corotation charge density. Such hot, dense plasma can be effectively stored in the outer magnetosphere, where cyclotron cooling is slow. The gradual loss of particles inward through the cooling radius is compensated by an upward flux driven by a fluctuating component of the current, and by the pumping of magnetic helicity on the closed field lines. The trapped particles are heated to relativistic energies by the damping of magnetospheric turbulence and, at a slower rate, by the absorption of the radio emission of the companion pulsar.

Maxim Lyutikov; Christopher Thompson

2005-02-17T23:59:59.000Z

325

A magnetic white dwarf in a detached eclipsing binary  

E-Print Network [OSTI]

SDSS J030308.35+005444.1 is a close, detached, eclipsing white dwarf plus M dwarf binary which shows a large infrared excess which has been interpreted in terms of a circumbinary dust disk. In this paper we present optical and near-infrared photometric and spectroscopic data for this system. At optical wavelengths we observe heated pole caps from the white dwarf caused by accretion of wind material from the main-sequence star on to the white dwarf. At near-infrared wavelengths we see the eclipse of two poles on the surface of the white dwarf by the main-sequence star, indicating that the white dwarf is magnetic. Our spectroscopic observations reveal Zeeman split emission lines in the hydrogen Balmer series, which we use to measure the magnetic field strength as 8MG. This measurement indicates that the cyclotron lines are located in the infrared, naturally explaining the infrared excess without the need for a circumbinary dust disk. We also detect magnetically-confined material located roughly midway between t...

Parsons, S G; Gnsicke, B T; Schreiber, M R; Bours, M C P; Dhillon, V S; Littlefair, S P

2013-01-01T23:59:59.000Z

326

Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries  

Science Journals Connector (OSTI)

Helium that accretes onto a carbon/oxygen white dwarf in double white dwarf AM Canum Venaticorum (AM CVn) binaries undergoes unstable thermonuclear flashes when the orbital period is in the 3.5-25 minute range. At the shortest orbital periods (and highest accretion rates, > 10-7 M? yr-1), the flashes are weak and likely lead to the helium equivalent of classical nova outbursts. However, as the orbit widens and drops, the mass required for the unstable ignition increases, leading to progressively more violent flashes up to a final flash with helium shell mass ?0.02-0.1 M?. The high pressures of these last flashes allow the burning to produce the radioactive elements 48Cr, 52Fe, and 56Ni that power a faint (MV = -15 to -18) and rapidly rising (few days) thermonuclear supernova. Current galactic AM CVn space densities imply one such explosion every 5,000-15,000 years in 1011 M? of old stars (?2%-6% of the Type Ia rate in E/SO galaxies). These ".Ia" supernovae (one-tenth as bright for one-tenth the time as a Type Ia supernovae) are excellent targets for deep (e.g., V = 24) searches with nightly cadences, potentially yielding an all-sky rate of 1000 per year.

Lars Bildsten; Ken J. Shen; Nevin N. Weinberg; Gijs Nelemans

2007-01-01T23:59:59.000Z

327

Monolithic Active Pixel Matrix with Binary Counters (MAMBO) ASIC  

SciTech Connect (OSTI)

Monolithic Active Matrix with Binary Counters (MAMBO) is a counting ASIC designed for detecting and measuring low energy X-rays from 6-12 keV. Each pixel contains analogue functionality implemented with a charge preamplifier, CR-RC{sup 2} shaper and a baseline restorer. It also contains a window comparator which can be trimmed by 4 bit DACs to remove systematic offsets. The hits are registered by a 12 bit ripple counter which is reconfigured as a shift register to serially output the data from the entire ASIC. Each pixel can be tested individually. Two diverse approaches have been used to prevent coupling between the detector and electronics in MAMBO III and MAMBO IV. MAMBO III is a 3D ASIC, the bottom ASIC consists of diodes which are connected to the top ASIC using {mu}-bump bonds. The detector is decoupled from the electronics by physically separating them on two tiers and using several metal layers as a shield. MAMBO IV is a monolithic structure which uses a nested well approach to isolate the detector from the electronics. The ASICs are being fabricated using the SOI 0.2 {micro}m OKI process, MAMBO III is 3D bonded at T-Micro and MAMBO IV nested well structure was developed in collaboration between OKI and Fermilab.

Khalid, Farah F.; Deptuch, Grzegorz; Shenai, Alpana; Yarema, Raymond J.; /Fermilab

2010-11-01T23:59:59.000Z

328

Magnetic energy production by turbulence in binary neutron star mergers  

E-Print Network [OSTI]

The simultaneous detection of electromagnetic and gravitational wave emission from merging neutron star binaries would aid greatly in their discovery and interpretation. By studying turbulent amplification of magnetic fields in local high-resolution simulations of neutron star merger conditions, we demonstrate that magnetar-level (~10^16) G fields are present throughout the merger duration. We find that the small-scale turbulent dynamo converts 60% of the randomized kinetic energy into magnetic fields on a merger time scale. Since turbulent magnetic energy dissipates through reconnection events which accelerate relativistic electrons, turbulence may facilitate the conversion of orbital kinetic energy into radiation. If 10^-4 of the ~ 10^53 erg of orbital kinetic available gets processed through reconnection, and creates radiation in the 15-150 keV band, then the fluence at 200 Mpc would be 10^-7 erg/cm^2, potentially rendering most merging neutron stars in the advanced LIGO and Virgo detection volumes detecta...

Zrake, Jonathan

2013-01-01T23:59:59.000Z

329

Irradiation-induced composition patterns in binary solid solutions  

SciTech Connect (OSTI)

A theoretical/computational model for the irradiation-driven compositional instabilities in binary solid solutions has been developed. The model is suitable for investigating the behavior of structural alloys and metallic nuclear fuels in a reactor environment as well as the response of alloy thin films to ion beam irradiation. The model is based on a set of reaction-diffusion equations for the dynamics of vacancies, interstitials, and lattice atoms under irradiation. The dynamics of these species includes the stochastic generation of defects by collision cascades as well as the defect reactions and diffusion. The atomic fluxes in this model are derived based on the transitions of lattice defects. The set of reaction-diffusion equations are stiff, hence a stiffly stable method, also known as the Gear method, has been used to numerically approximate the equations. For the Cu-Au alloy in the solid solution regime, the model results demonstrate the formation of compositional patterns under high-temperature particle irradiation, with Fourier space properties (Fourier spectrum, average wavelength, and wavevector) depending on the cascade damage characteristics, average composition, and irradiation temperature.

Dubey, Santosh; El-Azab, Anter [School of Nuclear Engineering, Purdue University, West Lafayette, Indiana 47906 (United States)] [School of Nuclear Engineering, Purdue University, West Lafayette, Indiana 47906 (United States)

2013-09-28T23:59:59.000Z

330

Summary of Historical Production for Nevada Binary Facilities  

SciTech Connect (OSTI)

The analysis described was initiated to validate inputs used in the US Department of Energys (DOE) economic modeling tool GETEM (Geothermal Electricity Technology Evaluation Model) by using publically available data to identify production trends at operating geothermal binary facilities in the state of Nevada. Data required for this analysis was obtained from the Nevada Bureau of Mines and Geology (NBMG), whom received the original operator reports from the Nevada Division of Minerals (NDOM). The data from the NBMG was inputted into Excel files that have been uploaded to the DOEs National Geothermal Data System (NGDS). Once data was available in an Excel format, production trends for individual wells and facilities could be established for the periods data was available (thru 2009). Additionally, this analysis identified relationships existing between production (temperature and flow rates), power production and plant conversion efficiencies. The data trends showed that temperature declines have a significant impact on power production, and that in some instances operators increased production flow rate to offset power declines. The production trends with time that were identified are being used to update GETEMs default inputs.

Mines, Greg; Hanson, Hillary

2014-09-01T23:59:59.000Z

331

Dynamical evolution of quasi-circular binary black hole data  

E-Print Network [OSTI]

We study the fully nonlinear dynamical evolution of binary black hole data, whose orbital parameters are specified via the effective potential method for determining quasi-circular orbits. The cases studied range from the Cook-Baumgarte innermost stable circular orbit (ISCO) to significantly beyond that separation. In all cases we find the black holes to coalesce (as determined by the appearance of a common apparent horizon) in less than half an orbital period. The results of the numerical simulations indicate that the initial holes are not actually in quasi-circular orbits, but that they are in fact nearly plunging together. The dynamics of the final horizon are studied to determine physical parameters of the final black hole, such as its spin, mass, and oscillation frequency, revealing information about the inspiral process. We show that considerable resolution is required to extract accurate physical information from the final black hole formed in the merger process, and that the quasi-normal modes of the final hole are strongly excited in the merger process. For the ISCO case, by comparing physical measurements of the final black hole formed to the initial data, we estimate that less than 3% of the total energy is radiated in the merger process.

Miguel Alcubierre; Bernd Bruegmann; Peter Diener; F. Siddhartha Guzman; Ian Hawke; Scott Hawley; Frank Herrmann; Michael Koppitz; Denis Pollney; Edward Seidel; Jonathan Thornburg

2004-11-30T23:59:59.000Z

332

The early-type close binary CV Velorum revisited  

E-Print Network [OSTI]

Our goal was to improve the fundamental parameters of the massive close double-lined eclipsing B2.5V+B2.5V binary CV Velorum.We gathered new high-resolution echelle spectroscopy on 13 almost consecutive nights covering essentially two orbits. We computed a simultaneous solution to all the available high-quality radial-velocity and light data with the latest version of the Wilson-Deviney code. We obtained the following values for the physical parameters: $M_1 = 6.066(74) M_\\odot$, $M_2 = 5.972(70) M_\\odot$, $R_1 = 4.126(24) R_\\odot$, $R_2 = 3.908(27) R_\\odot$, $\\log L_1 = 3.20(5) L_\\odot$, and $\\log L_2 = 3.14(5) L_\\odot$. The quoted errors contain a realistic estimate of systematic uncertainties mainly stemming from the effective temperature estimation. We derived abundances for both components and found them to be compatible with those of B stars in the solar neighbourhood. We discovered low-amplitude periodic line-profile variations with the orbital frequency for both components. Their interpretation requires new data with a longer time span. The primary rotates subsynchronously while the secondary's $v\\sin i$ and radius are compatible with synchronous rotation. Finally, we provide an update of the empirical mass-luminosity relation for main-sequence B stars which can be used for statistical predictions of masses or luminosities.

K. Yakut; C. Aerts; Th. Morel

2007-01-25T23:59:59.000Z

333

Faint Thermonuclear Supernovae from AM Canum Venaticorum Binaries  

E-Print Network [OSTI]

Helium that accretes onto a Carbon/Oxygen white dwarf in the double white dwarf AM Canum Venaticorum (AM CVn) binaries undergoes unstable thermonuclear flashes when the orbital period is in the 3.5-25 minute range. At the shortest orbital periods (and highest accretion rates, Mdot > 10^-7 Msol/yr), the flashes are weak and likely lead to the Helium equivalent of classical nova outbursts. However, as the orbit widens and Mdot drops, the mass required for the unstable ignition increases, leading to progressively more violent flashes up to a final flash with Helium shell mass ~ 0.02-0.1 Msol. The high pressures of these last flashes allow the burning to produce the radioactive elements 48Cr, 52Fe, and 56Ni that power a faint (M_V in the range of -15 to -18) and rapidly rising (few days) thermonuclear supernova. Current galactic AM CVn space densities imply one such explosion every 5,000-15,000 years in 10^11 Msol of old stars (~ 2-6% of the Type Ia rate in E/SO galaxies). These ".Ia" supernovae (one-tenth as bright for one-tenth the time as a Type Ia supernovae) are excellent targets for deep (e.g. V=24) searches with nightly cadences, potentially yielding an all-sky rate of 1,000 per year.

Lars Bildsten; Ken J. Shen; Nevin N. Weinberg; Gijs Nelemans

2007-05-06T23:59:59.000Z

334

Sudden loss of mass from a binary gravitating system  

Science Journals Connector (OSTI)

A recent discussion by Mitalas is generalized to treat sudden mass loss from a binary system in an originally e l l i p t i c a l orbit. Emphasis is placed on characterizing the orbits by angular momentum and energy and it is shown that none of the changes in the r e l a t i v e orbit depends on which object loses part of its mass; indeed in principle each could lose a different fraction. Time averages are introduced so that the orbital changes which depend on w h e r e in orbit the mass loss occurs can be suitably averaged over a statistical ensemble of initial systems. Although I present several results that appear to be new (such as a unique relation between the increase in the semimajor axis and the change in eccentricity independent of the orbital phase at the moment of mass loss) the main thrust is to choose and manipulate variables yielding the greatest economy of description and the greatest power of computation. (All calculations were easily done on a pocket calculator.) Graphs are presented showing the fraction of systems that on the average will be disrupted the mean orbital changes for the survivors (which can easily turn out to have s m a l l e r mean eccentricity than the progenitors) and the extreme limits for the change in eccentricity.

Peter D. Noerdlinger

1982-01-01T23:59:59.000Z

335

The Evolution of the Multiplicity of Embedded Protostars. II. Binary Separation Distribution and Analysis  

Science Journals Connector (OSTI)

We present the Class I protostellar binary separation distribution based on the data tabulated in a companion paper. We verify the excess of Class I binary stars over solar-type main-sequence stars in the separation range from 500 AU to 4500 AU. Although our sources are in nearby star-forming regions distributed across the entire sky (including Orion), none of our objects are in a high stellar density environment. A log-normal function, used by previous authors to fit the main-sequence and T Tauri binary separation distributions, poorly fits our data, and we determine that a log-uniform function is a better fit. Our observations show that the binary separation distribution changes significantly during the Class I phase, and that the binary frequency at separations greater than 1000 AU declines steadily with respect to spectral index. Despite these changes, the binary frequency remains constant until the end of the Class I phase, when it drops sharply. We propose a scenario to account for the changes in the Class I binary separation distribution. This scenario postulates that a large number of companions with a separation greater than ~1000 AU were ejected during the Class 0 phase, but remain gravitationally bound due to the significant mass of the Class I envelope. As the envelope dissipates, these companions become unbound and the binary frequency at wide separations declines. Circumstellar and circumbinary disks are expected to play an important role in the orbital evolution at closer separations. This scenario predicts that a large number of Class 0 objects should be non-hierarchical multiple systems, and that many Class I young stellar objects (YSOs) with a widely separated companion should also have a very close companion. We also find that Class I protostars are not dynamically pristine, but have experienced dynamical evolution before they are visible as Class I objects. Our analysis shows that the Class I binary frequency and the binary separation distribution strongly depend on the star-forming environment.

Michael S. Connelley; Bo Reipurth; Alan T. Tokunaga

2008-01-01T23:59:59.000Z

336

SKA SA test telescope reveals binary star system South Africa's test telescope reveals secrets of a binary star system and proves the country is able to  

E-Print Network [OSTI]

SKA SA test telescope reveals binary star system South Africa's test telescope reveals secrets, has created huge research and job opportunities. South Africa's Karoo Array Telescope (KAT-7) has at the SKA South Africa. The 64-dish MeerKAT ­ which SKA South Africa director Bernie Fanaroff once described

Jarrett, Thomas H.

337

Energy Dissipation Through Quasi-static Tides in White Dwarf Binaries  

Science Journals Connector (OSTI)

We present a formalism to study tidal interactions in white dwarf binaries in the limiting case of quasi-static tides, in which the tidal forcing frequencies are small, compared to the inverse of the white dwarf's dynamical timescale. The formalism is valid for arbitrary orbital eccentricities and therefore applicable to white dwarf binaries in the Galactic disk as well as globular clusters. In the quasi-static limit, the total perturbation of the gravitational potential shows a phase shift with respect to the position of the companion, the magnitude of which is determined primarily by the efficiency of energy dissipation through convective damping. We determine rates of secular evolution of the orbital elements and white dwarf rotational angular velocity for a 0.3 M ? helium white dwarf in binaries with orbital frequencies in the Laser Interferometer Space Antenna (LISA) gravitational wave frequency band and companion masses ranging from 0.3 M ? to 105 M ?. The resulting tidal evolution timescales for the orbital semimajor axis are longer than a Hubble time, so that convective damping of quasi-static tides need not be considered in the construction of gravitational wave templates of white dwarf binaries in the LISA band. Spin-up of the white dwarf, on the other hand, can occur on timescales of less than 10Myr, provided that the white dwarf is initially rotating with a frequency much smaller than the orbital frequency. For semi-detached white dwarf binaries spin-up can occur on timescales of less than 1Myr. Nevertheless, the timescales remain longer than the orbital inspiral timescales due to gravitational radiation, so that the degree of asynchronism in these binaries increases. As a consequence, tidal forcing eventually occurs at forcing frequencies beyond the quasi-static tide approximation. For the shortest period binaries, energy dissipation is therefore expected to take place through dynamic tides and resonantly excited g-modes.

B. Willems; C. J. Deloye; V. Kalogera

2010-01-01T23:59:59.000Z

338

Energy Dissipation through Quasi-Static Tides in White Dwarf Binaries  

E-Print Network [OSTI]

We study tidal interactions in white dwarf binaries in the limiting case of quasi-static tides. The formalism is valid for arbitrary orbital eccentricities and therefore applicable to white dwarf binaries in the Galactic disk as well as globular clusters. In the quasi-static limit, the total perturbation of the gravitational potential shows a phase shift with respect to the position of the companion, the magnitude of which is determined primarily by the efficiency of energy dissipation through convective damping. We determine rates of secular evolution of the orbital elements and white dwarf rotational angular velocity for a 0.3 solar mass helium white dwarf in binaries with orbital frequencies in the LISA gravitational wave frequency band and companion masses ranging from 0.3 to 10^5 solar masses. The resulting tidal evolution time scales for the orbital semi-major axis are longer than a Hubble time, so that convective damping of quasi-static tides need not be considered in the construction of gravitational wave templates of white dwarf binaries in the LISA band. Spin-up of the white dwarf, on the other hand, can occur on time scales of less than 10Myr, provided that the white dwarf is initially rotating with a frequency much smaller than the orbital frequency. For semi-detached white dwarf binaries spin-up can occur on time scales of less than 1Myr. Nevertheless, the time scales remain longer than the orbital inspiral time scales due to gravitational radiation, so that the degree of asynchronism in these binaries increases. As a consequence, tidal forcing eventually occurs at forcing frequencies beyond the quasi-static tide approximation. For the shortest period binaries, energy dissipation is therefore expected to take place through dynamic tides and resonantly excited g-modes.

B. Willems; C. J. Deloye; V. Kalogera

2009-04-13T23:59:59.000Z

339

Formation of binary phase gratings in photopolymer-liquid crystal composites by a surface-controlled anisotropic phase separation  

SciTech Connect (OSTI)

We report on formation of binary phase gratings in photopolymer-liquid crystal (PLC) composites using a surface-controlled phase separation method. The binary nature of the PLC phase gratings is produced by employing a single step photo-ablation through an amplitude photomask which precisely controls the interfacial interactions between the LC and the photopolymer on the alignment layer. A subsequent illumination of the ultraviolet light onto the whole PLC promotes an anisotropic phase separation resulting in the formation of distinct binary patterns for the PLC structure. The electrically tunable diffraction properties of the binary phase gratings are presented.

Park, Jae-Hong; Khoo, Iam Choon; Yu, Chang-Jae; Jung, Min-Sik; Lee, Sin-Doo [216 Electrical Engineering East, Pennsylvania State University, University Park, Pennsylvania 16802 (United States); School of Electrical Engineering no. 32, Seoul National University, Kwanak P.O. Box 34, Seoul 151-600 (Korea, Republic of)

2005-01-10T23:59:59.000Z

340

Verification of universal surface scaling behavior in critical binary liquid mixtures with neutron and x-ray reflectometry.  

E-Print Network [OSTI]

??We have studied two critical binary liquid mixtures in the mixed phase regime with x-ray and neutron reflectometry to verify universal critical scaling at a (more)

Brown, Matthew D.

2007-01-01T23:59:59.000Z

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341

Do X-ray Binary Spectral State Transition Luminosities Vary?  

E-Print Network [OSTI]

We tabulate the luminosities of the soft-to-hard state transitions of all X-ray binaries for which there exist good X-ray flux measurements at the time of the transition, good distance estimates, and good mass estimates for the compact star. We show that the state transition luminosities are at about 1-4% of the Eddington rate, markedly smaller than those typically quoted in the literature, with a mean value of 2%. Only the black hole candidate GRO J~1655-40 and the neutron star systems Aql X-1 and 4U 1728-34 have measured state transition luminosities inconsistent with this value at the 1$\\sigma$ level. GRO J~1655-40, in particular, shows a state transition luminosity below the mean value for the other sources at the $4\\sigma$ level. This result, combined with the known inner disk inclination angle (the disk is nearly parallel to the line of sight) from GRO J~1655-40's relativistic jets suggest that the hard X-ray emitting region in GRO J~1655-40 can have a velocity of no more than about $\\beta=0.68$, with a most likely value of about $\\beta=0.52$, and a minimum speed of $\\beta=0.45$, assuming that the variations in state transition luminosities are solely due to relativistic beaming effects. The variance in the state transition luminosities suggests an emission region with a velocity of $\\sim0.2c$. The results are discussed in terms of different emission models for the low/hard state. We also discuss the implications for measuring the dimensionless viscosity parameter $\\alpha$. We also find that if its state transitions occur at typical luminosities, then GX 339-4 is likely to be at a distance of at least 7.6 kpc, much further than typically quoted estimates.

Thomas J. Maccarone

2003-08-02T23:59:59.000Z

342

ON THE PULSATIONAL-ORBITAL-PERIOD RELATION OF ECLIPSING BINARIES WITH ?-SCT COMPONENTS  

SciTech Connect (OSTI)

We have deduced a theoretical relation between the pulsation and orbital-periods of pulsating stars in close binaries based on their Roche lobe filling. It appears to be of a simple linear form, with the slope as a function of the pulsation constant, the mass ratio, and the filling factor for an individual system. Testing the data of 69 known eclipsing binaries containing ?-Sct-type components yields an empirical slope of 0.020 0.006 for the P{sub pul}-P{sub orb} relation. We have further derived the upper limit of the P{sub pul}/P{sub orb} ratio for the ?-Sct stars in eclipsing binaries with a value of 0.09 0.02. This value could serve as a criterion to distinguish whether or not a pulsator in an eclipsing binary pulsates in the p-mode. Applying the deduced P{sub pul}-P{sub orb} relation, we have computed the dominant pulsation constants for 37 ?-Sct stars in eclipsing systems with definite photometric solutions. These ranged between 0.008 and 0.033 days with a mean value of about 0.014 days, indicating that ?-Sct stars in eclipsing binaries mostly pulsate in the fourth or fifth overtones.

Zhang, X. B.; Luo, C. Q. [Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012 (China); Fu, J. N. [Department of Astronomy, Beijing Normal University, Beijing 100875 (China)

2013-11-01T23:59:59.000Z

343

Photometry of four binary subdwarf B stars and the nature of their unseen companion stars  

E-Print Network [OSTI]

We present lightcurves of four binary subdwarf B stars, Ton 245, Feige 11, PG1432+159 and PG1017-086. We also present new spectroscopic data for PG1017-086 from which we derive its orbital period, P=0.073d, and the mass function, f_m = 0.0010 +/- 0.0002 solar masses. This is the shortest period for an sdB binary measured to-date. The values of P and f_m for the other sdB binaries have been published elsewhere. We are able to exclude the possibility that the unseen companion stars to Ton 245, Feige 11 and PG1432+159 are main-sequence stars or sub-giant stars from the absence of a sinusoidal signal which would be caused by the irradiation of such a companion star, i.e., they show no reflection effect. The unseen companion stars in these binaries are likely to be white dwarf stars. By contrast, the reflection effect in PG1017-086 is clearly seen. The lack of eclipses in this binary combined with other data suggests that the companion is a low mass M-dwarf or, perhaps, a brown dwarf.

P. F. L. Maxted; T. R. Marsh; U. Heber; L. Morales-Rueda; R. C. North; W. A. Lawson

2002-02-08T23:59:59.000Z

344

Heber Binary-Cycle Geothermal Demonstration Power Plant: Half-load testing, performance, and thermodynamics  

SciTech Connect (OSTI)

This report describes the project's activities during the period July 1986 through June 1987; and includes results of two annual outages and eight months of low power testing and operating. The Heber Binary-Cycle Geothermal Demonstration Power Plant is a 45 MWe electric power generating plant in the Imperial Valley of Southern California. The purpose of the Heber Binary Project is to demonstrate the capability of binary-cycle technology to economically utilize moderate-temperature (300/degree/F to 410/degree/F (150/degree/C to 210/degree/C)) geothermal resources for electric power production. The main objective of the project is to show performance, cost, and environmental acceptability of binary-cycle technology. Experience with demonstration plant and heat supply facilities is described. Details of equipment problems are included. Heat supply shortfall prevented the planned ascent to full power, but binary-cycle experience was favorable at power levels up to 50% of design. 68 refs., 80 figs., 34 tabs.

Berning, J.L.; Fishbaugher, J.R.

1988-08-01T23:59:59.000Z

345

Wind mass transfer in S-type symbiotic binaries I. Focusing by the wind compression model  

E-Print Network [OSTI]

Context: Luminosities of hot components in symbiotic binaries require accretion rates that are higher than those that can be achieved via a standard Bondi-Hoyle accretion. This implies that the wind mass transfer in symbiotic binaries has to be more efficient. Aims: We suggest that the accretion rate onto the white dwarfs (WDs) in S-type symbiotic binaries can be enhanced sufficiently by focusing the wind from their slowly rotating normal giants towards the binary orbital plane. Methods: We applied the wind compression model to the stellar wind of slowly rotating red giants in S-type symbiotic binaries. Results: Our analysis reveals that for typical terminal velocities of the giant wind, 20 to 50 km/s, and measured rotational velocities between 6 and 10 km/s, the densities of the compressed wind at a typical distance of the accretor from its donor correspond to the mass-loss rate, which can be a factor of $\\sim$10 higher than for the spherically symmetric wind. This allows the WD to accrete at rates of $10^{-...

Skopal, Augustin

2014-01-01T23:59:59.000Z

346

Testing Low-Mass Stellar Models: Three New Detached Eclipsing Binaries below 0.75 Msun  

E-Print Network [OSTI]

Full tests to stellar models below 1 Msun have been hindered until now by the scarce number of precise measurements of the stars' most fundamental parameters: their masses and radii. With the current observational techniques, the required precision to distinguish between different models (errors < 2-3 %) can only be achieved using detached eclipsing binaries where 1) both stars are similar in mass, i.e. q = M1/M2 ~ 1.0, and 2) each star is a main sequence object below 1 Msun. Until 2003 only three such binaries had been found and analyzed in detail. Two new systems were published in 2005 (Creevey et al.; Lopez-Morales & Ribas), almost doubling the previous number of data points. Here we present preliminary results for 3 new low-mass detached eclipsing binaries. These are the first studied systems from our sample of over 41 new binaries (Shaw & Lopez-Morales, this proceedings). We also provide an updated comparison between the Mass-Radius and the Mass-Teff relations predicted by the models and the observational data from detached eclipsing binaries.

Mercedes Lopez-Morales; J. Scott Shaw

2006-03-28T23:59:59.000Z

347

Close binary stars in the solar-age Galactic open cluster M67  

E-Print Network [OSTI]

We present multi-colour time-series CCD photometry of the solar-age galactic open cluster M67 (NGC 2682). About 3600 frames spread over 28 nights were obtained with the 1.5 m Russian-Turkish and 1.2 m Mercator telescopes. High-precision observations of the close binary stars AH Cnc, EV Cnc, ES Cnc, the $\\delta$ Scuti type systems EX Cnc and EW Cnc, and some long-period variables belonging to M67 are presented. Three full multi-colour light curves of the overcontact binary AH Cnc were obtained during three observing seasons. Likewise we gathered three light curves of EV Cnc, an EB-type binary, and two light curves of ES Cnc, a blue straggler binary. Parts of the light change of long-term variables S1024, S1040, S1045, S1063, S1242, and S1264 are obtained. Period variation analysis of AH Cnc, EV Cnc, and ES Cnc were done using all times of mid-eclipse available in the literature and those obtained in this study. In addition, we analyzed multi-colour light curves of the close binaries and also determined new fre...

Yakut, K; Kalomeni, B; Van Winckel, H; Waelkens, C; De Cat, P; Bauwens, E; Vuckovic, M; Saesen, S; Guillou, L Le; Parmaksizoglu, M; Uluc, K; Khamitov, I; Raskin, G; Aerts, C

2009-01-01T23:59:59.000Z

348

Preliminary reliability and availability analysis of the Heber geothermal binary demonstration plant. Final report  

SciTech Connect (OSTI)

An assessment is presented of the reliability and availability of the Heber Geothermal Binary Demonstration Plant on the basis of preliminary design information. It also identifies and ranks components of the plant in order of their criticality to system operation and their contribution to system unavailability. The sensitivity of the various components to uncertainties of data and the potential for reliability growth are also examined. The assessment results were obtained through the adaptation and application of an existing reliability and availability methodology to the Heber plant design. These preliminary assessments were made to assist (1) in evaluating design alternatives for the plant and (2) in demonstrating that the closed-loop, multiple-fluid, binary cycle geothermal concept is competitive with the more conventional flashed steam cycle technology. The Heber Geothermal Binary Demonstration Plant Project is a cooperative effort directed toward accelerating geothermal development for power generation and establishing the binary cycle technology as a proven alternative to the flashed steam cycle for moderate temperature hydrothermal resources. The binary power plant would have a capacity of 45 MW/sub e/ net and would derive its energy from the low salinity (14,000 ppM), moderate temperature (360/sup 0/F, 182/sup 0/C) fluid from the Heber reservoir in southern California.

Himpler, H.; White, J.; Witt, J.

1981-10-01T23:59:59.000Z

349

ANALYSIS OF THE MOTION OF AN EXTRASOLAR PLANET IN A BINARY SYSTEM  

SciTech Connect (OSTI)

More than 10% of extra-solar planets (EPs) orbit in a binary or multiple stellar system. We investigated the motion of planets revolving in binary systems in the case of the three-body problem. We carried out an analysis of the motion of an EP revolving in a binary system with the following conditions: (1) a planet in a binary system revolves around one of the components (parent star); (2) the distance between the star's components is greater than that between the parent star and the orbiting planet (ratio of the semi-major axes is a small parameter); and (3) the mass of the planet is smaller than the mass of the stars, but is not negligible. The Hamiltonian of the system without short periodic terms was used. We expanded the Hamiltonian in terms of the Legendre polynomial and truncated after the second-order term, depending on only one angular variable. In this case, the solution of the system was obtained and the qualitative analysis of the motion was produced. We have applied this theory to real EPs and compared to the numerical integration. Analyses of the possible regions of motion are presented. It is shown that stable and unstable motions of EPs are possible. We applied our calculations to two binary systems hosting an EP and calculated the possible values for their unknown orbital elements.

Plvalov, Eva [Astronomical Institute, Slovak Academy of Science, Bratislava (Slovakia); Solovaya, Nina A., E-mail: plavala@slovanet.sk, E-mail: solov@sai.msu.ru [Sternberg State Astronomical Institute, Lomonosov Moscow State University, Moscow (Russian Federation)

2013-11-01T23:59:59.000Z

350

Domain walls and bubble-droplets in immiscible binary Bose gases  

E-Print Network [OSTI]

The existence and stability of domain walls (DWs) and bubble-droplet (BD) states in binary mixtures of quasi-one-dimensional ultracold Bose gases with inter- and intra-species repulsive interactions is considered. Previously, DWs were studied by means of coupled systems of Gross-Pitaevskii equations (GPEs) with cubic terms, which model immiscible binary Bose-Einstein condensates (BECs). We address immiscible BECs with two- and three-body repulsive interactions, as well as binary Tonks--Girardeau (TG) gases, using systems of GPEs with cubic and quintic nonlinearities for the binary BEC, and coupled nonlinear Schr\\"{o}dinger equations with quintic terms for the TG gases. Exact DW\\ solutions are found for the symmetric BEC mixture, with equal intra-species scattering lengths. Stable asymmetric DWs in the BEC mixtures with dissimilar interactions in the two components, as well as of symmetric and asymmetric DWs in the binary TG gas, are found by means of numerical and approximate analytical methods. In the BEC sy...

Filatrella, G; Salerno, M

2014-01-01T23:59:59.000Z

351

Binaries discovered by the SPY project. IV. Five single-lined DA double white dwarfs  

E-Print Network [OSTI]

We present results from our ongoing follow-up observations of double white dwarf binaries detected in the ESO SN Ia Progenitor SurveY (SPY). We discuss our observing strategy and data analysis and present the orbital solutions of five close double white dwarf binaries: HE0320-1917, HE1511-0448, WD0326-273, WD1013-010 and WD1210+140. Their periods range from 0.44 to 3.22 days. In none of these systems we find any spectral lines originating from the companion. This rules out main sequence companions and indicates that the companion white dwarfs are significantly older and cooler than the bright component. Infrared photometry suggests the presence of a cool, helium-rich white dwarf companion in the binary WD0326-273. We briefly discuss the consequences of our findings for our understanding of the formation and evolution of double white dwarfs.

G. Nelemans; R. Napiwotzki; C. Karl; T. R. Marsh; B. Voss; G. Roelofs; R. G. Izzard; M. Montgomery; T. Reerink; N. Christlieb; D. Reimers

2005-06-10T23:59:59.000Z

352

Gravitational Waveforms for Precessing, Quasicircular Compact Binaries with Multiple Scale Analysis: Small Spin Expansion  

E-Print Network [OSTI]

We obtain analytical gravitational waveforms in the frequency-domain for precessing, quasi-circular compact binaries with small spins, applicable, for example, to binary neutron star inspirals. We begin by calculating an analytic solution to the precession equations, obtained by expanding in the dimensionless spin parameters and using multiple-scale analysis to separate timescales. We proceed by analytically computing the Fourier transform of time-domain waveform through the stationary phase approximation. We show that the latter is valid for systems with small spins. Finally, we show that these waveforms have a high overlap with numerical waveforms obtained through direct integration of the precession equations and discrete Fourier transformations. The resulting, analytic waveform family is ideal for detection and parameter estimation of gravitational waves emitted by inspiraling binary neutron stars with ground-based detectors.

Katerina Chatziioannou; Antoine Klein; Nicolas Yunes; Neil Cornish

2013-07-16T23:59:59.000Z

353

Wide Binary Effects on Asymmetries in Asymptotic Giant Branch Circumstellar Envelopes  

E-Print Network [OSTI]

Observations of increasingly higher spatial resolution reveal the existence of asymmetries in the circumstellar envelopes of a small fraction of asymptotic giant branch (AGB) stars. Although there is no general consensus for their origin, a binary companion star may be responsible. Within this framework, we investigate the gravitational effects associated with a sufficiently wide binary system, where Roche lobe overflow is unimportant, on the outflowing envelopes of AGB stars using three dimensional hydrodynamic simulations. The effects due to individual binary components are separately studied, enabling investigation of the stellar and circumstellar characteristics in detail. The reflex motion of the AGB star alters the wind velocity distribution, thereby, determining the overall shape of the outflowing envelope. On the other hand, the interaction of the companion with the envelope produces a gravitational wake, which exhibits a vertically thinner shape. The two patterns overlap and form clumpy structures. T...

Kim, Hyosun

2012-01-01T23:59:59.000Z

354

A search for binary candidates among the fundamental mode RR Lyrae stars observed by Kepler  

E-Print Network [OSTI]

Although roughly half of all stars are considered to be part of binary or multiple systems, there are only two confirmed cases of RR Lyrae pulsators with companions. One of them is TU Uma (Wade et al 1999) - a classical RR Lyrae star in a very eccentric orbit - and the other is OGLE-BLG-RRLYR-02792 (Pietrzynski et al 2012). Considering the wealth of well-studied RR Lyrae stars, this number is astoundingly low. Having more RR Lyrae stars in binary systems at hand would be extremely valuable to get independent measurements of the masses. The data from the Kepler mission with their unprecedented precision and the long time span of about four years offer a unique possibility to systematically search for the signatures of binarity in RR Lyrae stars. Using the pulsation as a clock, we studied the variations in the timing of maximum light to hunt for possible binary systems in the sample.

Guggenberger, Elisabeth

2014-01-01T23:59:59.000Z

355

The colliding-wind binary WR140: the particle acceleration laboratory  

E-Print Network [OSTI]

WR+O star binary systems exhibit synchrotron emission arising from relativistic electrons accelerated where the wind of the WR star and that of its massive binary companion collide - the wind-collision region (WCR). These ``colliding-wind'' binaries (CWB), provide an excellent laboratory for the study of particle acceleration, with the same physical processes as observed in SNRs, but at much higher mass, photon and magnetic energy densities. WR140 is the best studied CWB, and high resolution radio observations permit a determination of several system parameters, particularly orbit inclination and distance, that are essential constraints for newly developed models of CWBs. We show a model fit to the radio data at orbital phase 0.9, and show how these models may be used to predict the high energy emission from WR140.

S. M. Dougherty; J. M. Pittard

2005-10-18T23:59:59.000Z

356

Shrinking binary and planetary orbits by Kozai cycles with tidal friction  

E-Print Network [OSTI]

At least two arguments suggest that the orbits of a large fraction of binary stars and extrasolar planets shrank by 1-2 orders of magnitude after formation: (i) the physical radius of a star shrinks by a large factor from birth to the main sequence, yet many main-sequence stars have companions orbiting only a few stellar radii away, and (ii) in current theories of planet formation, the region within ~0.1 AU of a protostar is too hot and rarefied for a Jupiter-mass planet to form, yet many "hot Jupiters" are observed at such distances. We investigate orbital shrinkage by the combined effects of secular perturbations from a distant companion star (Kozai oscillations) and tidal friction. We integrate the relevant equations of motion to predict the distribution of orbital elements produced by this process. Binary stars with orbital periods of 0.1 to 10 days, with a median of ~2 d, are produced from binaries with much longer periods (10 d to 10^5 d), consistent with observations indicating that most or all short-period binaries have distant companions (tertiaries). We also make two new testable predictions: (1) For periods between 3 and 10 d, the distribution of the mutual inclination between the inner binary and the tertiary orbit should peak strongly near 40 deg and 140 deg. (2) Extrasolar planets whose host stars have a distant binary companion may also undergo this process, in which case the orbit of the resulting hot Jupiter will typically be misaligned with the equator of its host star.

Daniel Fabrycky; Scott Tremaine

2007-05-30T23:59:59.000Z

357

Search for gravitational waves from low mass compact binary coalescence in LIGOs sixth science run and Virgos science runs 2 and 3  

E-Print Network [OSTI]

We report on a search for gravitational waves from coalescing compact binaries using LIGO and Virgo observations between July 7, 2009, and October 20, 2010. We searched for signals from binaries with total mass between 2 ...

Barsotti, Lisa

358

THE BANANA PROJECT. IV. TWO ALIGNED STELLAR ROTATION AXES IN THE YOUNG ECCENTRIC BINARY SYSTEM EP CRUCIS: PRIMORDIAL ORIENTATION AND TIDAL ALIGNMENT  

E-Print Network [OSTI]

With observations of the EP Cru system, we continue our series of measurements of spin-orbit angles in eclipsing binary star systems, the BANANA project (Binaries Are Not Always Neatly Aligned). We find a close alignment ...

Albrecht, Simon

359

Shear viscosity measurements in the binary mixture butyl cellosolve-water near its upper and lower critical consolute points  

E-Print Network [OSTI]

has been measured for a two-component critical liquid system, butyl cellosolve-water, in the region to report measurements of the shear viscosity of critical binary mixture butyl cello- solve (2-n353 Shear viscosity measurements in the binary mixture butyl cellosolve-water near its upper

Boyer, Edmond

360

Effects of a Supermassive Black Hole Binary on a Nuclear Gas Disk  

E-Print Network [OSTI]

We study influence of a galactic central supermassive black hole (SMBH) binary on gas dynamics and star formation activity in a nuclear gas disk by making three-dimensional Tree+SPH simulations. Due to orbital motions of SMBHs, there are various resonances between gas motion and the SMBH binary motion. We have shown that these resonances create some characteristic structures of gas in the nuclear gas disk, for examples, gas elongated or filament structures, formation of gaseous spiral arms, and small gas disks around SMBHs. In these gaseous dense regions, active star formations are induced. As the result, many star burst regions are formed in the nuclear region.

Hidenori Matsui; Asao Habe; Takayuki R. Saitoh

2006-06-07T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


361

Binary and ternary gas mixtures for use in glow discharge closing switches  

DOE Patents [OSTI]

Highly efficient binary and ternary gas mixtures for use in diffuse glow discharge closing switches are disclosed. The binary mixtures are combinations of helium or neon and selected perfluorides. The ternary mixtures are combinations of helium, neon, or argon, a selected perfluoride, and a small amount of gas that exhibits enhanced ionization characteristics. These mixtures are shown to be the optimum choices for use in diffuse glow discharge closing switches by virtue if the combines physio-electric properties of the mixture components. 9 figs.

Hunter, S.R.; Christophorou, L.G.

1988-04-27T23:59:59.000Z

362

Puna Geothermal Venture 8MW Expantion | Open Energy Information  

Open Energy Info (EERE)

Venture 8MW Expantion Venture 8MW Expantion Jump to: navigation, search OpenEI Reference LibraryAdd to library Journal Article: Puna Geothermal Venture 8MW Expantion Abstract Adding to its existing generating capacity of 27 MW, Ormat's Puna Geothermal Venture (PGV) geothermal power plant recently completed a successful 8MW expansion project bringing more renewable, low-cost electricity to the people of Hawaii. The project presented several technical challenges including use of high scale potential brine in a state-of-the-art binary plant, development of highly reliable brine pH monitoring and control system, and brine injection management in a high energy resource. Each of the project challenges were overcome with unique engineering solutions. Authors Mike Kaleikini, Paul Spielman, Tom Buchanan, Ormat Technologies

363

Brawley- Resurrection Of A Previously Developed Geothermal Field | Open  

Open Energy Info (EERE)

Brawley- Resurrection Of A Previously Developed Geothermal Field Brawley- Resurrection Of A Previously Developed Geothermal Field Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Conference Paper: Brawley- Resurrection Of A Previously Developed Geothermal Field Details Activities (1) Areas (1) Regions (0) Abstract: The Brawley Geothermal Field was originally developed by Unocal. In addition to drilling geothermal wells, this development included building and operating a 10 MWe power plant. Corrosion and scaling issues resulted in Unocal abandoning the project in the 1980's. Ormat Nevada investigated the potential of the shallow sands in 2006. It was concluded that these matrixpermeable sands contained moderately saline water, high porosity, and could support a binary-type power plant. In 2007, Ormat Nevada drilled and tested five wells. These test results confirmed the

364

CX-006662: Categorical Exclusion Determination | Department of Energy  

Broader source: Energy.gov (indexed) [DOE]

62: Categorical Exclusion Determination 62: Categorical Exclusion Determination CX-006662: Categorical Exclusion Determination Geothermal Technologies Program - ORMAT Generator CX(s) Applied: B3.6, B5.1 Date: 10/26/2009 Location(s): Casper, Wyoming Office(s): RMOTC This is for the existing ORMAT geothermal processing unit. The original project consisted of the installation and one year testing of the binary geothermal power unit at the Tensleep battery using the hot produced water source as the heat medium. The unit is connected to the field electrical system for dissipation of the produced energy that is metered and monitored for reliability and quality. It is planned for the unit to remain in place so that an additional approximately 2.5 years of testing can be conducted to evaluate if fouling, erosion, corrosion, and any other factor that may

365

NEPA COMPLIANCE SURVEY  

Broader source: Energy.gov (indexed) [DOE]

7 7 Project lnfonnat ion Project Title: Geothermal Technologies Program - ORMAT Generator Date: 10-22-09 DOE Code: 6730.020.61041 Contractor Code: 8067-731 Project Lead: Lyle Johnson Project Overview 1. What are the environmental This NEPA is for the existing ORMAT geothermal processing unit that was used for testing during CRADA impacts? No 2007-083. The Original project consisted of the installation and 1 year testing of the binary geothermal power unit at the Tensleep battery using the hot produced water source as the heat medium. The unit is 2. What is the legal location? connected to the field electrical system for dissipation of the produced energy that is metered and monitored 3. What is the duration of the project? for reliability and quality. It is planned for the unit to remain in place so that an additional approximately 2.5

366

Brawley Resurrection of a Previously Developed Geothermal Field | Open  

Open Energy Info (EERE)

Brawley Resurrection of a Previously Developed Geothermal Field Brawley Resurrection of a Previously Developed Geothermal Field Jump to: navigation, search OpenEI Reference LibraryAdd to library Journal Article: Brawley Resurrection of a Previously Developed Geothermal Field Abstract The Brawley Geothermal Field was originally developed byUnocal. In addition to drilling geothermal wells, this developmentincluded building and operating a 10 MWe power plant.Corrosion and scaling issues resulted in Unocal abandoning theproject in the 1980's. Ormat Nevada investigated the potentialof the shallow sands in 2006. It was concluded that these matrixpermeablesands contained moderately saline water, high porosity,and could support a binary-type power plant. In 2007, OrmatNevada drilled and tested five wells. These test results confirmedthe earlier conclusions and

367

List of Geothermal Facilities | Open Energy Information  

Open Energy Info (EERE)

Facilities Facilities Jump to: navigation, search Facility Location Owner Aidlin Geothermal Facility Geysers Geothermal Area Calpine Amedee Geothermal Facility Honey Lake, California Amedee Geothermal Venture BLM Geothermal Facility Coso Junction, California, Coso Operating Co. Bear Canyon Geothermal Facility Clear Lake, California, Calpine Beowawe Geothermal Facility Beowawe, Nevada Beowawe Power LLC Big Geysers Geothermal Facility Clear Lake, California Calpine Blundell 1 Geothermal Facility Milford, Utah PacificCorp Energy Blundell 2 Geothermal Facility Milford, Utah PacificCorp Brady Hot Springs I Geothermal Facility Churchill, Nevada Ormat Technologies Inc CE Turbo Geothermal Facility Calipatria, California CalEnergy Generation Calistoga Geothermal Facility The Geysers, California Calpine

368

T-561: IBM and Oracle Java Binary Floating-Point Number Conversion Denial  

Broader source: Energy.gov (indexed) [DOE]

61: IBM and Oracle Java Binary Floating-Point Number Conversion 61: IBM and Oracle Java Binary Floating-Point Number Conversion Denial of Service Vulnerability T-561: IBM and Oracle Java Binary Floating-Point Number Conversion Denial of Service Vulnerability February 21, 2011 - 7:00am Addthis PROBLEM: IBM and Oracle Java Binary Floating-Point Number Conversion Denial of Service Vulnerability. PLATFORM: The following Java products are affected: Java SE: Oracle JDK and JRE 6 Update 23 and prior for Windows, Solaris, and Linux Oracle JDK 5.0 Update 27 and prior for Solaris 9 Oracle SDK 1.4.2_29 and prior for Solaris 8 IBM JDK 6 Update SR9 and prior IBM JDK 5 Update SR12-FP3 and prior IBM JDK 1.4.2 Update SR13-FP8 and prior Java for Business: Oracle JDK and JRE 6 Update 23 and prior for Windows, Solaris, and Linux Oracle JDK and JRE 5.0 Update 27 and prior for Windows, Solaris, and Linux

369

FINDING THE GLOBAL MINIMUM FOR BINARY IMAGE RESTORATION Tony F. Chan  

E-Print Network [OSTI]

- est. In this paper we define the restored image as the global min- imizer of the total-variation (TVFINDING THE GLOBAL MINIMUM FOR BINARY IMAGE RESTORATION Tony F. Chan , Selim Esedo¯glu and Mila and there are no general methods to calculate the global minimum, while local minimziers are very often of limited inter

Esedoglu, Selim

370

Detached white-dwarf close-binary stars -- CV's extended family  

E-Print Network [OSTI]

I review detached binaries consisting of white dwarfs with either other white dwarfs or low mass main-sequence stars in tight orbits around them. Orbital periods have been measured for 15 white dwarf/white dwarf systems and 22 white dwarf/M dwarf systems. While small compared to the number of periods known for CVs (>300), I argue that each variety of detached system has a space density an order of magnitude higher that of CVs. While theory matches the observed distribution of orbital periods of the white dwarf/white dwarf binaries, it predicts white dwarfs of much lower mass than observed. Amongst both types of binary are clear examples of helium core white dwarfs, as opposed to the usual CO composition; similar systems must exist amongst the CVs. White dwarf/M dwarf binaries suffer from selection effects which diminish the numbers seen at long and short periods. They are useful for the study of irradiation; I discuss evidence to suggest that Balmer emission is broadened by optical depth effects to an extent which limits its usefulness for imaging the secondary stars in CVs.

T. R. Marsh

1999-06-07T23:59:59.000Z

371

First all-sky search for continuous gravitational waves from unknown sources in binary systems  

E-Print Network [OSTI]

We present the first results of an all-sky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency- and period-dependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semi-major axes of the orbit from ~0.6e-3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e-24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the low-mass x-ray binary Scorpius X-1 between 20 Hz and 57.25 Hz.

The LIGO Scientific Collaboration; the Virgo Collaboration; J. Aasi; B. P. Abbott; R. Abbott; T. Abbott; M. R. Abernathy; T. Accadia; F. Acernese; K. Ackley; C. Adams; T. Adams; P. Addesso; R. X. Adhikari; C. Affeldt; M. Agathos; N. Aggarwal; O. D. Aguiar; A. Ain; P. Ajith; A. Alemic; B. Allen; A. Allocca; D. Amariutei; M. Andersen; R. Anderson; S. B. Anderson; W. G. Anderson; K. Arai; M. C. Araya; C. Arceneaux; J. Areeda; S. M. Aston; P. Astone; P. Aufmuth; C. Aulbert; L. Austin; B. E. Aylott; S. Babak; P. T. Baker; G. Ballardin; S. W. Ballmer; J. C. Barayoga; M. Barbet; B. C. Barish; D. Barker; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; A. Basti; J. C. Batch; J. Bauchrowitz; Th. S. Bauer; B. Behnke; M. Bejger; M. G. Beker; C. Belczynski; A. S. Bell; C. Bell; G. Bergmann; D. Bersanetti; A. Bertolini; J. Betzwieser; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Biscans; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; S. Bloemen; M. Blom; O. Bock; T. P. Bodiya; M. Boer; G. Bogaert; C. Bogan; C. Bond; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; Sukanta Bose; L. Bosi; C. Bradaschia; P. R. Brady; V. B. Braginsky; M. Branchesi; J. E. Brau; T. Briant; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; A. F. Brooks; D. A. Brown; D. D. Brown; F. Brckner; S. Buchman; T. Bulik; H. J. Bulten; A. Buonanno; R. Burman; D. Buskulic; C. Buy; L. Cadonati; G. Cagnoli; J. Caldern Bustillo; E. Calloni; J. B. Camp; P. Campsie; K. C. Cannon; B. Canuel; J. Cao; C. D. Capano; F. Carbognani; L. Carbone; S. Caride; A. Castiglia; S. Caudill; M. Cavagli; F. Cavalier; R. Cavalieri; C. Celerier; G. Cella; C. Cepeda; E. Cesarini; R. Chakraborty; T. Chalermsongsak; S. J. Chamberlin; S. Chao; P. Charlton; E. Chassande-Mottin; X. Chen; Y. Chen; A. Chincarini; A. Chiummo; H. S. Cho; J. Chow; N. Christensen; Q. Chu; S. S. Y. Chua; S. Chung; G. Ciani; F. Clara; J. A. Clark; F. Cleva; E. Coccia; P. -F. Cohadon; A. Colla; C. Collette; M. Colombini; L. Cominsky; M. Constancio Jr.; A. Conte; D. Cook; T. R. Corbitt; M. Cordier; N. Cornish; A. Corpuz; A. Corsi; C. A. Costa; M. W. Coughlin; S. Coughlin; J. -P. Coulon; S. Countryman; P. Couvares; D. M. Coward; M. Cowart; D. C. Coyne; R. Coyne; K. Craig; J. D. E. Creighton; T. D. Creighton; S. G. Crowder; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; T. Dal Canton; M. Damjanic; S. L. Danilishin; S. D'Antonio; K. Danzmann; V. Dattilo; H. Daveloza; M. Davier; G. S. Davies; E. J. Daw; R. Day; T. Dayanga; G. Debreczeni; J. Degallaix; S. Delglise; W. Del Pozzo; T. Denker; T. Dent; H. Dereli; V. Dergachev; R. De Rosa; R. T. DeRosa; R. DeSalvo; S. Dhurandhar; M. Daz; L. Di Fiore; A. Di Lieto; I. Di Palma; A. Di Virgilio; A. Donath; F. Donovan; K. L. Dooley; S. Doravari; S. Dossa; R. Douglas; T. P. Downes; M. Drago; R. W. P. Drever; J. C. Driggers; Z. Du; S. Dwyer; T. Eberle; T. Edo; M. Edwards; A. Effler; H. Eggenstein; P. Ehrens; J. Eichholz; S. S. Eikenberry; G. Endr?czi; R. Essick; T. Etzel; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Q. Fang; S. Farinon; B. Farr; W. M. Farr; M. Favata; H. Fehrmann; M. M. Fejer; D. Feldbaum; F. Feroz; I. Ferrante; F. Ferrini; F. Fidecaro; L. S. Finn; I. Fiori; R. P. Fisher; R. Flaminio; J. -D. Fournier; S. Franco; S. Frasca; F. Frasconi; M. Frede; Z. Frei; A. Freise; R. Frey; T. T. Fricke; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; J. Gair; L. Gammaitoni; S. Gaonkar; F. Garufi; N. Gehrels; G. Gemme; E. Genin; A. Gennai; S. Ghosh; J. A. Giaime; K. D. Giardina; A. Giazotto; C. Gill; J. Gleason; E. Goetz; R. Goetz; L. Gondan; G. Gonzlez; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Goler; R. Gouaty; C. Grf; P. B. Graff; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; P. Groot; H. Grote; K. Grover; S. Grunewald; G. M. Guidi; C. Guido; K. Gushwa; E. K. Gustafson; R. Gustafson; D. Hammer; G. Hammond; M. Hanke; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. Hart; M. T. Hartman; C. -J. Haster; K. Haughian; A. Heidmann; M. Heintze; H. Heitmann; P. Hello; G. Hemming; M. Hendry; I. S. Heng; A. W. Heptonstall; M. Heurs; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; S. Hooper; P. Hopkins; D. J. Hosken; J. Hough; E. J. Howell; Y. Hu; E. Huerta; B. Hughey; S. Husa; S. H. Huttner; M. Huynh; T. Huynh-Dinh; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; B. R. Iyer; K. Izumi; M. Jacobson; E. James; H. Jang; P. Jaranowski; Y. Ji; F. Jimnez-Forteza; W. W. Johnson; D. I. Jones; R. Jones; R. J. G. Jonker; L. Ju; Haris K; P. Kalmus; V. Kalogera; S. Kandhasamy; G. Kang; J. B. Kanner; J. Karlen; M. Kasprzack; E. Katsavounidis; W. Katzman; H. Kaufer; K. Kawabe; F. Kawazoe; F. Kflian; G. M. Keiser; D. Keitel; D. B. Kelley; W. Kells; A. Khalaidovski

2014-05-30T23:59:59.000Z

372

A Comparative Assessment of Malware Classification using Binary Texture Analysis and Dynamic Analysis  

E-Print Network [OSTI]

.ucsb.edu Vinod Yegneswaran SRI International Menlo Park, USA vinod@csl.sri.com Phillip Porras SRI International features. Further, feature extraction requires a time investment per binary that does not scale well and efficient complement to dynamic analysis. Categories and Subject Descriptors D.4.6 [Security and Protection

California at Santa Barbara, University of

373

Short gamma-ray bursts from binary neutron star mergers in globular clusters  

E-Print Network [OSTI]

ARTICLES Short gamma-ray bursts from binary neutron star mergers in globular clusters JONATHAN@cfa.harvard.edu Published online: 29 January 2006; doi:10.1038/nphys214 Observations by the Swift gamma-ray-burst (GRB, the so-called `long' GRBs (>2-200 s) were located by coded aperture imaging of their hard X-ray emission

Loss, Daniel

374

Black-Box Identification for PLC based MPC of a Binary Distillation Column  

E-Print Network [OSTI]

Black-Box Identification for PLC based MPC of a Binary Distillation Column B. Huyck ,, F. Logist J is to upgrade the control system with a linear MPC running on a PLC. However, before a model based controller can be used on a PLC, an accurate (but simple) process model has to be constructed. Hence, the aim

375

Towards new binary compounds: Synthesis of amorphous phosphorus carbide by pulsed laser deposition  

E-Print Network [OSTI]

Towards new binary compounds: Synthesis of amorphous phosphorus carbide by pulsed laser deposition Available online 28 November 2012 Keywords: Phosphorus carbide Pulsed laser deposition X-ray photoelectron possible crystal structures of the as yet unknown phosphorus carbide as a function of composition

Bristol, University of

376

The evolutionary state of short-period magnetic white dwarf binaries  

Science Journals Connector (OSTI)

......al. 2009). Using a grid of magnetic white dwarf...both systems, using a grid stepsize of 3000 K and...Clearly these binaries will benefit greatly from further observations...We used their updated grid of DA white dwarf cooling...monitoring light curve from the SMARTS telescope was presented......

E. Breedt; B. T. Gnsicke; J. Girven; A. J. Drake; C. M. Copperwheat; S. G. Parsons; T. R. Marsh

2012-06-21T23:59:59.000Z

377

Henry's law, surface tension, and surface adsorption in dilute binary mixtures  

E-Print Network [OSTI]

Henry's law, surface tension, and surface adsorption in dilute binary mixtures Akira Onukia. The solute partitioning between gas and liquid Henry's law and the surface tension change are discussed fraction X and the temperature-derivative / T cx,p of the surface tension at fixed pressure p

378

Filling the disk hollow following binary black hole merger: The transient accretion afterglow  

SciTech Connect (OSTI)

Tidal torques from a binary black hole empty out the central regions in any circumbinary gaseous accretion disk. The balance between tidal torques and viscosity maintain the inner edge of the disk at a radius r{approx}1.5a-2a, where a is the binary semimajor axis. Eventually, the inspiraling binary decouples from the disk and merges, leaving behind a central hollow (''donut hole'') in the disk orbiting the remnant black hole. We present a simple, time-dependent, Newtonian calculation that follows the secular (viscous) evolution of the disk as it fills up the hollow down to the black hole innermost stable circular orbit and then relaxes to stationary equilibrium. We use our model to calculate the electromagnetic radiation (''afterglow'') spectrum emitted during this transient accretion epoch. Observing the temporal increase in the total electromagnetic flux and the hardening of the spectrum as the donut hole fills may help confirm a binary black hole merger detected by a gravitational wave interferometer. We show how the very existence of the initial hollow can lead to super-Eddington accretion during this secular phase if the rate is not very far below Eddington prior to decoupling. Our model, though highly idealized, may be useful in establishing some of the key parameters, thermal emission features and scalings that characterize this transient. It can serve as a guide in the design and calibration of future radiation-magnetohydrodynamic simulations in general relativity.

Shapiro, Stuart L. [Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801 (United States)

2010-01-15T23:59:59.000Z

379

Stellar loci II. a model-free estimate of the binary fraction for field FGK stars  

E-Print Network [OSTI]

We propose a Stellar Locus OuTlier (SLOT) method to determine the binary fraction of main-sequence stars statistically. The method is sensitive to neither the period nor mass-ratio distributions of binaries, and able to provide model-free estimates of binary fraction for large numbers of stars of different populations in large survey volumes. We have applied the SLOT method to two samples of stars from the SDSS Stripe 82, constructed by combining the re-calibrated SDSS photometric data with respectively the spectroscopic information from the SDSS and LAMOST surveys. For the SDSS spectroscopic sample, we find an average binary fraction for field FGK stars of $41%\\pm2%$. The fractions decrease toward late spectral types, and are respectively $44%\\pm5%$, $43%\\pm3%$, $35%\\pm5%$, and $28%\\pm6%$ for stars of $g-i$ colors between 0.3 -- 0.6, 0.6 -- 0.9, 0.9 -- 1.2, and 1.2 - 1.6\\,mag. A modest metallicity dependence is also found. The fraction decreases with increasing metallicity. For stars of [Fe/H] between $-0.5$...

Yuan, Haibo; Xiang, Maosheng; Huang, Yang; Chen, Bingqiu

2014-01-01T23:59:59.000Z

380

On the invertibility of the XOR rotations of a binary word  

E-Print Network [OSTI]

We prove the following result regarding operations on a binary word whose length is a power of two: computing the exclusive-or of a number of rotated versions of the word is an invertible (one-to-one) operation if and only ...

Rivest, Ronald L.

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


381

TWO NEW LONG-PERIOD HOT SUBDWARF BINARIES WITH DWARF COMPANIONS  

SciTech Connect (OSTI)

Hot subdwarf stars with F-K main sequence binary companions have been known for decades, but the first orbital periods for such systems were published just recently. Current observations suggest that most have long periods, on the order of years, and that some are or once were hierarchical triple systems. As part of a survey with the Hobby-Eberly Telescope, we have been monitoring the radial velocities of several composite-spectra binaries since 2005 in order to determine their periods, velocities, and eccentricities. Here we present observations and orbital solutions for two of these systems, PG 1449+653 and PG 1701+359. Similar to the other sdB+F/G/K binaries with solved orbits, their periods are long, 909 and 734 days, respectively, and pose a challenge to current binary population synthesis models of hot subdwarf stars. Intrigued by their relatively large systemic velocities, we also present a kinematical analysis of both targets and find that neither is likely a member of the Galactic thin disk.

Barlow, Brad N.; Wade, Richard A. [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Lab, University Park, PA 16802 (United States); Liss, Sandra E. [Department of Astronomy, University of Virginia, P.O. Box 400325, Charlottesville, VA 22904-4325 (United States); Green, Elizabeth M., E-mail: bbarlow@psu.edu [Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721 (United States)

2013-07-01T23:59:59.000Z

382

Two-dimensional kinetics of binary nucleation in sulfuric acidwater mixtures  

E-Print Network [OSTI]

. INTRODUCTION Binary homogeneous nucleation is a mechanism for gas- to-particle conversion that can result in significant rates of new particle formation even if both components are under- saturated in the gas phase. An important example is the at- mospheric production of sulfuric acid in the presence of am- bient water vapor

383

Targeting supermassive black hole binaries and gravitational wave sources for the pulsar timing array  

Science Journals Connector (OSTI)

......INTRODUCTION Studies of the dynamics...of the two systems, it is customary...from binary systems (Misner, Thorne Wheeler 1973; Maggiore...the pulses (Foster Backer 1990...catalogue, and study how the efficiency...very massive systems in the low-redshift...signal is to study the distribution......

Pablo A. Rosado; Alberto Sesana

2014-01-01T23:59:59.000Z

384

Chemical Reaction of Metal-Carbon Binary Cluster Anions by FT-ICR Mass Spectrometer  

E-Print Network [OSTI]

45 48 51 54 57 60 Number of Carbon Atoms Intensity(arbitrary) (a) as injected (b) SWIFTed (c) NO 1sChemical Reaction of Metal-Carbon Binary Cluster Anions by FT-ICR Mass Spectrometer S. Maruyama, M- fullerene and single walled carbon nanotubes are investigated through experimental studies of interaction

Maruyama, Shigeo

385

FT-ICR ,,,Carbon Clusters and Metal/Carbon Binary Clusters  

E-Print Network [OSTI]

60 70 80 720 760 800 Ion Mass [amu] ScC60 + C64 + Number of Carbon Atoms Intensity(arb.units) ScC60FT-ICR ,?,æ,éCarbon Clusters and Metal/Carbon Binary Clusters ·>Í­ì·³"¹1 ·C Masamichi Kohno1 , Tetsuya

Maruyama, Shigeo

386

An optimal parallel algorithm for the Euclidean distance maps of 2D binary images  

E-Print Network [OSTI]

The Euclidean distance map (EDM) of a black and white n 2 n binary image is the n 2 n map where each element has the Euclidean distance between the corresponding pixel and the nearest black pixel. The EDM plays an important role in machine vision, pattern recognition, and robotics[9]. Many algorithms have been proposed

Fujiwara, Akihiro

387

The Hamilton principle for fluid binary mixtures with two temperatures Henri Gouin1  

E-Print Network [OSTI]

The Hamilton principle for fluid binary mixtures with two temperatures Henri Gouin1 and Tommaso, the Hamilton principle of least action is able to produce the equation of motion for each component that the Hamilton principle can afford to obtain the equations of motions for multi- temperature mixtures of fluids

Boyer, Edmond

388

Gravitational waves from inspiralling compact binaries: Energy loss and waveform to second--post-Newtonian order  

E-Print Network [OSTI]

Gravitational waves generated by inspiralling compact binaries are investigated to the second--post-Newtonian (2PN) approximation of general relativity. Using a recently developed 2PN-accurate wave generation formalism, we compute the gravitational waveform and associated energy loss rate from a binary system of point-masses moving on a quasi-circular orbit. The crucial new input is our computation of the 2PN-accurate ``source'' quadrupole moment of the binary. Tails in both the waveform and energy loss rate at infinity are explicitly computed. Gravitational radiation reaction effects on the orbital frequency and phase of the binary are deduced from the energy loss. In the limiting case of a very small mass ratio between the two bodies we recover the results obtained by black hole perturbation methods. We find that finite mass ratio effects are very significant as they increase the 2PN contribution to the phase by up to 52\\%. The results of this paper should be of use when deciphering the signals observed by the future LIGO/VIRGO network of gravitational-wave detectors.

Luc Blanchet; Thibault Damour; Bala R. Iyer

1995-01-24T23:59:59.000Z

389

White Dwarfs in Binary Systems A white dwarf orbiting another star can become active  

E-Print Network [OSTI]

White Dwarfs in Binary Systems A white dwarf orbiting another star can become active when the other becomes incandescent. #12;H and He from the companion build up on the white dwarf's surface. Classical. Explosions from White Dwarf Star RS Oph #12;Classical Novae: RS Ophiuci Recurrent Nova RS Ophiuci Explosions

Barnes, Joshua Edward

390

In vitro corrosion and biocompatibility of binary magnesium alloys Xuenan Gu a  

E-Print Network [OSTI]

In vitro corrosion and biocompatibility of binary magnesium alloys Xuenan Gu a , Yufeng Zheng a 2 September 2008 Accepted 21 October 2008 Available online 9 November 2008 Keywords: Magnesium alloy Corrosion In vitro Cytotoxicity Hemocompatibility a b s t r a c t As bioabsorbable materials, magnesium

Zheng, Yufeng

391

Simulation of Stresses during Casting of Binary Magnesium-Aluminum Alloys  

E-Print Network [OSTI]

Simulation of Stresses during Casting of Binary Magnesium-Aluminum Alloys M.G. POKORNY, C.A. MONROE properties that are suitable for advanced stress modeling is even more limited for magnesium alloys. Recently of an AZ91 magnesium alloy in order to predict hot tears.[4] This study relied on crude estimates

Beckermann, Christoph

392

Constraining the Equation of State of Neutron Stars from Binary Mergers  

E-Print Network [OSTI]

Determining the equation of state of matter at nuclear density and hence the structure of neutron stars has been a riddle for decades. We show how the imminent detection of gravitational waves from merging neutron star binaries can be used to solve this riddle. Using a large number of accurate numerical-relativity simulations of binaries with nuclear equations of state, we find that the postmerger emission is characterized by two distinct and robust spectral features. While the high-frequency peak has already been associated with the oscillations of the hypermassive neutron star produced by the merger and depends on the equation of state, a new correlation emerges between the low-frequency peak, related to the merger process, and the total compactness of the stars in the binary. More importantly, such a correlation is essentially universal, thus providing a powerful tool to set tight constraints on the equation of state. If the mass of the binary is known from the inspiral signal, the combined use of the two frequency peaks sets four simultaneous constraints to be satisfied. Ideally, even a single detection would be sufficient to select one equation of state over the others. We test our approach with simulated data and verify it works well for all the equations of state considered.

Kentaro Takami; Luciano Rezzolla; Luca Baiotti

2014-03-22T23:59:59.000Z

393

Spectral properties of the post-merger gravitational-wave signal from binary neutron stars  

E-Print Network [OSTI]

Extending previous work by a number of authors, we have recently presented a new approach in which the detection of gravitational waves from merging neutron star binaries can be used to determine the equation of state of matter at nuclear density and hence the structure of neutron stars. In particular, after performing a large number of numerical-relativity simulations of binaries with nuclear equations of state, we have found that the post-merger emission is characterized by two distinct and robust spectral features. While the high-frequency peak was already shown to be associated with the oscillations of the hypermassive neutron star produced by the merger and to depend on the equation of state, we have highlighted that the low-frequency peak is related to the merger process and to the total compactness of the stars in the binary. This relation is essentially universal and provides a powerful tool to set tight constraints on the equation of state. We here provide additional information on the extensive analysis performed, illustrating the methods used, the tests considered, and the robustness of the results. We also discuss additional relations that can be deduced when exploring the data and how these correlate with various properties of the binary. Finally, we present a simple mechanical toy model that explains the main spectral features of the post-merger signal and can even reproduce analytically the complex waveforms emitted right after the merger.

Kentaro Takami; Luciano Rezzolla; Luca Baiotti

2014-12-10T23:59:59.000Z

394

3D binary anti-commutative operadic Lax representations for harmonic oscillator  

E-Print Network [OSTI]

It is explained how the time evolution of the operadic variables may be introduced by using the operadic Lax equation. The operadic Lax representations for the harmonic oscillator are constructed in 3-dimensional binary anti-commutative algebras. As an example, an operadic Lax representation for the harmonic oscillator in the Lie algebra sl(2) is constructed.

Eugen Paal; Jyri Virkepu

2008-06-08T23:59:59.000Z

395

Ionic liquid binary mixtures: Promising reaction media for carbohydrate conversion into 5-hydroxymethylfurfural  

Science Journals Connector (OSTI)

Abstract The conversion of carbohydrates into 5-hydroxymethylfurfural (5-HMF) has been studied in binary mixtures of ionic liquids (ILs), using strongly acidic resin Amberlyst 15 as the catalyst. In particular, both mono- and disaccharides, such as fructose, glucose and sucrose have been investigated. Considering the favorable effect exerted by chloride-based ionic liquids in the dissolution of carbohydrates, we used binary mixtures of 1-butyl-3-methylimidazolium chloride ([bmim][Cl]) with [bmim+] based ionic liquids differing in size, shape and coordination ability of the anion ([bmim][BF4], [bmim][N(CF3SO2)2], [bmim][N(CN)2], [bmim][SbF6] and [bmim][CF3SO3]). Carbohydrate conversion in [bmim][BF4]/[bmim][Cl] binary mixtures, has been studied under both magnetic stirring and ultrasound (US) activation. The catalytic system used led to the formation of 5-hydroxymethylfurfural in good yield under mild conditions. A significant influence of IL binary mixture composition on the outcome of the target processes was evidenced. Improvements in both reaction time and temperature have been observed, under US activation.

Francesca DAnna; Salvatore Marullo; Paola Vitale; Carla Rizzo; Paolo Lo Meo; Renato Noto

2014-01-01T23:59:59.000Z

396

BUBBLE CHARACTERISTICS AND CONVECTIVE EFFECTS IN THE FLOW BOILING HEAT TRANSFER OF BINARY MIXTURES  

E-Print Network [OSTI]

BUBBLE CHARACTERISTICS AND CONVECTIVE EFFECTS IN THE FLOW BOILING HEAT TRANSFER OF BINARY MIXTURES on the bubble growth and associated heat transfer phenomena. The present work focuses on obtaining the bubble. The bubble growth is observed using a high speed camera (1000 fps) under a magnification of 290X. The bubble

Kandlikar, Satish

397

Affine Nested Loop Programs and their Binary Parameterized Dataflow Graph Counterparts  

E-Print Network [OSTI]

Affine Nested Loop Programs and their Binary Parameterized Dataflow Graph Counterparts Ed F Parameterized static affine nested loop programs can be automatically converted to input-output equivalent Kahn affine nested loop programs which are nested loop programs in which the loop boundaries, the conditions

Bhattacharyya, Shuvra S.

398

Liquid?Liquid Equilibria for Binary and Ternary Polymer Solutions with PC-SAFT  

Science Journals Connector (OSTI)

Liquid?Liquid Equilibria for Binary and Ternary Polymer Solutions with PC-SAFT ... The algorithms are used for investigating the correlative and predictive capabilities of the thermodynamic model PC-SAFT. ... The algorithms are used for testing of a state-of-the-art model in polymer thermodynamics, PC-SAFT, by Gross and Sadowski. ...

Thomas Lindvig; Michael L. Michelsen; Georgios M. Kontogeorgis

2004-01-21T23:59:59.000Z

399

Content-based Audio Classification using Collective Network of Binary Classifiers  

E-Print Network [OSTI]

Content-based Audio Classification using Collective Network of Binary Classifiers Toni Mäkinen) framework is presented for content-based audio classification. The topic has been studied in several and the number of classes, as well as to create a scalable network design, which allows introducing new audio

Gabbouj, Moncef

400

BOOSTED BINARY AUDIO FINGERPRINT BASED ON SPECTRAL SUBBAND MOMENTS Sungwoong Kim and Chang D. Yoo  

E-Print Network [OSTI]

BOOSTED BINARY AUDIO FINGERPRINT BASED ON SPECTRAL SUBBAND MOMENTS Sungwoong Kim and Chang D. Yoo@kaist.ac.kr, cdyoo@ee.kaist.ac.kr ABSTRACT An audio fingerprinting system identifies an audio based on a unique feature vector called the audio fingerprint. The performance of an audio fingerprinting system is directly

Yoo, Chang D.

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


401

An effectual template bank for the detection of gravitational waves from inspiralling compact binaries with generic spins  

E-Print Network [OSTI]

We report the construction of a three-dimensional template bank for the search for gravitational waves from inspiralling binaries consisting of spinning compact objects. The parameter space consists of two dimensions describing the mass parameters and one "reduced-spin" parameter, which describes the secular (non-precessing) spin effects in the waveform. The template placement is based on an efficient stochastic algorithm and makes use of the semi-analytical computation of a metric in the parameter space. We demonstrate that for "low-mass" ($m_1 + m_2 \\lesssim 12\\,M_\\odot$) binaries, this template bank achieves effective fitting factors $\\sim0.92$--$0.99$ towards signals from generic spinning binaries in the advanced detector era over the entire parameter space of interest (including binary neutron stars, binary black holes, and black hole-neutron star binaries). This provides a powerful and viable method for searching for gravitational waves from generic spinning low-mass compact binaries. Under the assumption that spin magnitudes of black-holes [neutron-stars] are uniformly distributed between 0--0.98 [0 -- 0.4] and spin angles are isotropically distributed, the expected improvement in the average detection volume (at a fixed signal-to-noise-ratio threshold) of a search using this reduced-spin bank is $\\sim20-52\\%$, as compared to a search using a non-spinning bank.

P. Ajith; N. Fotopoulos; S. Privitera; A. Neunzert; N. Mazumder; A. J. Weinstein

2014-05-21T23:59:59.000Z

402

Search for gravitational waves from low mass compact binary coalescence in 186 days of LIGOs fifth science run  

E-Print Network [OSTI]

We report on a search for gravitational waves from coalescing compact binaries, of total mass between 2 and 35M[subscript ?], using LIGO observations between November 14, 2006 and May 18, 2007. No gravitational-wave signals ...

Zucker, Michael E.

403

Search for gravitational waves from compact binary coalescence in LIGO and Virgo data from S5 and VSR1  

E-Print Network [OSTI]

We report the results of the first search for gravitational waves from compact binary coalescence using data from the Laser Interferometer Gravitational-Wave Observatory and Virgo detectors. Five months of data were collected ...

Barsotti, Lisa

404

Fundamental measure density functional theory studies on the freezing of binary hard-sphere and Lennard-Jones mixtures  

E-Print Network [OSTI]

Fundamental measure density functional theory studies on the freezing of binary hard are calculated using the fundamental measure density functional theory. Using the thermodynamic perturbation. INTRODUCTION Density functional theory DFT became a practical the- oretical tool for the calculation

Song, Xueyu

405

Diagnosing the Sensitivity of Binary Image Measures to Bias, Location, and Event Frequency within a Forecast Verification Framework  

Science Journals Connector (OSTI)

While the use of binary distance measures has a substantial history in the field of image processing, these techniques have only recently been applied in the area of forecast verification. Designed to quantify the distance between two images, ...

Benjamin R. J. Schwedler; Michael E. Baldwin

2011-12-01T23:59:59.000Z

406

Orbital-period variations of the close binaries with late-type components TY Del and RY Cnc  

Science Journals Connector (OSTI)

A detailed study of orbital-period variations was performed for TY Del and RY Cnc, which are both Algol-type eclipsing binaries ... with late-type second aries; for RY Cnc, this is the first study of this...? ...

A. I. Khaliullina

2014-08-01T23:59:59.000Z

407

Modeling the high resolution X-ray spectra from the relativistic jets of the X-ray binary SS 433  

E-Print Network [OSTI]

We test the physical model of the relativistic jets in the galactic X-ray binary SS 433 that was proposed by Marshall et al. 2002 (Paper I) using additional observations from the Chandra High Energy Transmission Grating ...

Lopez, Laura Ann, 1982-

2004-01-01T23:59:59.000Z

408

Predicting the High-Pressure Phase Equilibria of Binary Mixtures of n-Alkanes Using the SAFT-VR Approach  

Science Journals Connector (OSTI)

The phase behavior of selected alkane binary mixtures is studied using SAFT-VR, a version of the statistical associating ... theory for potentials of variable attractive range (SAFT). We treat the n-alkane molecu...

C. McCabe; A. Galindo; A. Gil-Villegas

1998-11-01T23:59:59.000Z

409

Diffusion of Binary Non-solvent Mixtures in Polymers: Aqueous Ethanol Solutions in Poly(vinyl acetate)  

Science Journals Connector (OSTI)

The diffusion of binary non-solvent mixtures of ethanol and deuterium oxide (D2O) into poly(vinyl acetate) (PVAc) was studied by FT-IR imaging. Initial diffusion rates...

Rafferty, Denise Wade; Koenig, Jack L

2002-01-01T23:59:59.000Z

410

Light curve solutions of six eclipsing binaries at the lower limit of periods of the W UMa stars  

E-Print Network [OSTI]

Photometric observations in V and I bands of six eclipsing binaries at the lower limit of the orbital periods of W UMa stars are presented. Three of them are newly discovered eclipsing systems. The light curve solutions revealed that all short-period targets were contact or overcontact binaries and added new six binaries to the family of short-period systems with estimated parameters. Four binaries have equal in size components and mass ratio near 1. The phase variability of the V-I colors of all targets may be explained by lower temperatures of their back surfaces than those of their side surfaces. Five systems revealed O'Connell effect that was reproduced by cool spots on the side surfaces of their primary components. The light curves of V1067 Her in 2011 and 2012 were fitted by diametrically opposite spots. The applying of the criteria for subdivision of the W UMa stars to our targets led to ambiguous results.

Kjurkchieva, Diana P; Ibryamov, Sunay I

2015-01-01T23:59:59.000Z

411

Polar Exploration and Coronal Structure in the Active Binary HR 5110  

Science Journals Connector (OSTI)

Overwhelming evidence exists for the importance of polar regions in controlling stellar atmospheric structure and dynamics in active binary systems. Uncertainties about the geometry of coronal emission have made conclusions about coronal structures on such stars ambiguous. We have obtained Chandra VLA and VLBA observations of the nearly pole?on active binary system HR 5110 in order to investigate coronal structures without such ambiguity. The X?ray spectra will constrain thermal coronal volumes through determinaion of electron densities; radio observations will constrain non?thermal coronal volumes directly and allow an estimation of the relative importance of thermal and nonthermal plasma in controlling and structuring active stellar coronae. Here we present preliminary results from the Chandra observations.

David P. Huenemoerder; Rachel A. Osten; Anthony Kesich; Paola Testa; Norbert Schulz

2009-01-01T23:59:59.000Z

412

Basic Parameter Estimation of Binary Neutron Star Systems by the Advanced LIGO/Virgo Network  

E-Print Network [OSTI]

Within the next five years, it is expected that the Advanced LIGO/Virgo network will have reached a sensitivity sufficient to enable the routine detection of gravitational waves. Beyond the initial detection, the scientific promise of these instruments relies on the effectiveness of our physical parameter estimation capabilities. The majority of this effort has been towards the detection and characterization of gravitational waves from compact binary coalescence, e.g. the coalescence of binary neutron stars. While several previous studies have investigated the accuracy of parameter estimation with advanced detectors, the majority have relied on approximation techniques such as the Fisher Matrix. Here we report the statistical uncertainties that will be achievable for optimal detection candidates (SNR = 20) using the full parameter estimation machinery developed by the LIGO/Virgo Collaboration via Markov-Chain Monte Carlo methods. We find the recovery of the individual masses to be fractionally within 9% (15%)...

Rodriguez, Carl L; Raymond, Vivien; Farr, Will M; Littenberg, Tyson; Fazi, Diego; Kalogera, Vicky

2013-01-01T23:59:59.000Z

413

Dissipative dynamics of the Josephson effect in binary Bose-Einstein-condensed mixtures  

SciTech Connect (OSTI)

The dissipative dynamics of a pointlike Josephson junction in binary Bose-Einstein-condensed mixtures is analyzed within the framework of the model of a tunneling Hamiltonian. The transmission of unlike particles across a junction is described by the different transmission amplitudes. The effective action that describes the dynamics of the phase differences across the junction for each of two condensed components is derived by employing the functional integration method. In the low-frequency limit the dynamics of a Josephson junction can be described by two coupled equations in terms of the potential energy and dissipative Rayleigh function using a mechanical analogy. The interplay between mass currents of each mixture component appears in the second-order term in the tunneling amplitudes due to the interspecies hybridizing interaction. The asymmetric case of the binary mixtures with different concentrations and order parameters is considered as well.

Burmistrov, S. N. [Kurchatov Institute, RU-123182 Moscow (Russian Federation)

2011-06-15T23:59:59.000Z

414

Next Generation Geothermal Power Plants (NGGPP) process data for binary cycle plants  

SciTech Connect (OSTI)

The Next Generation Geothermal Power Plants (NGGPP) study provides the firm estimates - in the public domain - of the cost and performance of U.S. geothermal systems and their main components in the early 1990s. The study was funded by the U.S. Department of Energy Geothermal Research Program, managed for DOE by Evan Hughes of the Electric Power Research Institute, Palo Alto, CA, and conducted by John Brugman and others of the CE Holt Consulting Firm, Pasadena, CA. The printed NGGPP reports contain detailed data on the cost and performance for the flash steam cycles that were characterized, but not for the binary cycles. The nine Tables in this document are the detailed data sheets on cost and performance for the air cooled binary systems that were studied in the NGGPP.

Not Available

1996-10-02T23:59:59.000Z

415

MS 1603. 6 + 2600, an unusual X-ray selected binary system at high Galactic latitude  

SciTech Connect (OSTI)

The discovery of an eclipsing binary system at Galactic latitude 47 deg, found as a serendipitous X-ray source in the Einstein Extended Medium Sensitivity Survey, is described. The object has X-ray flux 1.1 x 10 to the -12th ergs/sq cm s (0.3-3.5 keV) and mean magnitude R = 19.4. An orbital period of 111 minutes is found. The problem discussed is whether the system has a white dwarf or neutron star primary, in the end preferring the neutron star primary model. If the system has either optical or X-ray luminosities typical of low mass X-ray binaries (LMXB), it must be at a very large distance (30-80 kpc). Blueshifted He I absorption is seen, indicating cool outflowing material, similar to that seen in the LMXB AC 211 in the globular cluster M15. 29 refs.

Morris, S.L.; Liebert, J.; Stocke, J.T.; Gioia, I.M.; Schild, R.E. (Observatories of the Carnegie Institution, Pasadena, CA (USA) Colorado Univ., Boulder (USA) Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA))

1990-12-01T23:59:59.000Z

416

Calibration of the pre-main sequence RS Cha binary system  

E-Print Network [OSTI]

Context: The calibration of binary systems with accurately known masses and/or radii provides powerful tools to test stellar structure and evolution theory and to determine the age and helium content of stars. We study the eclipsing double-lined spectroscopic binary system RS Cha, for which we have accurate observations of the parameters of both stars (masses, radii, luminosities, effective temperatures and metallicity). Aims: We have calculated several sets of stellar models for the components of the RS Cha system, with the aim of reproducing simultaneously the available observational constraints and to estimate the age and initial helium abundance of the system. Methods: Using the CESAM stellar evolution code, we model both components starting from the initial mass and metallicity and adjusting the input parameters and physics in order to satisfy the observational constraints. Results: We find that the observations cannot be reproduced if we assume that the abundance ratios are solar but they are satisfied ...

Alecian, E; Lebreton, Y; Dupret, M A; Catala, C

2006-01-01T23:59:59.000Z

417

Efficient binary sources of working-body vapor for thermionic converters  

SciTech Connect (OSTI)

The objective of this investigation was an experimental determination of the parameters of a cylindrical thermionic converter (TC), with the binary system being cesium with bismuth, antimony, selenium, and germanium. In all devices, the emitter was a layer of tungsten, and the collector consisted of niobium or an alloy of molybdenum with ruthenium. The system characteristics of each binary system were studied, with the interaction kinetics of the cesium vapor with the active sorbent being examined by the gravimetric method. For each TC, the current-voltage characteristics were investigated as was the work function. For each case investigated, there was a 25-30% higher TC power output due to the presence of the active additive.

Kalandarishvili, A.G.; Kashiya, V.G.

1994-06-01T23:59:59.000Z

418

A binary ACO for controlling all-electric power take off system in wave energy converters  

Science Journals Connector (OSTI)

This paper describes a metaheuristic algorithm for controlling all-electric power take off (PTO) system of wave energy converters. It provides optimal parameter values to the controller following the instantaneously changing sea state. The output of the algorithm is used to tune the electrical control systems in the PTO system in order to provide sufficient time for the point absorber to achieve desired heaving resonance compare with the ocean wave. This maximises the power extraction capability of WECs. The method consists of a binary ant colony optimisation algorithm capable of performing optimisation in continuous space. A binary encoding method is introduced to enhance its search exploration feature, hence allowing it to find optimal solution in short time.

Phen Chiak See; Vin Cent Tai; Marta Molinas

2013-01-01T23:59:59.000Z

419

A BINARY ORBIT FOR THE MASSIVE, EVOLVED STAR HDE 326823, A WR+O SYSTEM PROGENITOR  

SciTech Connect (OSTI)

The hot star HDE 326823 is a candidate transition-phase object that is evolving into a nitrogen-enriched Wolf-Rayet star. It is also a known low-amplitude, photometric variable with a 6.123 day period. We present new, high- and moderate-resolution spectroscopy of HDE 326823, and we show that the absorption lines show coherent Doppler shifts with this period while the emission lines display little or no velocity variation. We interpret the absorption line shifts as the orbital motion of the apparently brighter star in a close, interacting binary. We argue that this star is losing mass to a mass gainer star hidden in a thick accretion torus and to a circumbinary disk that is the source of the emission lines. HDE 326823 probably belongs to a class of objects that produce short-period WR+O binaries.

Richardson, N. D.; Gies, D. R.; Williams, S. J., E-mail: richardson@chara.gsu.edu, E-mail: gies@chara.gsu.edu, E-mail: swilliams@chara.gsu.edu [Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, P.O. Box 4106, Atlanta, GA 30302-4106 (United States)

2011-12-15T23:59:59.000Z

420

Spiral Disk Instability Can Drive Thermonuclear Explosions in Binary White Dwarf Mergers  

E-Print Network [OSTI]

Thermonuclear, or Type Ia supernovae (SNe Ia), originate from the explosion of carbon-oxygen white dwarfs, and serve as standardizable cosmological candles. However, despite their importance, the nature of the progenitor systems which give rise to SNe Ia has not been hitherto elucidated. Observational evidence favors the double-degenerate channel, in which merging white dwarf binaries lead to SNe Ia. Furthermore, significant discrepancies exist between observations and theory, and to date, there has been no self-consistent merger model which yields a SNe Ia. Here we show that a spiral mode instability in the accretion disk formed during a binary white dwarf merger leads to a detonation on a dynamical timescale. This mechanism sheds light on how white dwarf mergers may frequently yield SNe Ia.

Kashyap, Rahul; Garca-Berro, Enrique; Aznar-Sigun, Gabriela; Ji, Suoqing; Lorn-Aguilar, Pablo

2015-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


421

Catalog of 174 Binary Black Hole Simulations for Gravitational Wave Astronomy  

Science Journals Connector (OSTI)

This Letter presents a publicly available catalog of 174 numerical binary black hole simulations following up to 35 orbits. The catalog includes 91 precessing binaries, mass ratios up to 8?1, orbital eccentricities from a few percent to 10-5, black hole spins up to 98% of the theoretical maximum, and radiated energies up to 11.1% of the initial mass. We establish remarkably good agreement with post-Newtonian precession of orbital and spin directions for two new precessing simulations, and we discuss other applications of this catalog. Formidable challenges remain: e.g., precession complicates the connection of numerical and approximate analytical waveforms, and vast regions of the parameter space remain unexplored.

Abdul H. Mrou; Mark A. Scheel; Bla Szilgyi; Harald P. Pfeiffer; Michael Boyle; Daniel A. Hemberger; Lawrence E. Kidder; Geoffrey Lovelace; Serguei Ossokine; Nicholas W. Taylor; An?l Zengino?lu; Luisa T. Buchman; Tony Chu; Evan Foley; Matthew Giesler; Robert Owen; Saul A. Teukolsky

2013-12-11T23:59:59.000Z

422

X-ray views of neutron star low-mass X-ray binaries  

E-Print Network [OSTI]

A neutron star low-mass X-ray binary is a binary stellar system with a neutron star and a low-mass companion star rotating around each other. In this system the neutron star accretes mass from the companion, and as this matter falls into the deep potential well of the neutron star, the gravitational potential energy is released primarily in the X-ray wavelengths. Such a source was first discovered in X-rays in 1962, and this discovery formally gave birth to the "X-ray astronomy". In the subsequent decades, our knowledge of these sources has increased enormously by the observations with several X-ray space missions. Here we give a brief overview of our current understanding of the X-ray observational aspects of these systems.

Sudip Bhattacharyya

2010-02-24T23:59:59.000Z

423

On the Origin of Pluto, Charon, and the Pluto-Charon Binary  

E-Print Network [OSTI]

Being small, binary, and in a highly unusual orbit, Pluto was long viewed as an enigma in the outer Solar System. Here we review the historical development of ideas concerning Pluto's origin and the origin of the Pluto-Charon Binary. We critically examine these theories in light of both recent advances about Pluto, and with regard to Pluto's broader context in the outer Solar System. Although Pluto no longer appears to be the stark anomaly it was in the years before the Kuiper Disk population was discovered, both its large comparative size and the presence of Charon continue to isolate Pluto as a "special" object in the present-day outer solar system. We examine various alternatives concerning how this circumstance came to be. These alternatives fall into two categories: either (i) Pluto was originally not unique, but became so as a result of the general dynamical evolution of the outer solar system, or (ii) Pluto was indeed unique (or nearly so) at the time of the formation epoch, perhaps due to some aspect of its special dynamical niche. These alternatives are discussed in light of both Pluto's cohort population in the Kuiper Disk, and the formation of the Pluto-Charon Binary. We then outline a preliminary paradigm for the origin of Pluto and the Pluto-Charon Binary. This paradigm intimately relates Pluto's origin and dynamical evolution both to Neptune, and to the recently-discovered objects populating the Kuiper Disk. Much work remains to be done to convert this scenario to a complete, quantitative theory, and major questions remain. Foremost among these are how quickly Pluto formed, and when in the sequence of events Charon was formed. The development presented below is constrained by the limited state of knowledge of the Pluto-Charon system, and the scant degree o...

S. Alan Stern; William B. Mckinnon; Jonathan I. Lunine

424

FT-ICR studies of metal-carbon binary clusters for formation mechanism of endohedral fullerene  

E-Print Network [OSTI]

Ion Mass [amu] C60 + Number of Carbon Atoms Intensity(arb.units) LaC44 + LaC50 + LaC60 + Figure 2FT-ICR studies of metal-carbon binary clusters for formation mechanism of endohedral fullerene-wall carbon nanotube), i.e. La, Y, Sc, Gd, Ce, Ca, and Ni-Y. An example of FT-ICR mass spectra is shown

Maruyama, Shigeo

425

Raft River binary-cycle geothermal pilot power plant final report  

SciTech Connect (OSTI)

The design and performance of a 5-MW(e) binary-cycle pilot power plant that used a moderate-temperature hydrothermal resource, with isobutane as a working fluid, are examined. Operating problems experienced and solutions found are discussed and recommendations are made for improvements to future power plant designs. The plant and individual systems are analyzed for design specification versus actual performance figures.

Bliem, C.J.; Walrath, L.F.

1983-04-01T23:59:59.000Z

426

An Optimal Parallel Algorithm for the Euclidean Distance Maps of Binary Images  

E-Print Network [OSTI]

black pixel. The EDM plays an important role in machine vision, pat­ tern recognition and robotics. Many@is.aist­nara.ac.jp 1 Introduction The Euclidean distance map (EDM) of a black and white n 2 n binary image is the n 2 n algorithms have been proposed for computing the EDM. In recent years, O(n 2 ) time sequential algo­ rithms

Fujiwara, Akihiro

427

Hydrogen deficient donors in low-mass X-ray binaries  

E-Print Network [OSTI]

A number of X-ray binaries (neutron stars or black holes accreting from a companion star) have such short orbital periods that ordinary, hydrogen rich, stars do not fit in. Instead the mass-losing star must be a compact, evolved star, leading to the transfer of hydrogen deficient material to the neutron star. I discuss the current knowledge of these objects, with focus on optical spectroscopy.

Gijs Nelemans

2007-11-05T23:59:59.000Z

428

THE RADIUS DISCREPANCY IN LOW-MASS STARS: SINGLE VERSUS BINARIES  

SciTech Connect (OSTI)

A long-standing issue in the theory of low-mass stars is the discrepancy between predicted and observed radii and effective temperatures. In spite of the increasing availability of very precise radius determinations from eclipsing binaries and interferometric measurements of radii of single stars, there is no unanimous consensus on the extent (or even the existence) of the discrepancy and on its connection with other stellar properties (e.g., metallicity, magnetic activity). We investigate the radius discrepancy phenomenon using the best data currently available (accuracy ?< 5%). We have constructed a grid of stellar models covering the entire range of low-mass stars (0.1-1.25 M{sub ?}) and various choices of the metallicity and mixing length parameter, ?. We used an improved version of the Yale Rotational stellar Evolution Code, implementing surface boundary conditions based on the most up-to-date PHOENIX atmosphere models. Our models are in good agreement with others in the literature and improve and extend the low mass end of the Yale-Yonsei isochrones. Our calculations include rotation-related quantities, such as moments of inertia and convective turnover timescales, useful in studies of magnetic activity and rotational evolution of solar-like stars. Consistent with previous works, we find that both binaries and single stars have radii inflated by about 3% with respect to the theoretical models; among binaries, the components of short orbital period systems are found to be the most deviant. We conclude that both binaries and single stars are comparably affected by the radius discrepancy phenomenon.

Spada, F. [Leibniz-Institut fr Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482, Potsdam (Germany); Demarque, P. [Department of Astronomy, Yale University, New Haven, CT 06520-8101 (United States); Kim, Y.-C. [Yonsei University Observatory and Astronomy Department, Yonsei University, Seoul 120-749 (Korea, Republic of); Sills, A., E-mail: fspada@aip.de [Department of Physics and Astronomy, McMaster University, Hamilton, ON, L8S 4M1 (Canada)

2013-10-20T23:59:59.000Z

429

Ultraluminous X-ray Sources: The most extreme X-ray binaries  

E-Print Network [OSTI]

1 Ultraluminous X-ray Sources: The most extreme X-ray binaries Luca Zampieri INAF ULXs ­ Lubiana ­ May 11, 2012- LZ #12;6 · X-ray observations of nearby galaxies show a population of pointlike, off-nuclear sources with L >> Ledd for 1 Msun (L>1.0e39 erg/s) UltraLuminous X-ray Sources (e

?umer, Slobodan

430

Aluto-Langano Geotermal Power Plant | Open Energy Information  

Open Energy Info (EERE)

System - Ethiopian Rift Valley Plant Information Facility Type Binary Cycle Power Plant, ORC Owner Ethiopian Electric Power Corporation Developer Ethiopian Electric Power...

431

The gravitational-wave signal generated by a galactic population of double neutron-star binaries  

E-Print Network [OSTI]

We investigate the gravitational wave (GW) signal generated by a population of double neutron-star binaries (DNS) with eccentric orbits caused by kicks during supernova collapse and binary evolution. The DNS population of a standard Milky-Way type galaxy has been studied as a function of star formation history, initial mass function (IMF) and metallicity and of the binary-star common-envelope ejection process. The model provides birth rates, merger rates and total numbers of DNS as a function of time. The GW signal produced by this population has been computed and expressed in terms of a hypothetical space GW detector (eLISA) by calculating the number of discrete GW signals at different confidence levels, where `signal' refers to detectable GW strain in a given frequency-resolution element. In terms of the parameter space explored, the number of DNS-originating GW signals is greatest in regions of recent star formation, and is significantly increased if metallicity is reduced from 0.02 to 0.001, consistent wi...

Yu, Shenghua

2015-01-01T23:59:59.000Z

432

The separation of the stars in the binary nucleus of the planetary nebula Abell 35  

E-Print Network [OSTI]

Using the Planetary Camera on board the Hubble Space Telescope we have measured the projected separation of the binary components in the nucleus of the planetary nebula Abell 35 to be larger than 0.08 arcsecs but less than 0.14 arcsecs. The system was imaged in three filters centered at 2950, 3350 and 5785 Ang. The white dwarf primary star responsible for ionizing the nebula is half as bright as its companion in the 2950 Ang filter causing the source to be visibly elongated. The 3350 Ang setting, on the other hand, shows no elongation as a result of the more extreme flux ratio. The F300W data allows the determinination of the binary's projected separation. At the minimum distance of 160 parsec to the system, our result corresponds to 18+/-5 AU. This outcome is consistent with the wind accretion induced rapid rotation hypothesis, but cannot be reconciled with the binary having emerged from a common-envelope phase.

A. A. Gatti; J. E. Drew; R. D. Oudmaijer; T. R. Marsh; A. E. Lynas-Gray

1998-09-25T23:59:59.000Z

433

The Discovery of a Short Period Double-Degenerate Binary Star  

E-Print Network [OSTI]

We have found that the white dwarf PG 1101+364 is a double-lined white dwarf/white dwarf binary with an orbital period of 3.47 hours. PG 1101+364 is the shortest period detached double-degenerate yet found and gravitational radiation will cause it to merge in 2.5 X 10**9 years. PG 1101+364 has a mass ratio of 0.87 +/- 0.03. From the relative strengths of the narrow core of Halpha, the lighter and therefore larger star appears to contribute more of the light by an amount that indicates almost equal temperatures for the two stars. We chose to observe PG 1101+364 on the basis of its low spectroscopic mass (0.31 Msun), and the discovery of its binary nature confirms the belief that binary evolution is required to produce such low mass white dwarfs. The radial velocity semi-amplitudes (69.7 +/- 1.7 km/s and 80.3 +/- 1.6 km/s) and the spectroscopic mass show that we see the orbit of PG 1101+364 at a low inclination of ~ 25 deg.

T. R. Marsh

1995-04-25T23:59:59.000Z

434

Colliding Winds in Low-Mass Binary Star Systems: wind interactions and implications for habitable planets  

E-Print Network [OSTI]

Context. In binary star systems, the winds from the two components impact each other, leading to strong shocks and regions of enhanced density and temperature. Potentially habitable circumbinary planets must continually be exposed to these interactions regions. Aims. We study, for the first time, the interactions between winds from low-mass stars in a binary system, to show the wind conditions seen by potentially habitable circumbinary planets. Methods. We use the advanced 3D numerical hydrodynamic code Nurgush to model the wind interactions of two identical winds from two solar mass stars with circular orbits and a binary separation of 0.5 AU. As input into this model, we use a 1D hydrodynamic simulation of the solar wind, run using the Versatile Advection Code. We derive the locations of stable and habitable orbits in this system to explore what wind conditions potentially habitable planets will be exposed to during their orbits. Results. Our wind interaction simulations result in the formation of two stron...

Johnstone, C P; Pilat-Lohinger, E; Bisikalo, D; Gdel, M; Eggl, S

2015-01-01T23:59:59.000Z

435

What Can Simbol-X Do for Gamma-ray Binaries?  

SciTech Connect (OSTI)

Gamma-ray binaries have been uncovered as a new class of Galactic objects in the very high energy sky (>100 GeV). The three systems known today have hard X-ray spectra (photon index {approx}1.5), extended radio emission and a high luminosity in gamma-rays. Recent monitoring campaigns of LSI +61 deg. 303 in X-rays have confirmed variability in these systems and revealed a spectral hardening with increasing flux. In a generic one-zone leptonic model, the cooling of relativistic electrons accounts for the main spectral and temporal features observed at high energy. Persistent hard X-ray emission is expected to extend well beyond 10 keV. We explain how Simbol-X will constrain the existing models in connection with Fermi Space Telescope measurements. Because of its unprecedented sensitivity in hard X-rays, Simbol-X will also play a role in the discovery of new gamma-ray binaries, giving new insights into the evolution of compact binaries.

Cerutti, B.; Dubus, G.; Henri, G.; Hill, A. B. [Laboratoire d'Astrophysique de Grenoble, UMR 5571 CNRS, Universite Joseph Fourier, BP 53, 38041 Grenoble (France); Szostek, A. [Laboratoire d'Astrophysique de Grenoble, UMR 5571 CNRS, Universite Joseph Fourier, BP 53, 38041 Grenoble (France); Astronomical Observatory, Jagiellonian University, Orla 171, 30-244 Krakow (Poland)

2009-05-11T23:59:59.000Z

436

Compact binary systems in scalar-tensor gravity. III. Scalar waves and energy flux  

E-Print Network [OSTI]

We derive the scalar waveform generated by a binary of nonspinning compact objects (black holes or neutron stars) in a general class of scalar-tensor theories of gravity. The waveform is accurate to 1.5 post-Newtonian order [$O((v/c)^3)$] beyond the leading order tensor gravitational waves (the "Newtonian quadrupole"). To solve the scalar-tensor field equations, we adapt the direct integration of the relaxed Einstein equations formalism developed by Will, Wiseman, and Pati. The internal gravity of the compact objects is treated with an approach developed by Eardley. We find that the scalar waves are described by the same small set of parameters which describe the equations of motion and tensor waves. For black hole-black hole binaries, the scalar waveform vanishes, as expected from previous results which show that these systems in scalar-tensor theory are indistinguishable from their general relativistic counterparts. For black hole-neutron star binaries, the scalar waveform simplifies considerably from the g...

Lang, Ryan N

2014-01-01T23:59:59.000Z

437

Temperature dependence of binary and ternary recombination of D{sub 3}{sup +} ions with electrons  

SciTech Connect (OSTI)

Flowing and stationary afterglow experiments were performed to study the recombination of D{sub 3}{sup +} ions with electrons at temperatures from 77 to 300 K. A linear dependence of apparent (effective) binary recombination rate coefficients on the pressure of the helium buffer gas was observed. Binary (D{sub 3}{sup +}+e{sup -}) and ternary (D{sub 3}{sup +}+e{sup -}+He) recombination rate coefficients were derived. The obtained binary rate coefficient agrees with recent theoretical values for dissociative recombination of D{sub 3}{sup +}. We describe the observed ternary process by a mechanism with two rate determining steps. In the first step, a rotationally excited long-lived neutral D{sub 3}* is formed in D{sub 3}{sup +}-e{sup -} collisions. As the second step, the D{sub 3}* collides with a helium atom that prevents autoionization of D{sub 3}*. We calculate lifetimes of D{sub 3}* formed from ortho-, para-, or metastates of D{sub 3}{sup +} and use the lifetimes to calculate ternary recombination rate coefficients.

Kotrik, T.; Dohnal, P.; Korolov, I.; Plasil, R.; Roucka, S.; Glosik, J. [Faculty of Mathematics and Physics, Charles University, 12116 Prague (Czech Republic); Greene, Chris H. [Department of Physics and JILA, University of Colorado, Boulder, Colorado 80309-0440 (United States); Kokoouline, V. [Department of Physics, University of Central Florida, Orlando, Florida 32816 (United States); Laboratoire Aime Cotton, CNRS, Universite Paris-Sud XI, 91405 Orsay (France)

2010-07-21T23:59:59.000Z

438

Short Gamma-Ray Bursts and Gravitational Waves from Dynamically Formed Merging Binaries  

E-Print Network [OSTI]

Merging binary systems consisting of two collapsed objects are among the most promising sources of high frequency gravitational wave, GW, signals for ground based interferometers. Double neutron star or black hole/neutron star mergers are also believed to give rise to short hard bursts, SHBs, a subclass of gamma ray bursts. SHBs might thus provide a powerful way to infer the merger rate of two-collapsed object binaries. Under the hypothesis that most SHBs originate from double neutron star or black hole/neutron star mergers, we outline here a method to estimate the incidence of merging events from dynamically formed binaries in globular clusters and infer the corresponding GW event rate that can be detected with Advanced LIGO/Virgo. In particular a sizeable fraction of detectable GW events is expected to be coincident with SHBs. The beaming and redshift distribution of SHBs are reassessed and their luminosity function constrained by using the results from recent SHBs observations. We confirm that a substantial fraction of SHBs goes off at low redshifts, where the merging of systems formed in globular clusters through dynamical interactions is expected.

Dafne Guetta; Luigi Stella

2008-11-10T23:59:59.000Z

439

KOI-54: The Kepler Discovery of Tidally Excited Pulsations and Brightenings in a Highly Eccentric Binary  

Science Journals Connector (OSTI)

Kepler observations of the star HD 187091 (KIC 8112039, hereafter KOI-54) revealed a remarkable light curve exhibiting sharp periodic brightening events every 41.8 days with a superimposed set of oscillations forming a beating pattern in phase with the brightenings. Spectroscopic observations revealed that this is a binary star with a highly eccentric orbit, e = 0.83. We are able to match the Kepler light curve and radial velocities with a nearly face-on (i = 55) binary star model in which the brightening events are caused by tidal distortion and irradiation of nearly identical A stars during their close periastron passage. The two dominant oscillations in the light curve, responsible for the beating pattern, have frequencies that are the 91st and 90th harmonic of the orbital frequency. The power spectrum of the light curve, after removing the binary star brightening component, reveals a large number of pulsations, 30 of which have a signal-to-noise ratio 7. Nearly all of these pulsations have frequencies that are either integer multiples of the orbital frequency or are tidally split multiples of the orbital frequency. This pattern of frequencies unambiguously establishes the pulsations as resonances between the dynamic tides at periastron and the free oscillation modes of one or both of the stars. KOI-54 is only the fourth star to show such a phenomenon and is by far the richest in terms of excited modes.

William F. Welsh; Jerome A. Orosz; Conny Aerts; Timothy M. Brown; Erik Brugamyer; William D. Cochran; Ronald L. Gilliland; Joyce Ann Guzik; D. W. Kurtz; David W. Latham; Geoffrey W. Marcy; Samuel N. Quinn; Wolfgang Zima; Christopher Allen; Natalie M. Batalha; Steve Bryson; Lars A. Buchhave; Douglas A. Caldwell; Thomas N. Gautier III; Steve B. Howell; K. Kinemuchi; Khadeejah A. Ibrahim; Howard Isaacson; Jon M. Jenkins; Andrej Prsa; Martin Still; Rachel Street; Bill Wohler; David G. Koch; William J. Borucki

2011-01-01T23:59:59.000Z

440

Energy Dissipation through Quasi-Static Tides in White Dwarf Binaries  

E-Print Network [OSTI]

We study tidal interactions in white dwarf binaries in the limiting case of quasi-static tides. The formalism is valid for arbitrary orbital eccentricities and therefore applicable to white dwarf binaries in the Galactic disk as well as globular clusters. In the quasi-static limit, the total perturbation of the gravitational potential shows a phase shift with respect to the position of the companion, the magnitude of which is determined primarily by the efficiency of energy dissipation through convective damping. We determine rates of secular evolution of the orbital elements and white dwarf rotational angular velocity for a 0.3 solar mass helium white dwarf in binaries with orbital frequencies in the LISA gravitational wave frequency band and companion masses ranging from 0.3 to 10^5 solar masses. The resulting tidal evolution time scales for the orbital semi-major axis are longer than a Hubble time, so that convective damping of quasi-static tides need not be considered in the construction of gravitational ...

Willems, B; Kalogera, V

2009-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


441

Short GRB and binary black hole standard sirens as a probe of dark energy  

SciTech Connect (OSTI)

Observations of the gravitational radiation from well-localized, inspiraling compact-object binaries can measure absolute source distances with high accuracy. When coupled with an independent determination of redshift through an electromagnetic counterpart, these standard sirens can provide an excellent probe of the expansion history of the Universe and the dark energy. Short {gamma}-ray bursts, if produced by merging neutron star binaries, would be standard sirens with known redshifts detectable by ground-based gravitational wave (GW) networks such as Advanced Laser Interferometer Gravitational-wave Observatory (LIGO), Virgo, and Australian International Gravitational Observatory (AIGO). Depending upon the collimation of these GRBs, the measurement of about 10 GW-GRB events (corresponding to about 1 yr of observation with an advanced GW detector network and an all-sky GRB monitor) can measure the Hubble constant h to {approx}2-3%. When combined with measurement of the absolute distance to the last scattering surface of the cosmic microwave background, this determines the dark energy equation of state parameter w to {approx}9%. Similarly, supermassive binary black hole inspirals will be standard sirens detectable by Laser Interferometer Space Antenna (LISA). Depending upon the precise redshift distribution, {approx}100 sources could measure w at the {approx}4% level.

Dalal, Neal [CITA, University of Toronto, 60 St. George St., Toronto, ON, M5S 3H8 (Canada); Holz, Daniel E. [Theoretical Division, Los Alamos National Laboratory, Los Alamos, New Mexico 87545 (United States); Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637 (United States); Hughes, Scott A. [Dept. of Physics and MIT Kavli Institute, 77 Massachusetts Avenue, Cambridge, Massachusetts 02139 (United States); Jain, Bhuvnesh [Dept. of Physics and Astronomy, University of Pennsylvania, Philadelphia, Pennsylvania 19104 (United States)

2006-09-15T23:59:59.000Z

442

Ejection of hypervelocity stars by the (binary) black hole(s) in the Galactic center  

E-Print Network [OSTI]

We study three processes that eject hypervelocity (>10^3 km/s) stars from the Galactic center: (i) close encounters of two single stars; (ii) tidal breakup of binary stars by the central black hole, as originally proposed by Hills; and (iii) three-body interactions between a star and a binary black hole (BBH). Mechanism (i) expels hypervelocity stars to the solar radius at a negligible rate, ~10^{-11}/yr. Mechanism (ii) expels hypervelocity stars at a rate ~ 10^{-5}(\\eta/0.1)/yr, where \\eta is the fraction of stars in binaries with semimajor axis a_b<~0.3 AU. For solar-mass stars, the corresponding number of hypervelocity stars within the solar radius R_0=8 kpc is ~60(\\eta/0.1)(a_b/0.1 AU)^{1/2}. For mechanism (iii), Sgr A^* is assumed to be one component of a BBH. We constrain the allowed parameter space (semimajor axis, mass ratio) of the BBH. In the allowed region (for example, semimajor axis of 0.5x10^{-3} pc and mass ratio of 0.01), the rate of ejecting hypervelocity stars can be as large as ~10^{-4}/yr and the expected number of hypervelocity stars within the solar radius can be as large as ~10^3. Hypervelocity stars may be detectable by the next generation of large-scale optical surveys.

Qingjuan Yu; Scott Tremaine

2003-09-03T23:59:59.000Z

443

Accretion disks around binary black holes of unequal mass: GRMHD simulations near decoupling  

E-Print Network [OSTI]

We report on simulations in general relativity of magnetized disks onto black hole binaries. We vary the binary mass ratio from 1:1 to 1:10 and evolve the systems when they orbit near the binary-disk decoupling radius. We compare (surface) density profiles, accretion rates (relative to a single, non-spinning black hole), variability, effective $\\alpha$-stress levels and luminosities as functions of the mass ratio. We treat the disks in two limiting regimes: rapid radiative cooling and no radiative cooling. The magnetic field lines clearly reveal jets emerging from both black hole horizons and merging into one common jet at large distances. The magnetic fields give rise to much stronger shock heating than the pure hydrodynamic flows, completely alter the disk structure, and boost accretion rates and luminosities. Accretion streams near the horizons are among the densest structures; in fact, the 1:10 no-cooling evolution results in a refilling of the cavity. The typical effective temperature in the bulk of the disk is $\\sim 10^5 (M/10^8 M_\\odot)^{-1/4} (L/L_{\\rm edd})^{1/4} {\\rm K}$ yielding characteristic thermal frequencies $\\sim 10^{15} (M/10^8 M_\\odot)^{-1/4} (L/L_{\\rm edd})^{1/4}(1+z)^{-1}{\\rm Hz} $. These systems are thus promising targets for many extragalactic optical surveys, such as LSST, WFIRST, and PanSTARRS.

Roman Gold; Vasileios Paschalidis; Zachariah B. Etienne; Stuart L. Shapiro; Harald P. Pfeiffer

2013-12-02T23:59:59.000Z

444

Clustering in rapid granular flows of binary and continuous particle size distributions  

Science Journals Connector (OSTI)

The dynamic clustering phenomenon in two-dimensional simple shear flows has been investigated using molecular dynamic simulations of systems containing binary and continuous size distributions of equal-material-density particles. Particular attention has been paid to two questions: (1) Does the presence of size nonuniformities serve to enhance or attenuate the presence of clusters? (2) Do particles of a given size preferentially segregate within the clusters? With respect to the first question, the prominence of clustered regions increases with increasing deviation from the monodisperse limit in the case of both binary and continuous size distributions. With respect to the second question, the larger particles of both binary and continuous size distributions are consistently observed to segregate within the transient clustered regions. Further investigation of granular temperatures within the clustered and dilute regions reveals that this segregation is consistent with previously observed temperature-driven segregation in steady-state systems; large particles favor the lower-temperature (clustered) regions. Moreover, observation of clustering length scales suggests that large particles may favor the center of the clustered regions, where granular temperatures are expected to reach a minimum.

R. Brent Rice and Christine M. Hrenya

2010-02-08T23:59:59.000Z

445

Impact of precession on aligned-spin searches for neutron-star--black-hole binaries  

E-Print Network [OSTI]

The inclusion of aligned-spin effects in gravitational-wave search pipelines for neutron-star--black-hole binary coalescence has been shown to increase the astrophysical reach with respect to search methods where spins are neglected completely, under astrophysically reasonable assumptions about black-hole spins. However, theoretical considerations and population synthesis models suggest that many of these binaries may have a significant misalignment between the black-hole spin and the orbital angular momentum, which could lead to precession of the orbital plane during the inspiral and a consequent loss in detection efficiency if precession is ignored. This work explores the effect of spin misalignment on a search pipeline that completely neglects spin effects and on a recently-developed pipeline that only includes aligned-spin effects. Using synthetic but realistic data, which could reasonably represent the first scientific runs of advanced-LIGO detectors, the relative sensitivities of both pipelines are shown for different assumptions about black-hole spin magnitude and alignment with the orbital angular momentum. Despite the inclusion of aligned-spin effects, the loss in signal-to-noise ratio due to precession can be as large as $40\\%$, but this has a limited impact on the overall detection rate: even if precession is a predominant feature of neutron-star--black-hole binaries, an aligned-spin search pipeline can still detect at least half of the signals compared to an idealized generic precessing search pipeline.

Tito Dal Canton; Andrew P. Lundgren; Alex B. Nielsen

2014-11-25T23:59:59.000Z

446

DETERMINATION OF ORBITAL ELEMENTS OF SPECTROSCOPIC BINARIES USING HIGH-DISPERSION SPECTROSCOPY  

SciTech Connect (OSTI)

Orbital elements of 37 single-lined spectroscopic binary systems (SB1s) and 5 double-lined spectroscopic binary systems (SB2s) were determined using high-dispersion spectroscopy. To determine the orbital elements accurately, we carried out precise Doppler shift measurements using the HIgh Dispersion Echelle Spectrograph mounted on the Okayama Astrophysical Observatory 1.88 m telescope. We achieved a radial-velocity precision of {approx}10 m s{sup -1} over seven years of observations. The targeted binaries have spectral types between F5 and K3, and are brighter than the 7th magnitude in the V band. The orbital elements of 28 SB1s and 5 SB2s were determined at least 10 times more precisely than previous measurements. Among the remaining nine SB1s, five objects were found to be single stars, and the orbital elements of four objects were not determined because our observations did not cover the entire orbital period. We checked the absorption lines from the secondary star for 28 SB1s and found that three objects were in fact SB2s.

Katoh, Noriyuki [Graduate School of Science, Kobe University, 1-1 Rokkoudai, Nada-ku, Kobe, Hyogo 657-8501 (Japan); Itoh, Yoichi [Nishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo, Sayo, Hyogo 679-5313 (Japan); Toyota, Eri [Kobe Science Museum, 7-7-6 Minatojimanakacho, Chou-ku, Kobe, Hyogo 650-0046 (Japan); Sato, Bun'ei [Tokyo Institute of Technology, 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551 (Japan)

2013-02-01T23:59:59.000Z

447

Screened thermonuclear reactions and predictive stellar evolution of detached double-lined eclipsing binaries  

E-Print Network [OSTI]

The low energy fusion cross sections of charged-particle nuclear reactions (and the respective reaction rates) in stellar plasmas are enhanced due to plasma screening effects. We study the impact of those effects on predictive stellar evolution simulations for detached double-lined eclipsing binaries. We follow the evolution of binary systems (pre-main sequence or main sequence stars) with precisely determined radii and masses from 1.1Mo to 23Mo (from their birth until their present state). The results indicate that all the discrepancies between the screened and unscreened models (in terms of luminosity, stellar radius, and effective temperature) are within the observational uncertainties. Moreover, no nucleosynthetic or compositional variation was found due to screening corrections. Therefore all thermonuclear screening effects on the charged-particle nuclear reactions that occur in the binary stars considered in this work (from their birth until their present state) can be totally disregarded. In other words, all relevant charged-particle nuclear reactions can be safely assumed to take place in a vacuum, thus simplifying and accelerating the simulation processes.

Theodore Liolios; Theocharis Kosmas

2005-07-06T23:59:59.000Z

448

Proper motions of new dust in the colliding-wind binary WR 140  

E-Print Network [OSTI]

The eccentric WR+O binary system WR 140 produces dust for a few months at intervals of 7.94 yrs coincident with periastron passage. We present the first resolved images of this dust shell, at binary phases ~0.039 and ~0.055, using aperture masking techniques on the Keck-I telescope to achieve diffraction-limited resolution. Proper motions of approximately 1.1 milliarcsecond per day were detected, implying a distance ~1.5 kpc from the known wind speed. The dust plume observed is not as simple as the ``pinwheel'' nebulae seen around other WR colliding wind binaries, indicating the orbital plane is highly inclined to our line-of-sight and/or the dust formation is very clumpy. Follow-up imaging in the mid-infrared and with adaptive optics is urgently required to track the dust motion further, necessary for unambiguously determining the orbital geometry which we only partially constrain here. With full knowledge of the orbital elements, these infrared images can be used to reconstruct the dust distribution along t...

Monnier, J D; Danchi, W C

2002-01-01T23:59:59.000Z

449

Proper motions of new dust in the colliding-wind binary WR 140  

E-Print Network [OSTI]

The eccentric WR+O binary system WR 140 produces dust for a few months at intervals of 7.94 yrs coincident with periastron passage. We present the first resolved images of this dust shell, at binary phases ~0.039 and ~0.055, using aperture masking techniques on the Keck-I telescope to achieve diffraction-limited resolution. Proper motions of approximately 1.1 milliarcsecond per day were detected, implying a distance ~1.5 kpc from the known wind speed. The dust plume observed is not as simple as the ``pinwheel'' nebulae seen around other WR colliding wind binaries, indicating the orbital plane is highly inclined to our line-of-sight and/or the dust formation is very clumpy. Follow-up imaging in the mid-infrared and with adaptive optics is urgently required to track the dust motion further, necessary for unambiguously determining the orbital geometry which we only partially constrain here. With full knowledge of the orbital elements, these infrared images can be used to reconstruct the dust distribution along the colliding wind interface, providing a unique tool for probing the post-shock physical conditions of violent astrophysical flows.

J. D. Monnier; P. G. Tuthill; W. C. Danchi

2002-02-16T23:59:59.000Z

450

Binary orbits as the driver of gamma-ray emission and mass ejection in classical novae  

E-Print Network [OSTI]

Classical novae are the most common astrophysical thermonuclear explosions, occurring on the surfaces of white dwarf stars accreting gas from companions in binary star systems. Novae typically expel ~10^(-4) solar masses of material at velocities exceeding 1,000 kilometres per second. However, the mechanism of mass ejection in novae is poorly understood, and could be dominated by the impulsive flash of thermonuclear energy, prolonged optically thick winds, or binary interaction with the nova envelope. Classical novae are now routinely detected in gigaelectronvolt gamma-ray wavelengths, suggesting that relativistic particles are accelerated by strong shocks in the ejecta. Here we report high-resolution radio imaging of the gamma-ray-emitting nova V959 Mon. We find that its ejecta were shaped by the motion of the binary system: some gas was expelled rapidly along the poles as a wind from the white dwarf, while denser material drifted out along the equatorial plane, propelled by orbital motion. At the interface ...

Chomiuk, Laura; Yang, Jun; O'Brien, T J; Paragi, Zsolt; Mioduszewski, Amy J; Beswick, R J; Cheung, C C; Mukai, Koji; Nelson, Thomas; Ribeiro, Valerio A R M; Rupen, Michael P; Sokoloski, J L; Weston, Jennifer; Zheng, Yong; Bode, Michael F; Eyres, Stewart; Roy, Nirupam; Taylor, Gregory B

2014-01-01T23:59:59.000Z

451

Gamma-rays and neutrinos from dense environment of massive binary systems in open clusters  

E-Print Network [OSTI]

TeV gamma-ray emission has been recently observed from direction of a few open clusters containing massive stars. We consider the high energy processes occurring within massive binary systems and in their dense environment by assuming that nuclei, from the stellar winds of massive stars, are accelerated at the collision region of the stellar winds. We calculate the rates of injection of protons and neutrons from fragmentation of these nuclei in collisions with stellar radiation and matter of the winds from the massive companions in binary system. Protons and neutrons can interact with the matter, within the stellar wind cavity and within the open cluster, producing pions which decay into $\\gamma$-rays and neutrinos. We discuss the detectability of such $\\gamma$-ray emission by the present and future Cherenkov telescopes for the case of two binary systems Eta Carinae, within the Carina Nebula, and WR 20a, within the Westerlund 2 open cluster. We also calculate the neutrino fluxes produced by protons around the...

Bednarek, W; Sobczak, T

2014-01-01T23:59:59.000Z

452

DOE Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

transition) transition) 6/15/1999 6/30/2011 2 three month option periods 9/30/2011 M&O 1999 http://www.id.energy.gov/PSD/AMWTPHomepage.html Mike Adams 208-526-5277 Wendy Bauer 208-526-2808 Paducah Remediation EM LATA Environmental Services of Kentucky 4/22/2010 7/21/2015 7/21/2015 Site Clean up 2009 http://www.emcbc.doe.gov/dept/contracting/primecontracts.php Pam Thompson 859-219-4056 Bill Creech 859-219-4044 Argonne National Laboratory SC UChicago Argonne, LLC 7/31/2006 9/30/2015 4 yrs Award Term Earned/additional 11 yrs Award Term Available 9/30/2026 M&O 2006 http://www.anl.gov/contract/ Patricia Schuneman 630-252-2956 Sergio Martinez 630-252-2075 Kristin Palmer 630-252-2127 Oak Ridge Environmental Management

453

DOE Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

UChicago Argonne, LLC UChicago Argonne, LLC 7/31/2006 9/30/2011 4 yrs Award Term Earned/additional 11 yrs Award Term Available 9/30/2026 M&O 2006 http://www.anl.gov/contract/ Patricia Schuneman 630-252-2956 Sergio Martinez 630-252-2075 Kristin Palmer 630-252-2127 Oak Ridge Environmental Management EM Bechtel Jacobs Co LLC 12/18/1997 12/31/2011 12/31/2011 Environmental Mgmt 1998 http://www.oakridge.doe.gov/external/Home/Procurement/RecentAwards/tabid/101/De fault.aspx Barbara Jackson 865-576-0976 Karen Shears 865-241-6411 Ames National Laboratory SC Iowa State University 12/4/2006 12/31/2011 4yrs Award Term Earned/additional 11 yrs Award Term Available 12/31/2026 M&O 2007 http://www.ameslab.gov/operations/resources/contract Patricia Schuneman

454

DOE Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

Univ. Of Chicago Argonne Univ. Of Chicago Argonne LLC 7/31/2006 9/30/2011 4 yrs Award Term Earned/additional 11 yrs Award Term Available 9/30/2026 M&O 2006 http://www.anl.gov/contract/ Patricia Schuneman 630-252-2956 Sergio Martinez 630-252-2075 Kristin Palmer 630-252-2127 Oak Ridge Environmental Management EM Bechtel Jacobs Co LLC 12/18/1997 12/31/2011 12/31/2011 Environmental Mgmt 1998 http://www.oakridge.doe.gov/external/Home/Procurement/RecentAwards/tabid/101/De fault.aspx Barbara Jackson 865-576-0976 Karen Shears 865-241-6411 Ames National Laboratory SC Iowa State University 12/4/2006 12/31/2011 4yrs Award Term Earned/additional 11yrs Award Term Available 12/31/2026 M&O 2007 http://www.ameslab.gov/operations/resources/contract Patricia Schuneman

455

Certification of Timesharing LOGON ID Owner Responsibilities  

Broader source: Energy.gov (indexed) [DOE]

FORM AD-798 FORM AD-798 (3-78) Section 1 - Section 2 - Section 3 - Section 4 - Section 5 - Hi - 3 Dates (Include all Within-Grade Increases) (Begin with most recent date in Card 20) Service Periods For Which Retirement Deductions Were Withdrawn (Begin with old- est period in Card 30) Service Periods For Which Retirement Deductions Were Not Withheld (Begin with old- est period in Card 40) Periods of Separation Prior to 10/1/56 (Begin with most recent date in Card 50) Request Number 1 45 49 50 20 30 40 50 / / / / / / / / / / / / / / / / / / / / / / / / 21 31 41 51 / / / / / / / / / / / / / / / / 22 32 42 52 / / / / / / / / / / / / / / / / 23 33 43 53 / / / / / / / / / / / / / / / / 24 34 44 54 / / / / / / / / / / / / / / / / 25 35 45 55 / / / / / / / / / / / / / / / / 26 36 46 56 / / / / / / / / / / / / / / / / 27 37 47 57 / / / / / / / / / / / / / / / / 28 38 48 58 / / / / / / / / / / / / / / / / 29 39 49 59 / / / / / / / / / / / / / / / / 11 11 11 11 12 12 12 12 13 13 13 13 18 18 18 18 19 19 19 19 24 24 24 24 25 25 25 29 29 29 30 30 30 32 32 32 33 33 33 35 35 35 52 53 58 59 62 63 68 69 70 75

456

DOE Facility Management Contracts Facility Owner Contractor  

Broader source: Energy.gov (indexed) [DOE]

Ultimate Potential Ultimate Potential Expiration Date Contract FY Competed Parent Companies INEEL (AMWTP Ops) EM Bechtel BWXT Idaho LLC (Under Protest) 6/15/1999 3/31/2011 2 three month option periods until protest resolved 9/30/2011 M&O 1999 Bechtel National, Inc. (67%) and Babcock and Wilcox Company (33%) Portsmouth Remediation EM LATA/Parallax 1/10/2005 6/30/2010 2/28/2011 Site Clean up 2005 Los Alamos Technical Associates (LATA) 51%; Parallax (name changed to ES Performance Plus) 49% Paducah Remediation EM LATA Environmental Services of Kentucky 4/22/2010 7/21/2015 7/21/2015 Site Clean up 2009 Los Alamos Technical Associates, Inc. 100% West Valley Demonstration Project EM West Valley Environmental Svcs 6/29/2007 6/30/2011 6/30/2011 Site Clean up 2007 URS -60% Jacobs - 20% ECC - 10% Paralax - 10%

457

Business Owners: Prepare for Utility Disruptions | Department...  

Broader source: Energy.gov (indexed) [DOE]

to operate vital systems and equipment during an emergency; Choosing the best type of generator, such as a diesel- or natural gas-fueled generator, or a commercial-grade...

458

Scott Roseman: Owner, New Leaf Community Markets  

E-Print Network [OSTI]

history, first met Roseman while she was an undergraduate student at UCSC doing an internship in alternative energy

Reti, Irene H.

2010-01-01T23:59:59.000Z

459

Energy Performance and Home Owner Behavior  

E-Print Network [OSTI]

to describe occupancy behavior in buildings. Integrate with energy consumption patterns ESL-KT-13-12-04 CATEE 2013: Clean Air Through Energy Efficiency Conference, San Antonio, Texas Dec. 16-18 IEA Annex 66 IEA Annex 66 Definition and Simulation...

Dong, B.

2013-01-01T23:59:59.000Z

460

Vision of a Multi Properties Owner  

E-Print Network [OSTI]

Upscale8%Midscale37%Economy55% 4 000 HOTELS450 000 guest rooms DGTHDGTH The General Management of Hotel Technical Services is in charge :?To write the Technical Standards Documents?To manage construction of new properties and main refurbishment... was indicated + / -:-guest not able to select himself the right temperature-many guest complains-therefore modification of the system BMS SMALL STORIESBMS SMALL STORIES Sofitel, energy management in guest rooms :?Room no booked : temperature = set point ? 5?C?Room...

Bouilleaud

2004-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "binary owner ormat" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


461

SAFETY MANUAL Fishermen, Captains, and Owners  

E-Print Network [OSTI]

... . ....... ,', .... "., .. , ....... , ..... ".,.. . 28 Main and auxiliary engines, ........... , ...... , ..... , . , .. , . . 29 Fuel systems ..... , ..... , ... , .. , .. , ... ,',." .... , ... ,.. 32 Storage batteries ....... , , .. , ..... , , ... , ... , , , , ... , , , , , , . , , , 33 Alarms

462

Governmental-Owner Power Imbalance and Privatization  

E-Print Network [OSTI]

Privatization is defined as the sale of state-owned assets by governmental agencies to private investors (e.g., Megginson, Nash, Netter, and Poulsen, 2004; Villalonga, 2000). Research on privatization has focused on privatization techniques (e...

Xu, Kehan

2011-10-21T23:59:59.000Z

463

Scott Roseman: Owner, New Leaf Community Markets  

E-Print Network [OSTI]

worked for the Alternative Energy Co-op, an organizationdoing an internship in alternative energy systems. After theat what was called the Alternative Energy Co-op, which was a

Reti, Irene H.

2010-01-01T23:59:59.000Z

464

Scott Roseman: Owner, New Leaf Community Markets  

E-Print Network [OSTI]

pioneered a sustainable-seafood labeling program namedheavily for us. Sustainable Seafood Fishwise Program Reti:have is the Sustainable Seafood program. Roseman: Yes. New

Reti, Irene H.

2010-01-01T23:59:59.000Z

465

An Owner's Guide to Smoothed Particle Hydrodynamics  

E-Print Network [OSTI]

We present a practical guide to Smoothed Particle Hydrodynamics (\\SPH) and its application to astrophysical problems. Although remarkably robust, \\SPH\\ must be used with care if the results are to be meaningful since the accuracy of \\SPH\\ is sensitive to the arrangement of the particles and the form of the smoothing kernel. In particular, the initial conditions for any \\SPH\\ simulation must consist of particles in dynamic equilibrium. We describe some of the numerical difficulties that may be encountered when using \\SPH, and how these may be overcome. Through our experience in using \\SPH\\ code to model convective stars, galaxy clusters and large scale structure problems we have developed many diagnostic tests. We give these here as an aid to rapid identification of errors, together with a list of basic prerequisites for the most efficient implementation of \\SPH.

T. J. Martin; F. R. Pearce; P. A. Thomas

1993-10-13T23:59:59.000Z

466

Business Owners: Prepare for Utility Disruptions  

Broader source: Energy.gov [DOE]

Have a plan in place in case a natural disaster or other hazard knocks out your businesss electricity or natural gas service.

467

Well Owner's Guide To Water Supply  

E-Print Network [OSTI]

's groundwater and guidelines, including national drinking water standards, to test well water to insure safe drinking water in private wells. National drinking water standards and common methods of home water .....................22 Contaminants in Water........................................23 Drinking Water Guidelines

Fay, Noah

468

CHARACTERIZING LOW-MASS BINARIES FROM OBSERVATION OF LONG-TIMESCALE CAUSTIC-CROSSING GRAVITATIONAL MICROLENSING EVENTS  

SciTech Connect (OSTI)

Despite the astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stellar multiplicity across a broad range of physical parameters. In this paper, we report the detections and measurements of two binaries discovered from observations of microlensing events MOA-2011-BLG-090 and OGLE-2011-BLG-0417. Determinations of the binary masses are possible by simultaneously measuring the Einstein radius and the lens parallax. The measured masses of the binary components are 0.43 M{sub Sun} and 0.39 M{sub Sun} for MOA-2011-BLG-090 and 0.57 M{sub Sun} and 0.17 M{sub Sun} for OGLE-2011-BLG-0417 and thus both lens components of MOA-2011-BLG-090 and one component of OGLE-2011-BLG-0417 are M dwarfs, demonstrating the usefulness of microlensing in detecting binaries composed of low-mass components. From modeling of the light curves considering full Keplerian motion of the lens, we also measure the orbital parameters of the binaries. The blended light of OGLE-2011-BLG-0417 comes very likely from the lens itself, making it possible to check the microlensing orbital solution by follow-up radial-velocity observation. For both events, the caustic-crossing parts of the light curves, which are critical for determining the physical lens parameters, were resolved by high-cadence survey observations and thus it is expected that the number of microlensing binaries with measured physical parameters will increase in the future.

Shin, I.-G.; Han, C.; Choi, J.-Y. [Department of Physics, Institute for Astrophysics, Chungbuk National University, Cheongju 371-763 (Korea, Republic of); Udalski, A.; Szymanski, M. K.; Kubiak, M.; Soszynski, I.; Pietrzynski, G.; Poleski, R.; Ulaczyk, K.; Pietrukowicz, P.; Kozlowski, S.; Wyrzykowski, L. [Warsaw University Observatory, Al. Ujazdowskie 4, 00-478 Warszawa (Poland); Sumi, T. [Department of Earth and Space Science, Osaka University, Osaka 560-0043 (Japan); Gould, A.; Skowron, J. [Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States); Bozza, V. [Dipartimento di Fisica 'E.R. Caianiello', Universita degli Studi di Salerno, Via S. Allende, 84081 Baronissi (Italy); Dominik, M.; Horne, K. [SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS (United Kingdom); Fouque, P. [IRAP, Universite de Toulouse, CNRS, 14 Avenue Edouard Belin, 31400 Toulouse (France); Collaboration: OGLE Collaboration; MOA Collaboration; RoboNet Collaboration; MiNDSTEp Consortium; muFUN Collaboration; PLANET Collaboration; and others

2012-08-20T23:59:59.000Z

469

Can the Organization of a Binary Mix Be Predicted from the Surface Energy, Cohesion Parameter and Particle Size of Its Components?  

Science Journals Connector (OSTI)

Purpose.... The aim of this study was to relate the organization of several binary mixes with three physical parameters (surface energy, cohesion parameter, and particle size) of...

J. Barra; F. Lescure; F. Falson-Rieg; E. Doelker

1998-11-01T23:59:59.000Z

470

Lattice stability of aluminum-rare earth binary systems: A first-principles approach  

Science Journals Connector (OSTI)

The thermodynamics of over 330 compounds in 15 Al-RE (RE=rare earth elements) binary systems is studied via first-principles density-functional theory at low-temperature limit. The calculated phase stabilities at T=0K are in very good agreement with experimentally reported ones for the majority of the systems. For example, we show the Al2RE.cF24 structure is the most stable compound phase in each binary and it indeed has the highest (congruent) melting point in each system. In some other cases, we obtain results previously unknown experimentally. For example, we suggest that the structure of the observed compound AlTm2 is isostructural with Co2Si.oP12 (prototype Co2Si, Pearson symbol oP12), we confirm the stability of AlEu.oP20 rather than AlEu.oP18 by examining the energetics of vacancy substitution, and we predict the unreported Al-Pm phase diagram. Relative accuracy of different potentials and calculational details are addressed. This study predicts that the Al-RE phase diagrams evolve systematically across the entire RE series, interrupted by anomalies at elements Ce and especially Eu and Yb. Trends in lattice stability across the RE series are explained on the basis of interatomic bonding and strain. This study demonstrates that first-principles calculations can be employed to (1) further examine and improve the experimentally established binary-alloy phase diagrams, and (2) provide accurate enthalpy data for stable and hypothetical compounds and structures.

Michael C. Gao; Anthony D. Rollett; Michael Widom

2007-05-31T23:59:59.000Z

471

Basic Parameter Estimation of Binary Neutron Star Systems by the Advanced LIGO/Virgo Network  

Science Journals Connector (OSTI)

Within the next five years, it is expected that the Advanced LIGO/Virgo network will have reached a sensitivity sufficient to enable the routine detection of gravitational waves. Beyond the initial detection, the scientific promise of these instruments relies on the effectiveness of our physical parameter estimation capabilities. A major part of this effort has been toward the detection and characterization of gravitational waves from compact binary coalescence, e.g., the coalescence of binary neutron stars. While several previous studies have investigated the accuracy of parameter estimation with advanced detectors, the majority have relied on approximation techniques such as the Fisher Matrix which are insensitive to the non-Gaussian nature of the gravitational wave posterior distribution function. Here we report average statistical uncertainties that will be achievable for strong detection candidates (S/N = 20) over a comprehensive sample of source parameters. We use the Markov Chain Monte Carlo based parameter estimation software developed by the LIGO/Virgo Collaboration with the goal of updating the previously quoted Fisher Matrix bounds. We find the recovery of the individual masses to be fractionally within 9% (15%) at the 68% (95%) credible intervals for equal-mass systems, and within 1.9% (3.7%) for unequal-mass systems. We also find that the Advanced LIGO/Virgo network will constrain the locations of binary neutron star mergers to a median uncertainty of 5.1 deg2 (13.5 deg2) on the sky. This region is improved to 2.3 deg2 (6 deg2) with the addition of the proposed LIGO India detector to the network. We also report the average uncertainties on the luminosity distances and orbital inclinations of strong detections that can be achieved by different network configurations.

Carl L. Rodriguez; Benjamin Farr; Vivien Raymond; Will M. Farr; Tyson B. Littenberg; Diego Fazi; Vicky Kalogera

2014-01-01T23:59:59.000Z

472

On the Properties of Hypermassive Neutron Stars Formed in Mergers of Spinning Binaries  

E-Print Network [OSTI]

We present numerical simulations of binary neutron star (BNS) mergers, comparing irrotational binaries to binaries of NSs rotating aligned to the orbital angular momentum. For the first time, we study spinning BNSs employing nuclear physics equations of state (EOS), namely the ones of Lattimer & Swesty as well as Shen & Horowitz & Teige. We study mainly equal mass systems leading to a hypermassive neutron star (HMNS), and analyze in detail its structure and dynamics. In order to exclude gauge artifacts, we introduce a novel coordinate system used for post-processing. The results for our equal mass models show that the strong radial oscillations of the HMNS modulate the instantaneous frequency of the gravitational wave (GW) signal to an extend that leads to separate peaks in the corresponding Fourier spectrum. In particular, the high frequency peaks which are often attributed to combination frequencies can also be caused by the modulation of the m=2 mode frequency in the merger phase. As a consequence for GW data analysis, the offset of the high frequency peak does not necessarily carry information about the radial oscillation frequency. Further, the low frequency peak in our simulations is dominated by the contribution of the plunge and the first 1-2 bounces. The amplitude of the radial oscillations depends on the initial NS spin, which therefore has a complicated influence on the spectrum. Another important result is that HMNSs can consist of a slowly rotating core with an extended, massive envelope rotating close to Keplerian velocity, contrary to the common notion that a rapidly rotating core is necessary to prevent a prompt collapse. Finally, our estimates on the amount of unbound matter show a dependency on the initial NS spin, explained by the influence of the latter on the amplitude of radial oscillations, which in turn cause shock waves.

Wolfgang Kastaun; Filippo Galeazzi

2014-11-28T23:59:59.000Z

473

The NINJA-2 project: Detecting and characterizing gravitational waveforms modelled using numerical binary black hole simulations  

E-Print Network [OSTI]

The Numerical INJection Analysis (NINJA) project is a collaborative effort between members of the numerical relativity and gravitational-wave astrophysics communities. The purpose of NINJA is to study the ability to detect gravitational waves emitted from merging binary black holes and recover their parameters with next-generation gravitational-wave observatories. We report here on the results of the second NINJA project, NINJA-2, which employs 60 complete binary black hole hybrid waveforms consisting of a numerical portion modelling the late inspiral, merger, and ringdown stitched to a post-Newtonian portion modelling the early inspiral. In a "blind injection challenge" similar to that conducted in recent LIGO and Virgo science runs, we added 7 hybrid waveforms to two months of data recolored to predictions of Advanced LIGO and Advanced Virgo sensitivity curves during their first observing runs. The resulting data was analyzed by gravitational-wave detection algorithms and 6 of the waveforms were recovered with false alarm rates smaller than 1 in a thousand years. Parameter estimation algorithms were run on each of these waveforms to explore the ability to constrain the masses, component angular momenta and sky position of these waveforms. We also perform a large-scale monte-carlo study to assess the ability to recover each of the 60 hybrid waveforms with early Advanced LIGO and Advanced Virgo sensitivity curves. Our results predict that early Advanced LIGO and Advanced Virgo will have a volume-weighted average sensitive distance of 300Mpc (1Gpc) for $10M_{\\odot}+10M_{\\odot}$ ($50M_{\\odot}+50M_{\\odot}$) binary black hole coalescences. We demonstrate that neglecting the component angular momenta in the waveform models used in matched-filtering will result in a reduction in sensitivity for systems with large component angular momenta. [Abstract abridged for ArXiv, full version in PDF

The LIGO Scientific Collaboration; the Virgo Collaboration; the NINJA-2 Collaboration; :; J. Aasi; B. P. Abbott; R. Abbott; T. Abbott; M. R. Abernathy; T. Accadia; F. Acernese; K. Ackley; C. Adams; T. Adams; P. Addesso; R. X. Adhikari; C. Affeldt; M. Agathos; N. Aggarwal; O. D. Aguiar; A. Ain; P. Ajith; A. Alemic; B. Allen; A. Allocca; D. Amariutei; M. Andersen; R. Anderson; S. B. Anderson; W. G. Anderson; K. Arai; M. C. Araya; C. Arceneaux; J. Areeda; S. M. Aston; P. Astone; P. Aufmuth; C. Aulbert; L. Austin; B. E. Aylott; S. Babak; P. T. Baker; G. Ballardin; S. W. Ballmer; J. C. Barayoga; M. Barbet; B. C. Barish; D. Barker; F. Barone; B. Barr; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; A. Basti; J. C. Batch; J. Bauchrowitz; Th. S. Bauer; B. Behnke; M. Bejger; M. G. Beker; C. Belczynski; A. S. Bell; C. Bell; G. Bergmann; D. Bersanetti; A. Bertolini; J. Betzwieser; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Biscans; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; S. Bloemen; M. Blom; O. Bock; T. P. Bodiya; M. Boer; G. Bogaert; C. Bogan; C. Bond; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; Sukanta Bose; L. Bosi; C. Bradaschia; P. R. Brady; V. B. Braginsky; M. Branchesi; J. E. Brau; T. Briant; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; A. F. Brooks; D. A. Brown; D. D. Brown; F. Brckner; S. Buchman; T. Bulik; H. J. Bulten; A. Buonanno; R. Burman; D. Buskulic; C. Buy; L. Cadonati; G. Cagnoli; J. Caldern Bustillo; E. Calloni; J. B. Camp; P. Campsie; K. C. Cannon; B. Canuel; J. Cao; C. D. Capano; F. Carbognani; L. Carbone; S. Caride; A. Castiglia; S. Caudill; M. Cavagli; F. Cavalier; R. Cavalieri; C. Celerier; G. Cella; C. Cepeda; E. Cesarini; R. Chakraborty; T. Chalermsongsak; S. J. Chamberlin; S. Chao; P. Charlton; E. Chassande-Mottin; X. Chen; Y. Chen; A. Chincarini; A. Chiummo; H. S. Cho; J. Chow; N. Christensen; Q. Chu; S. S. Y. Chua; S. Chung; G. Ciani; F. Clara; J. A. Clark; F. Cleva; E. Coccia; P. -F. Cohadon; A. Colla; C. Collette; M. Colombini; L. Cominsky; M. Constancio Jr.; A. Conte; D. Cook; T. R. Corbitt; M. Cordier; N. Cornish; A. Corpuz; A. Corsi; C. A. Costa; M. W. Coughlin; S. Coughlin; J. -P. Coulon; S. Countryman; P. Couvares; D. M. Coward; M. Cowart; D. C. Coyne; R. Coyne; K. Craig; J. D. E. Creighton; S. G. Crowder; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; T. Dal Canton; M. Damjanic; S. L. Danilishin; S. D'Antonio; K. Danzmann; V. Dattilo; H. Daveloza; M. Davier; G. S. Davies; E. J. Daw; R. Day; T. Dayanga; G. Debreczeni; J. Degallaix; S. Delglise; W. Del Pozzo; T. Denker; T. Dent; H. Dereli; V. Dergachev; R. De Rosa; R. T. DeRosa; R. DeSalvo; S. Dhurandhar; M. Daz; L. Di Fiore; A. Di Lieto; I. Di Palma; A. Di Virgilio; A. Donath; F. Donovan; K. L. Dooley; S. Doravari; S. Dossa; R. Douglas; T. P. Downes; M. Drago; R. W. P. Drever; J. C. Driggers; Z. Du; S. Dwyer; T. Eberle; T. Edo; M. Edwards; A. Effler; H. Eggenstein; P. Ehrens; J. Eichholz; S. S. Eikenberry; G. Endr?czi; R. Essick; T. Etzel; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Q. Fang; S. Farinon; B. Farr; W. M. Farr; M. Favata; H. Fehrmann; M. M. Fejer; D. Feldbaum; F. Feroz; I. Ferrante; F. Ferrini; F. Fidecaro; L. S. Finn; I. Fiori; R. P. Fisher; R. Flaminio; J. -D. Fournier; S. Franco; S. Frasca; F. Frasconi; M. Frede; Z. Frei; A. Freise; R. Frey; T. T. Fricke; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; J. Gair; L. Gammaitoni; S. Gaonkar; F. Garufi; N. Gehrels; G. Gemme; E. Genin; A. Gennai; S. Ghosh; J. A. Giaime; K. D. Giardina; A. Giazotto; C. Gill; J. Gleason; E. Goetz; R. Goetz; L. Gondan; G. Gonzlez; N. Gordon; M. L. Gorodetsky; S. Gossan; S. Goler; R. Gouaty; C. Grf; P. B. Graff; M. Granata; A. Grant; S. Gras; C. Gray; R. J. S. Greenhalgh; A. M. Gretarsson; P. Groot; H. Grote; K. Grover; S. Grunewald; G. M. Guidi; C. Guido; K. Gushwa; E. K. Gustafson; R. Gustafson; D. Hammer; G. Hammond; M. Hanke; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. Hart; M. T. Hartman; C. -J. Haster; K. Haughian; A. Heidmann; M. Heintze; H. Heitmann; P. Hello; G. Hemming; M. Hendry; I. S. Heng; A. W. Heptonstall; M. Heurs; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; S. Hooper; P. Hopkins; D. J. Hosken; J. Hough; E. J. Howell; Y. Hu; B. Hughey; S. Husa; S. H. Huttner; M. Huynh; T. Huynh-Dinh; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; B. R. Iyer; K. Izumi; M. Jacobson; E. James; H. Jang; P. Jaranowski; Y. Ji; F. Jimnez-Forteza; W. W. Johnson; D. I. Jones; R. Jones; R. J. G. Jonker; L. Ju; Haris K; P. Kalmus; V. Kalogera; S. Kandhasamy; G. Kang; J. B. Kanner; J. Karlen; M. Kasprzack; E. Katsavounidis; W. Katzman; H. Kaufer; K. Kawabe; F. Kawazoe; F. Kflian; G. M. Keiser; D. Keitel; D. B. Kelley; W. Kells; A. Khalaidovski

2014-01-05T23:59:59.000Z

474

A Hard X-ray View of Accreting X-ray Binary Pulsars  

E-Print Network [OSTI]

The study of the hard (E>10 keV) energy spectra of X-ray binary pulsars can give a wealth of information on the physical processes that occur close to the neutron star surface. Extreme matter regimes are probed, and precious information on how matter and radiation behave and interact in critical conditions can be obtained. We will give an overview on the most recent results obtained by RXTE and BeppoSAX on this class of objects, in order to pass the baton onto just launched experiments, like INTEGRAL, or soon to be launched, like AGILE and ASTRO-E2.

Mauro Orlandini

2004-02-26T23:59:59.000Z

475

Automatic synthesis of quantum circuits for point addition on ordinary binary elliptic curves  

E-Print Network [OSTI]

Implementing the group arithmetic is a cost-critical task when designing quantum circuits for Shor's algorithm to solve the discrete logarithm problem. We introduce a tool for the automatic generation of addition circuits for ordinary binary elliptic curves, a prominent platform group for digital signatures. Our Python software generates circuit descriptions that, without increasing the number of qubits or T-depth, involve less than 39% of the number of T-gates in the best previous construction. The software also optimizes the (CNOT) depth for GF(2)-linear operations by means of suitable graph colorings.

Parshuram Budhathoki; Rainer Steinwandt

2014-01-10T23:59:59.000Z

476

IUPAC-NIST Solubility Data Series 71. Nitromethane with Water or Organic Solvents: Binary Systems  

Science Journals Connector (OSTI)

The mutual solubilities and liquidliquid equilibrium of nitromethane binary systems with liquidsolvents are reviewed. The solvents include water inorganic compounds and a variety of organic compounds as hydrocarbons halogenated hydrocarbons alcohols acids esters and nitrogen compounds. A total 474 systems published through 1993 are compiled. For 39 systems sufficient data were available to allow critical evaluation. All data are expressed as mass and mole fractions as well as the originally reported units. Similar reviews of gas liquid and solid solubilities for other systems were published in the frame of Solubility Data Series.

Valerii P. Sazonov; Kenneth N. Marsh; Glenn T. Hefter

2000-01-01T23:59:59.000Z

477

On the Binary Nature of Dust-encircled BD+20 307  

E-Print Network [OSTI]

Three epochs of high resolution spectra of the star BD+20 307 show that it is a short period (~3.5 day) spectroscopic binary of two nearly identical stars. Surprisingly, the two stars, though differing in effective temperature by only ~250 K and having a mass ratio of 0.91, show very different Li line equivalent widths. A Li 6707 Angstrom line is only detected from the primary star, and it is weak. This star is therefore likely to be older than 1 Gyr. If so, the large amount of hot circumbinary dust must be from a very large and recent, but very late evolutionarily, collision of planetesimals.

A. J. Weinberger

2008-04-10T23:59:59.000Z

478

Phase diagram of EuI{sub 2}-KI binary system  

SciTech Connect (OSTI)

The phase diagram of the EuI{sub 2}-KI binary system was studied by differential thermal analysis (DTA) and X-ray powder diffraction (XRD). The phase diagram of the EuI{sub 2}-KI system shows the existence of one congruently melting compound, KEu{sub 2}I{sub 5}, and one incongruently melting compound, K{sub 4}EuI{sub 6}. There are two eutectic points located at 465 C, 20 mol% KI and 439 C, 60 mol% KI, respectively.

Sun, Y. [Beijing Normal Univ. (China). Dept. of Chemistry] [Beijing Normal Univ. (China). Dept. of Chemistry; [Univ. of Science and Technology, Beijing (China). Dept. of Physical Chemistry; Wang, S.; Wang, M. [Beijing Normal Univ. (China). Dept. of Chemistry] [Beijing Normal Univ. (China). Dept. of Chemistry; Qiao, Z. [Univ. of Science and Technology, Beijing (China). Dept. of Physical Chemistry] [Univ. of Science and Technology, Beijing (China). Dept. of Physical Chemistry

1998-02-15T23:59:59.000Z

479

The Origin of Power-Law Emergent Scaling in Large Binary Networks  

E-Print Network [OSTI]

In this paper we study the macroscopic conduction properties of large but finite binary networks with conducting bonds. By taking a combination of a spectral and an averaging based approach we derive asymptotic formulae for the conduction in terms of the component proportions p and the total number of components N. These formulae correctly identify both the percolation limits and also the emergent power law behaviour between the percolation limits and show the interplay between the size of the network and the deviation of the proportion from the critical value of p = 1/2. The results compare excellently with a large number of numerical simulations.

D. P. Almond; C. J. Budd; M. A. Freitag; G. W. Hunt; N. J. McCullen; N. D. Smith

2012-04-25T23:59:59.000Z

480

THE REFLECTION EFFECT IN INTERACTING BINARIES OR IN PLANET-STAR SYSTEMS  

SciTech Connect (OSTI)

There are many similarities between interacting binary stars and stars with a close-in giant extrasolar planet. The reflection effect is a well-known example. Although the generally accepted treatment of this effect in interacting binaries is successful in fitting light curves of eclipsing binaries, it is not very suitable for studying cold objects irradiated by hot objects or extrasolar planets. The aim of this paper is to develop a model of the reflection effect which could be easily incorporated into the present codes for modeling of interacting binaries so that these can be used to study the aforementioned objects. Our model of the reflection effect takes into account the reflection (scattering), heating, and heat redistribution over the surface of the irradiated object. The shape of the object is described by the non-spherical Roche potential expected for close objects. Limb and gravity darkening are included in the calculations of the light output from the system. The model also accounts for the orbital revolution and rotation of the exoplanet with appropriate Doppler shifts for the scattered and thermal radiation. Subsequently, light curves and/or spectra of several exoplanets have been modeled and the effects of the heat redistribution, limb darkening/brightening, (non-)gray albedo, and non-spherical shape have been studied. Recent observations of planet-to-star flux ratio of HD189733b, WASP12b, and WASP-19b at various phases were reproduced with very good accuracy. It was found that HD189733b has a low Bond albedo and intense heat redistribution, while WASP-19b has a low Bond albedo and low heat redistribution. The exact Roche geometries and temperature distributions over the surface of all 78 transiting extrasolar planets have been determined. Departures from the spherical shape may vary considerably but departures of about 1% in the radius are common within the sample. In some cases, these departures can reach 8%, 12%, or 14%, for WASP-33b, WASP-19b, and WASP-12b, respectively. The mean temperatures of these planets also vary considerably from 300 K to 2600 K. The extreme cases are WASP-18b, WASP-12b, and WASP-33b, with mean temperatures of 2330 K, 2430 K, and 2600 K, respectively.

Budaj, J., E-mail: budaj@ta3.sk [Astronomical Institute, Slovak Academy of Sciences, Tatranska Lomnica 05960 (Slovakia)

2011-02-15T23:59:59.000Z

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