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Note: This page contains sample records for the topic "waha lone star" from the National Library of EnergyBeta (NLEBeta).
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We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


1

Lone Star Healthy Streams Final Report  

E-Print Network (OSTI)

. Portions of this program were delivered to audiences at over 40 events throughout the state, reaching well over 2,200 participants. In addition, unique visitors to the ?Improving Water Quality of Grazing Lands? website exceeded 1,100. This highly... beneficial program will continue to be carried out throughout the state in coordination with the TSSWCB and other project partners. Lone Star Healthy Streams Final Report 2 Table of Contents Executive Summary...

Wagner, Kevin; Redmon, Larry

2

Clean Cities: Lone Star Clean Fuels Alliance (Central Texas) coalition  

Alternative Fuels and Advanced Vehicles Data Center (EERE)

Lone Star Clean Fuels Alliance (Central Texas) Coalition Lone Star Clean Fuels Alliance (Central Texas) Coalition The Lone Star Clean Fuels Alliance (Central Texas) coalition works with vehicle fleets, fuel providers, community leaders, and other stakeholders to reduce petroleum use in transportation. Lone Star Clean Fuels Alliance (Central Texas) coalition Contact Information Stacy Neef 512-773-8794 stacy.neef@lonestarcfa.org Coalition Website Clean Cities Coordinator Stacy Neef Photo of Stacy Neef Stacy Neef has served as the coordinator for Lone Star Clean Fuels Alliance (Austin) (LSCFA) promoting and advancing the use of alternative fuel and vehicles for fleets in central Texas since 2000. The central Texas region includes Bastrop, Caldwell, Hays, Travis, Williamson Counties; Fort Hood and City of Temple, Texas. LSCFA works closely with other Texas Clean

3

Lone Star Healthy Streams: Teaching best managment practices statewide  

E-Print Network (OSTI)

txH2O | pg. 22 Story by Leslie Lee The Lone Star Healthy Streams (LSHS) Program uses education to reduce the amount of bacteria entering Texas water bodies from livestock operations and feral hogs. This program, originally developed...

Lee, Leslie

2011-01-01T23:59:59.000Z

4

Lone Star Healthy Streams: Teaching best management practices statewide  

E-Print Network (OSTI)

txH2O | pg. 22 Story by Leslie Lee The Lone Star Healthy Streams (LSHS) Program uses education to reduce the amount of bacteria entering Texas water bodies from livestock operations and feral hogs. This program, originally developed...

Lee, Leslie

2010-01-01T23:59:59.000Z

5

Lone Star I (Q3) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

I (Q3) Wind Farm I (Q3) Wind Farm Jump to: navigation, search Name Lone Star I (Q3) Wind Farm Facility Lone Star I (Q3) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Developer RES/Horizon Energy Purchaser Direct Energy Location Callahan and Shackelford counties TX Coordinates 32.594885°, -99.506464° 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":32.594885,"lon":-99.506464,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

6

Lone Star I (Q2) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Q2) Wind Farm Q2) Wind Farm Jump to: navigation, search Name Lone Star I (Q2) Wind Farm Facility Lone Star I (Q2) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Developer RES/Horizon Energy Purchaser Direct Energy Location Callahan and Shackelford counties TX Coordinates 32.594885°, -99.506464° 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":32.594885,"lon":-99.506464,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

7

Lone Star Wind Alliance LSWA | Open Energy Information  

Open Energy Info (EERE)

Wind Alliance LSWA Wind Alliance LSWA Jump to: navigation, search Name Lone Star Wind Alliance (LSWA) Place Houston, Texas Sector Wind energy Product Texas-based research centres, focusing on large composite structures, wind engineering, electromechanical controls and power electronics. The organisation is led by the University of Houston. Coordinates 29.76045°, -95.369784° 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":29.76045,"lon":-95.369784,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

8

Lone Star Reds: the Socialist Party and cotton tenancy in Texas, 1901-1917  

E-Print Network (OSTI)

ideal, the party of Eugene Debs seized on the strong Texas tradition of agrarian revolt to build a formidable, if short-lived, Socialist movement in the Lone Star State. There were Socialist newspapers, unions, rural encampments, and a Socialist...

Mellard, Jason Dean

2000-01-01T23:59:59.000Z

9

Lone Star I (4Q07) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Lone Star I (4Q07) Wind Farm Lone Star I (4Q07) Wind Farm Facility Lone Star I (4Q07) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Developer RES/Horizon Energy Purchaser Direct Energy Location Callahan and Shackleford Counties TX Coordinates 32.594885°, -99.506464° 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":32.594885,"lon":-99.506464,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

10

Lone Star II (1Q08) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

1Q08) Wind Farm 1Q08) Wind Farm Facility Lone Star II (1Q08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Developer RES/Horizon Energy Purchaser JAron Location Callahan and Shackelford counties TX Coordinates 32.594885°, -99.506464° 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":32.594885,"lon":-99.506464,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

11

Lone Star II (4Q07) Wind Farm | Open Energy Information  

Open Energy Info (EERE)

4Q07) Wind Farm 4Q07) Wind Farm Facility Lone Star II (4Q07) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Horizon Wind Energy Developer RES/Horizon Energy Purchaser JAron Location Callahan and Shackleford Counties TX Coordinates 32.594885°, -99.506464° 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":32.594885,"lon":-99.506464,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

12

LoneSTAR Program: Maximizing Energy Efficiency while Protecting the Envrionment  

E-Print Network (OSTI)

Assessment Report (EAR) ? Utility Assessment Report (UAR) ? Systems Commissioning Report (in the case where the commissioning meets LoanSTAR payback requirements) ESL-KT-14-11-31 CATEE 2014: Clean Air Through Efficiency Conference, Dallas, Texas Nov. 18...Maximiz ing Energy Eff ic iency whi le Protect ing the Envi ronment LoanSTAR PROGRAM ESL-KT-14-11-31 CATEE 2014: Clean Air Through Efficiency Conference, Dallas, Texas Nov. 18-20 ? Executed 240 loans totaling $407,923,762.32 ? 93 loans to publ...

Trevino, E.

2014-01-01T23:59:59.000Z

13

Lone Star Transmission LLC | Open Energy Information  

Open Energy Info (EERE)

Zip: 33408 Product: Wholly owned subsidiary of FPL Energy, developing transmission lines. First project is the DFW Express high voltage DC line from West Texas to DallasFort...

14

CA-TRIBE-PAIUTE-SHOSHONE INDIANS OF THE LONE PINE  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

U.S. Department of Energy Categorical Exclusion Determination Form Program or Field Office: Energy Efficiency and Conservation Block Grant Program Project Title CA-TRIBE-PAIUTE-SHOSHONE INDIANS OF THE LONE PINE COMMUNITY Location: Tribe CA-TRIBE-PAIUTE- SHOSHONE INDIANS OF THE LONE PINE COMMUNITY CA American Recovery and Reinvestment Act: Proposed Action or Project Description The Paiute-Shoshone Indians of the Lone Pine Community propose to prepare a feasibility study for

15

Lone Star Healthy Streams: Keeping Texas streams clean  

E-Print Network (OSTI)

-farm composting system using windrows, static piles and in-vessel composting can effectively reduce pathogens to levels that are acceptable in organic soil amendments. ... Association, Texas Association of Dairymen, Texas Horse, Texas Poultry Federation, Texas Pork Producers Association and Texas Parks and Wildlife Department. Funding for the LSHS program was provided by NRCS, the State of Texas and the Texas State Soil...

Boutwell, Kathryn S.

2013-01-01T23:59:59.000Z

16

Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides  

NLE Websites -- All DOE Office Websites (Extended Search)

Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print "Ferroelectricity," by analogy to ferromagnetism, is defined as the presence of spontaneous electrical polarization in a material, often arising from distortions in the material's crystal structure. In oxides of the metals lead and bismuth, such distortions were for many years attributed to the existence of "lone pair" electrons: pairs of chemically inert, nonbonding valence electrons in hybrid orbitals that leave noticeable voids in the crystal structure. At the ALS, researchers from the U.K., Ireland, and the U.S. have now obtained definitive experimental evidence that this lone-pair model must be revised. High-resolution x-ray photoemission spectroscopy (XPS) and soft x-ray emission spectroscopy (XES) have clarified the subtle electronic origins of the prototypical distortions in these crystal structures. The results have important implications for the tantalizing possibility of spintronic or superconducting devices combining ferroelectric and ferromagnetic properties.

17

Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides  

NLE Websites -- All DOE Office Websites (Extended Search)

Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print "Ferroelectricity," by analogy to ferromagnetism, is defined as the presence of spontaneous electrical polarization in a material, often arising from distortions in the material's crystal structure. In oxides of the metals lead and bismuth, such distortions were for many years attributed to the existence of "lone pair" electrons: pairs of chemically inert, nonbonding valence electrons in hybrid orbitals that leave noticeable voids in the crystal structure. At the ALS, researchers from the U.K., Ireland, and the U.S. have now obtained definitive experimental evidence that this lone-pair model must be revised. High-resolution x-ray photoemission spectroscopy (XPS) and soft x-ray emission spectroscopy (XES) have clarified the subtle electronic origins of the prototypical distortions in these crystal structures. The results have important implications for the tantalizing possibility of spintronic or superconducting devices combining ferroelectric and ferromagnetic properties.

18

BAUCHE TALLIES LONE GOAL IN HUSKIE WIN By Nicole Betker, University of Saskatchewan Sports Information  

E-Print Network (OSTI)

BAUCHE TALLIES LONE GOAL IN HUSKIE WIN By Nicole Betker, University of Saskatchewan Sports Information SASKATOON, SK - University of Saskatchewan rookie Mitch Bauche tallied his first CIS goal in a 1 sides had numerous opportunities to score. Saskatchewan tallied 30 shots in the game, while UNBC had 16

Northern British Columbia, University of

19

Policy Recommendations for Establishing the LoneSTAR Monitoring and Analysis Program  

E-Print Network (OSTI)

in Texas The Monitoring and Analysis Program should be conducted by: A Monitoring and Analysis Contractor (MAC) Data Acquisition Subcontractors (DAS) A Monitoring Advisory and Review Committee (MARC) Monitoring and data analysis should be conducted at three... primary levels: Facility/whole building(s) utility data Facility/whole building (s) short-term demand and consumption data Sub-metered retrofit data Monitoring and Analysis Program cost is expected to be approximately: Three percent of retrofit cost...

Claridge, D. E.; O'Neal, D. L.; Turner, W. D.

1989-01-01T23:59:59.000Z

20

Audit of Lone Star Gas Invoices and Billing Procedures, Task #3  

E-Print Network (OSTI)

information on a SHEET NO. 3 "real-time" basis. Any such systems so installed shall be compatible with Shipper's SCADA system to the extent possible. (f) The other party may, at its option and expense, install and operate meters, instruments and equipment...

Turner, W. D.; Liu, M.

1997-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Development of a Synergistic, Comprehensive Statewide Lone Star Healthy Streams Program  

E-Print Network (OSTI)

) March 9, 2011 Victoria Co. TPWD and USDA-NRCS personnel (32) March 12, 2011 Brazos Co. (96) March 22, 2011 Weatherford (67) March 28, 2011 McLennan Co. (60) March 31, 2011 Caldwell Co. (31) April 7, 2011 Henderson Co. (137...

Wagner, K.; Redmon, L.; Peterson, J.

2013-01-01T23:59:59.000Z

22

"Climate Wise" in the Lone Star State: A Successful Partnership for Energy Efficiency in Austin, Texas  

E-Print Network (OSTI)

The City of Austin, Texas is forming partnerships with local companies to lower energy consumption and improve environmental performance within the industrial sector. As a local government participant in the federal Climate Wise program, Austin...

Allen, S. J.; Schare, S.

23

Physiological Ageing as it is Related to Gene Function in the Lone Star Tick, Amblyomma americanum  

E-Print Network (OSTI)

............................ 15 Figure 4 Electrophoresis gel results for the expression of the 16S gene in Amblyomma americanum subdivided by the mortality percentile to the right of the result, the sample number over the top of the result, and the group... as assessed by Image J software displaying the expression of Amblyomma americaum gene 16S for the female control (FC), male control (MC), female experimental (FE), and male experimental (ME) groups from Day 0 to Day 77...

Catena, Amanda M.

2010-07-14T23:59:59.000Z

24

Doing science: teachers' authentic experiences at the Lone Star Dinosaur Field Institute  

E-Print Network (OSTI)

Winkler and Dr. Louis Jacobs also deserve special thanks for being great science teachers. Though I was engaged primarily as an educational researcher, I found myself to be a science student as well. Through the experience that the scientists help... of excavating fossils, teachers, museum educators, and scientists sat around the campfire ruminating over their experiences. The team's videographer tumed his camera on paleontologist Louis Jacobs. With the campfire in the background, Louis Jacobs took...

Stiles, Thomas William

2001-01-01T23:59:59.000Z

25

DeLone & McLean IS Success Model in Evaluating Knowledge Transfer in a Virtual Learning Environment  

Science Journals Connector (OSTI)

DeLone & McLean's success model has been actively used since its first introduction in 1992. In this article, the authors extend this model to describe the success of knowledge sharing in an information system that included a part of the knowledge ... Keywords: Apprenticeship, DeLone & McLean Success Model, Knowledge Management, Knowledge Sharing, Systems Analysis, User Attitudes, Virtual Learning Environment

Raija Halonen; Heli Thomander; Elisa Laukkanen

2010-04-01T23:59:59.000Z

26

Ligand Lone-Pair Influence on Hydrocarbon C-H Activation: A Computational Perspective  

SciTech Connect

Mid to late transition metal complexes that break hydrocarbon C?H bonds by transferring the hydrogen to a heteroatom ligand while forming a metal?alkyl bond offer a promising strategy for C?H activation. Here we report a density functional (B3LYP, M06, and X3LYP) analysis of cis-(acac){sub 2}MX and TpM(L)X (M = Ir, Ru, Os, and Rh; acac = acetylacetonate, Tp = tris(pyrazolyl)borate; X = CH{sub 3}, OH, OMe, NH{sub 2}, and NMe{sub 2}) systems for methane C?H bond activation reaction kinetics and thermodynamics. We address the importance of whether a ligand lone pair provides an intrinsic kinetic advantage through possible electronic d{sub ?}?p{sub ?} repulsions for M?OR and M?NR{sub 2} systems versus M?CH{sub 3} systems. This involves understanding the energetic impact of the X ligand group on ligand loss, C?H bond coordination, and C?H bond cleavage steps as well as understanding how the nucleophilicity of the ligand X group, the electrophilicity of the transition metal center, and cis-ligand stabilization effect influence each of these steps. We also explore how spectator ligands and second- versus third-row transition metal centers impact the energetics of each of these C?H activation steps.

Ess, Daniel H; Gunnoe, T. Brent; Cundari, Thomas R; Goddard, William A; Periana, Roy A

2010-01-01T23:59:59.000Z

27

Evaluation and Demonstration of BMPs for Cattle on Grazing Lands for the Lone Star Healthy Streams Program  

E-Print Network (OSTI)

Life Research Center at McGregor utilizing Lotek GPS collars. Results suggest that stocking rates heavier than 6 ha/AUY (14.8 ac/AUY) increased E. coli loading, but only when sites were actively or recently (within the last two weeks) stocked when runoff.../Objectives........................................................................................................................... 6 Methods and Results .................................................................................................................................... 7 Task 1: Project Coordination and Administration...

Wagner, K.; Redmon, L.; Gentry, T.; Clary, C.

28

Understanding the Hydrogen Bond in Terms of the Location of the Bond Critical Point and the Geometry of the Lone Pairs  

Science Journals Connector (OSTI)

The origin of such high dCP values has been related to the constellation of the various interaction centersthe lone pairs and the atom cores of the donor and the acceptor oxygens and the hydrogen atom. ... Furthermore, for closed-shell interactions, the kinetic energy density, G(rCP), and the potential energy density, V(rCP), at the critical point depend exponentially on the HO distance. ... The crystal contains three short strong N-H ? O hydrogen bonds (HBs) with dN?O energies above 13 kcal mol-1, although the hydrogen atoms are firmly localized in the "nitrogen wells". ...

Anupama Ranganathan; G. U. Kulkarni; C. N. R. Rao

2003-07-15T23:59:59.000Z

29

STAR METRICS  

Energy.gov (U.S. Department of Energy (DOE))

Energy continues to define Phase II of the STAR METRICS program, a collaborative initiative to track Research and Development expenditures and their outcomes. Visit the STAR METRICS website for...

30

ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

and Other and Other Climate Protection Partnerships 2011 Annual Report CONTENTS Letter from the Administrator ............................................................................................................................................................................. 1 Executive Summary .............................................................................................................................................................................................. 2 Highlights of 2011 ......................................................................................................................................................................................... 4 ENERGY STAR Overview ......................................................................................................................................................................................

31

Electron lone pair distortion facilitated metal-insulator transition in ?-Pb{sub 0.33}V{sub 2}O{sub 5} nanowires  

SciTech Connect

The electronic structure of ?-Pb{sub 0.33}V{sub 2}O{sub 5} nanowires has been studied with x-ray photoelectron spectroscopy techniques. The recent synthesis of defect-free ?-Pb{sub 0.33}V{sub 2}O{sub 5} nanowires resulted in the discovery of an abrupt voltage-induced metal insulator transition. First principle calculations predicted an additional V-O-Pb hybridized in-gap state unique to this vanadium bronze playing a significant role in facilitating the transition. We confirm the existence, energetic position, and orbital character of the in-gap state. Moreover, we reveal that this state is a hybridized Pb 6sO 2p antibonding lone pair state resulting from the asymmetric coordination of the Pb{sup 2+} ions.

Wangoh, L.; Quackenbush, N. F. [Department of Physics, Applied Physics and Astronomy, Binghamton University, Binghamton, New York 13902 (United States); Marley, P. M.; Banerjee, S. [Department of Chemistry, University at Buffalo, The State University of New York, Buffalo, New York 14260 (United States); Sallis, S. [Materials Science and Engineering, Binghamton University, Binghamton, New York 13902 (United States); Fischer, D. A.; Woicik, J. C. [Materials Science and Engineering Laboratory, National Institute of Standards and Technology, Gaithersburg, Maryland 20899 (United States); Piper, L. F. J., E-mail: lpiper@binghamton.edu [Department of Physics, Applied Physics and Astronomy, Binghamton University, Binghamton, New York 13902 (United States); Materials Science and Engineering, Binghamton University, Binghamton, New York 13902 (United States)

2014-05-05T23:59:59.000Z

32

Petrologic and stable isotopic evidence for reaction-enhanced fluid flow during metamorphism of Precambrian-Cambrian sedimentary rocks, Lone Mountain, Nevada  

SciTech Connect

Upper Precambrian to Cambrian sedimentary rocks, regionally metamorphosed during the Mesozoic to produce marbles and calc-silicate rocks, were contact metamorphosed at the end of the Cretaceous by the Lone Mountain granitic pluton. Mineral assemblages within the calc-silicates were in equilibrium with H[sub 2]O-rich fluids, while the marbles were in equilibrium with more CO[sub 2]-rich fluids. Mineralogical variation between two different calc-silicate lithologies is the result of differences in bulk rock chemical composition, which also results in differences in isotopic composition between the calc-silicate lithologies. delta O-18 and delta C-13 values show differences of greater than 6 and 4 per mil respectively across lithologic boundaries between interlayered calc-silicates and between interlayered marbles and calc-silicates. The absence of any systematic variation between delta O-18 and delta C-13 values in the calc-silicates suggests that isotopic variation due to decarbonation reactions was limited. The differences in mineralogy and isotopic composition indicate that permeability was enhanced by reaction, permitting the focused flow of fluid through the calc-silicates. Calculated mass balance variations in delta O-18 based on reaction space analysis and Rayleigh decarbonation cannot explain the observed variations of delta O-18, requiring infiltration of externally derived fluids, while the delta C-13 compositions in the calc-silicates can be explained by Rayleigh decarbonation alone.

Richards, I.J.; Labotka, T.C. (Univ. of Tennessee, Knoxville, TN (United States). Dept. of Geochemical Sciences)

1992-01-01T23:59:59.000Z

33

ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Protection Agency program helping businesses and individuals fight global warming through superior energy efficiency. Bring Your Green to Work with ENERGY STAR ® 1 Give It a rest Use the ENERGY STAR power management settings on your computer and monitor so they go into power save mode when not in use. Also use a power strip as a central "turn off" point when you are using equipment to completely disconnect the power supply. 2 Unplug It Unplug electronics such as cell phones and laptops once they are charged. Adapters plugged into outlets use energy even if they are not charging. 3 Light Up Your Work Life Replace the light bulb in your desk lamp with an ENERGY STAR qualified bulb. It will last up to 10 times longer and use about 75 percent less energy. Turn off the lights when

34

Star Power  

SciTech Connect

The U.S. Department of Energy's Princeton Plasma Physics Laboratory has released ''Star Power,'' a new informational video that uses dramatic and beautiful images and thought-provoking interviews to highlight the importance of the Laboratory's research into magnetic fusion.

None

2014-10-17T23:59:59.000Z

35

Star Power  

ScienceCinema (OSTI)

The U.S. Department of Energy's Princeton Plasma Physics Laboratory has released ''Star Power,'' a new informational video that uses dramatic and beautiful images and thought-provoking interviews to highlight the importance of the Laboratory's research into magnetic fusion.

None

2014-11-18T23:59:59.000Z

36

ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

of Air and Radiation * For more information www.energystar.gov or call 1.888.STAR.YES (1.888.782.7937) * (6202J) EPA 430-H-08-002 * December 2008 * Recycled/Recyclable - Printed with Vegetable Oil Based Inks on Recycled Paper (Minimum 50% Post-consumer Content) of Air and Radiation * For more information www.energystar.gov or call 1.888.STAR.YES (1.888.782.7937) * (6202J) EPA 430-H-08-002 * December 2008 * Recycled/Recyclable - Printed with Vegetable Oil Based Inks on Recycled Paper (Minimum 50% Post-consumer Content) Enable power management settings so they automatically enter a low-power mode when not in use. monitor/computer Use a power strip as a central "turn off" point when you are done using office equipment to completely disconnect the power supply. power strip Unplug electronics

37

Energy Star  

E-Print Network (OSTI)

ENERGY STAR ENERGY TARGETS ESL-KT-12-10-08 CATEE 2012: Clean Air Through Energy Efficiency Conference, Galveston, TX, October 9-11, 2012 POP QUIZ!!!! What is EUI?? Energy Use Intensity Do you know the EUI and any of the buildings you designed... this past year? Do you know what a good EUI is for an Office building? K-12 School? ESL-KT-12-10-08 CATEE 2012: Clean Air Through Energy Efficiency Conference, Galveston, TX, October 9-11, 2012 POP QUIZ!!!! ESL-KT-12-10-08 CATEE 2012: Clean Air...

Reihl, K.; Tullos, A.

2012-01-01T23:59:59.000Z

38

Social networks for lonely objects  

E-Print Network (OSTI)

Visions of ubiquitous computing describe a network of devices that quietly supports human goals, but this may also add complexity to an already frustrating relationship between humans and their electronic objects. As we ...

Kestner, John Anthony

2010-01-01T23:59:59.000Z

39

ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

New Energy Technology 2754 Compass Drive, Grand Junction, CO 81506 Business: Energy Management Services/Consulting Sarah Faverman Phone: 970-243-0255 / Fax: 970-245-4268 Email: sarah@newenergytech.net Customer JCPenney Company, Inc. 6501 Legacy Drive, Plano, TX 75024 Business: Retail Rob Keller, P.E., Energy Management & Engineering Services Director Phone: 972-431-1788 / Fax: 972-531-1788 Email: rkeller@jcpenney.com New Energy Technology helped JCPenney earn the first ENERGY STAR labels for retail buildings and Partner of the Year Award. Project Scope New Energy Technology (NET) supports JCPenney's (JCP) energy conservation culture through three programs focused on high-quality energy data and energy management. Through its automated benchmarking

40

ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Green Team Checklist Green Team Checklist One person cannot do it all! So when it comes to making your workplace greener and more energy efficient, nothing beats a team. The Environmental Protection Agency (EPA) has learned from ENERGY STAR partners that forming a green team with coworkers is a great way to help increase energy efficiency and reduce office waste. Consider the following checklist of creative ideas from EPA to help your green team get started. Once you've formed your team, start by planting the seeds for success with small changes in individual workspaces. Then move through the list and help success bloom with bigger changes that can affect the whole organization. Together, these actions can help your green team build a better world! Start Off Right-Meet with management to get approval and buy-in for the idea of forming a green team. Not only does support

Note: This page contains sample records for the topic "waha lone star" 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

2014 ENERGY STAR Awards : ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Partner Resources Partner Resources Manufacturers Retailers New Home Industry Utilities/EEPS Residential & Commercial Products Programs Service & Product Providers Buildings & Plants Small Businesses Congregations For Contractors For Federal Agencies Join ENERGY STAR Home > Partner Resources > ENERGY STAR Awards 2014 ENERGY STAR Awards The application submission period for the 2014 ENERGY STAR Awards has closed. Each year, the ENERGY STAR program honors organizations that have made outstanding contributions to protecting the environment through energy efficiency. Please save the date for our awards ceremony on April 29, 2014. Ceremony registration information will be available on this website in January 2014. If you have any questions, please contact Rebecca Hudson, at

42

STAR Test Environment  

NLE Websites -- All DOE Office Websites (Extended Search)

STAR Test Environment STAR Test Environment STAR Test Environment These instructions describe how to set up the STAR environment independent of the production environment in order to test different installations in $OPTSTAR and $GROUP_DIR. If you want to modify those installations you will need access to the starofl account. Bypass STAR envionment login Edit your ~/.pdsf_setup file changing the STAR_LINUX_SETUP to "use_none" and start a new session. You should not see all the STAR environmental variables defined when you do this (and it will probably be much quicker than usual, too). Do a manual STAR login If you want to modify what test environment you use copy the test login scripts to your own working area: cp -r /common/star/startest /path/to/myworkdir/. If you don't want to modify these files you can source them directly from

43

ENERGY STAR Challenge  

NLE Websites -- All DOE Office Websites (Extended Search)

STAR Challenge STAR Challenge for Industry Participant Handbook June 2013 ENERGY STAR is a U.S. Environmental Protection Agency Program helping organizations and individuals fight climate change through superior energy efficiency. Learn more at energystar.gov/buildings. 2 Contents Overview ............................................................................................................................. 3 Participation Eligibility .......................................................................................................... 4 How to Participate ............................................................................................................... 5 Step 1: Establish an energy intensity metric ................................................................ 5

44

Maintaining STAR - Hanford Site  

NLE Websites -- All DOE Office Websites (Extended Search)

VPP Hanford Site Champions Committee Getting Started Maintaining STAR VPP CampaignPosters VPP Tools VPP Presentations VPP Awareness VPP Communications VPP Conferences...

45

Star-ND (Multi-Dimensional Star-Identification)  

E-Print Network (OSTI)

In order to perform star-identification with lower processing requirements, multi-dimensional techniques are implemented in this research as a database search as well as to create star pattern parameters. New star pattern parameters are presented...

Spratling, Benjamin

2012-07-16T23:59:59.000Z

46

ENERGY STAR certification | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR certification ENERGY STAR certification 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 How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Facts and stats Climate change and buildings ENERGY STAR certification

47

Neutron Stars and Fractal Dimensionality  

E-Print Network (OSTI)

We argue that the material inside Neutron stars behaves anomalously with fractal statistics and that in principle, we could induce mini Neutron stars, with the release of energy.

Burra G. Sidharth

2008-05-06T23:59:59.000Z

48

Carbon Stars | Open Energy Information  

Open Energy Info (EERE)

Stars Jump to: navigation, search Name: Carbon Stars Place: Netherlands Sector: Services Product: General Financial & Legal Services ( Private family-controlled ) References:...

49

Home : ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Who dared imagine? Who dared imagine? Our newest video celebrates 20 years of success with our innovative ENERGY STAR partners. See the Video EPA Logo ENERGY STAR is a U.S. Environmental Protection Agency voluntary program that helps businesses and individuals save money and protect our climate through superior energy efficiency. Learn more about ENERGY STAR. A comprehensive review of ENERGY STAR and other EPA climate protection partnerships. See 2011 Annual Report. Basic information on climate change, greenhouse gas emissions, and climate change science. See Climate Change. With help from ENERGY STAR, by 2012, Americans had cumulatively prevented more than 1.8 billion metric tons of GHG emissions. See 2012 Achievements. Energy Efficiency For Your Home

50

Dark Stars: A Review  

E-Print Network (OSTI)

Dark Stars (DS) are stellar objects made (almost entirely) of ordinary atomic material but powered by the heat from Dark Matter (DM) annihilation (rather than by fusion). Weakly Interacting Massive Particles (WIMPs), among the best candidates for DM, can be their own antimatter and can accumulate inside the star, with their annihilation products thermalizing with and heating the DS. The resulting DSs are in hydrostatic and thermal equilibrium. The first phase of stellar evolution in the history of the Universe may have been dark stars. Though DM constituted only $power the star for millions to billions of years. Depending on their DM environment, early DSs can become very massive ($>10^6 M_\\odot$), very bright ($>10^9 L_\\odot$), and potentially detectable with the James Webb Space Telescope (JWST). Once the DM runs out and the dark star dies, it may collapse to a black hole; thus DSs can provide seeds for the supermassive black holes observed throughout the Universe and at early times. Other sites for dark star formation exist in the Universe today in regions of high dark matter density such as the centers of galaxies. The current review briefly discusses DSs existing today but focuses on the early generation of dark stars.

Katherine Freese; Tanja Rindler-Daller; Douglas Spolyar; Monica Valluri

2015-01-10T23:59:59.000Z

51

Leading organizations choose ENERGY STAR | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Leading organizations choose ENERGY STAR Leading organizations choose ENERGY STAR 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 design to earn ENERGY STAR Leading organizations choose ENERGY STAR Sell others on the idea of ENERGY STAR An overview of the ENERGY STAR lifecycle Design to earn ENERGY STAR Leading organizations choose ENERGY STAR Facebook's data center achieved Designed to Earn the ENERGY STAR More than

52

Hyperons in neutron stars  

E-Print Network (OSTI)

Using the Dirac-Brueckner-Hartree-Fock approach, the properties of neutron-star matter including hyperons are investigated. In the calculation, we consider both time and space components of the vector self-energies of baryons as well as the scalar ones. Furthermore, the effect of negative-energy states of baryons is partly taken into account. We obtain the maximum neutron-star mass of $2.08\\,M_{\\odot}$, which is consistent with the recently observed, massive neutron stars. We discuss a universal, repulsive three-body force for hyperons in matter.

Katayama, Tetsuya

2015-01-01T23:59:59.000Z

53

On the conversion of neutron stars into quark stars  

E-Print Network (OSTI)

The possible existence of two families of compact stars, neutron stars and quark stars, naturally leads to a scenario in which a conversion process between the two stellar objects occurs with a consequent release of energy of the order of $10^{53}$ erg. We discuss recent hydrodynamical simulations of the burning process and neutrino diffusion simulations of cooling of a newly formed strange star. We also briefly discuss this scenario in connection with recent measurements of masses and radii of compact stars.

Giuseppe Pagliara

2013-12-04T23:59:59.000Z

54

Nuclear Reactions in Stars  

Science Journals Connector (OSTI)

21 February 1961 research-article Nuclear Reactions in Stars T. G. Cowling Thermonuclear reactions important for the generation of stellar energy during different phases of stellar evolution are discussed. The Royal...

1961-01-01T23:59:59.000Z

55

Neutron stars - thermal emitters  

E-Print Network (OSTI)

Confronting theoretical models with observations of thermal radiation emitted by neutron stars is one of the most important ways to understand the properties of both, superdense matter in the interiors of the neutron stars and dense magnetized plasmas in their outer layers. Here we review the theory of thermal emission from the surface layers of strongly magnetized neutron stars, and the main properties of the observational data. In particular, we focus on the nearby sources for which a clear thermal component has been detected, without being contaminated by other emission processes (magnetosphere, accretion, nebulae). We also discuss the applications of the modern theoretical models of the formation of spectra of strongly magnetized neutron stars to the observed thermally emitting objects.

Potekhin, A Y; Pons, J A

2014-01-01T23:59:59.000Z

56

Masers and star formation  

E-Print Network (OSTI)

Recent observational and theoretical advances concerning astronomical masers in star forming regions are reviewed. Major masing species are considered individually and in combination. Key results are summarized with emphasis on present science and future prospects.

Vincent L. Fish

2007-04-02T23:59:59.000Z

57

Holographic Neutron Stars  

E-Print Network (OSTI)

We construct in the context of the AdS/CFT correspondence degenerate composite operators in the conformal field theory that are holographically dual to degenerate stars in anti de Sitter space. We calculate the effect of the gravitational back-reaction using the Tolman-Oppenheimer-Volkoff equations, and determine the "Chandrasekhar limit" beyond which the star undergoes gravitational collapse towards a black hole.

Jan de Boer; Kyriakos Papadodimas; Erik Verlinde

2009-07-16T23:59:59.000Z

58

ENERGY STAR industrial partnership | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR industrial partnership ENERGY STAR industrial partnership 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance ENERGY STAR industrial partnership New ENERGY STAR industrial partners Energy guides Energy efficiency and air regulation

59

Use ENERGY STAR benchmarking tools | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Use ENERGY STAR benchmarking tools Use ENERGY STAR benchmarking tools 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use Learn about benchmarking Use ENERGY STAR benchmarking tools ENERGY STAR in action Communicate and educate

60

Star Power | Princeton Plasma Physics Lab  

NLE Websites -- All DOE Office Websites (Extended Search)

Star Power Star Power The U.S. Department of Energy's Princeton Plasma Physics Laboratory has released "Star Power," a new informational video that uses dramatic and beautiful...

Note: This page contains sample records for the topic "waha lone star" 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

ENERGY STAR | Open Energy Information  

Open Energy Info (EERE)

ENERGY STAR ENERGY STAR Jump to: navigation, search Logo: ENERGY STAR Name ENERGY STAR Year founded 1992 Notes Partnered with more than 20,000 public sector organizations. Website https://www.energystar.gov/ind References About ENERGY STAR[1] LinkedIn Connections Contents 1 About ENERGY STAR 1.1 For the Home 1.2 For Business 1.3 References About ENERGY STAR ENERGY STAR is a joint program of the U.S. Environmental Protection Agency and the U.S. Department of Energy helping us all save money and protect the environment through energy efficient products and practices. Results are already adding up. Americans, with the help of ENERGY STAR, saved enough energy in 2010 alone to avoid greenhouse gas emissions equivalent to those from 33 million cars - all while saving nearly $18 billion on their

62

Dark Stars: A Review  

E-Print Network (OSTI)

Dark Stars (DS) are stellar objects made (almost entirely) of ordinary atomic material but powered by the heat from Dark Matter (DM) annihilation (rather than by fusion). Weakly Interacting Massive Particles (WIMPs), among the best candidates for DM, can be their own antimatter and can accumulate inside the star, with their annihilation products thermalizing with and heating the DS. The resulting DSs are in hydrostatic and thermal equilibrium. The first phase of stellar evolution in the history of the Universe may have been dark stars. Though DM constituted only $10^6 M_\\odot$), very bright ($>10^9 L_\\odot$), and potentially detectable with the James Webb Space Telescope (JWST). Once the DM runs out and the dark star dies, it may collapse to a black hole; thus DSs can provide seeds for the supermassive black holes observed throughout the Universe and at early times. Other sites for dark star formation exist in the Universe today in regions of high dark matter density such as the centers of galaxies. The curre...

Freese, Katherine; Spolyar, Douglas; Valluri, Monica

2015-01-01T23:59:59.000Z

63

Cooling of neutron stars  

Science Journals Connector (OSTI)

On the basis of current physical understanding, it is impossible to predict with confidence the interior constitution of neutron stars. Cooling of neutron stars provides a possible way of discriminating among possible states of matter within them. In the standard picture of cooling by neutrino emission developed over the past quarter of a century, neutron stars are expected to cool relatively slowly if their cores are made up of nucleons, and to cool faster if matter is in an exotic state, such as a pion condensate, a kaon condensate, or quark matter. This view has recently been called into question by the discovery of a number of other processes that could lead to copious neutrino emission and rapid cooling.

C. J. Pethick

1992-10-01T23:59:59.000Z

64

On the efficiency of field star capture by star clusters  

E-Print Network (OSTI)

An exciting recent finding regarding scaling relations among globular clusters is the so-called 'blue tilt': clusters of the blue sub-population follow a trend of redder colour with increasing luminosity. In this paper we evaluate to which extent field star capture over a Hubble time may explain the 'blue tilt'. We perform collisional N-body simulations to quantify the amount of field star capture occuring over a Hubble time to star clusters with 10^3 to 10^6 stars. In the simulations we follow the orbits of field stars passing through a star cluster and calculate the energy change that the field stars experience due to gravitational interaction with cluster stars during one passage through the cluster. The capture condition is that their total energy after the passage is smaller than the gravitational potential at the cluster's tidal radius. By folding this with the fly-by rates of field stars with an assumed space density as in the solar neighbourhood and a range of velocity dispersions, we derive estimates on the mass fraction of captured field stars as a function of environment. We find that integrated over a Hubble time, the ratio between captured field stars and total number of clusters stars is very low (capture is not a probable mechanism for creating the colour-magnitude trend of metal-poor globular clusters.

Steffen Mieske; Holger Baumgardt

2007-09-10T23:59:59.000Z

65

A Star on Earth  

ScienceCinema (OSTI)

At the Energy Department's Princeton Plasma Physics Lab, scientists are trying to accomplish what was once considered the realm of science fiction: create a star on Earth. The National Spherical Torus Experiment (NSTX) is a magnetic fusion device that is used to study the physics principles of spherically shaped plasmas -- hot ionized gases in which, under the right conditions, nuclear fusion will occur. Fusion is the energy source of the sun and all of the stars. Not just limited to theoretical work, the NSTX is enabling cutting-edge research to develop fusion as a future energy source.

Prager, Stewart; Zwicker, Andrew; Hammet, Greg; Tresemer, Kelsey; Diallo, Ahmed

2014-06-06T23:59:59.000Z

66

A Star on Earth  

SciTech Connect

At the Energy Department's Princeton Plasma Physics Lab, scientists are trying to accomplish what was once considered the realm of science fiction: create a star on Earth. The National Spherical Torus Experiment (NSTX) is a magnetic fusion device that is used to study the physics principles of spherically shaped plasmas -- hot ionized gases in which, under the right conditions, nuclear fusion will occur. Fusion is the energy source of the sun and all of the stars. Not just limited to theoretical work, the NSTX is enabling cutting-edge research to develop fusion as a future energy source.

Prager, Stewart; Zwicker, Andrew; Hammet, Greg; Tresemer, Kelsey; Diallo, Ahmed

2014-03-05T23:59:59.000Z

67

Star Biomass | Open Energy Information  

Open Energy Info (EERE)

India Sector: Biomass Product: Plans to set up biomass projects in Rajasthan. References: Star Biomass1 This article is a stub. You can help OpenEI by expanding it. Star Biomass...

68

Star clusters as diaries of galaxies  

E-Print Network (OSTI)

Most if not all stars form in star clusters. Thus the distribution of star clusters preserves the information on the star formation history of a galaxy. Massive clusters form only during episodes of high star formation activity whereas periods of low star formation activity cannot produce them. We present here the method of Maschberger & Kroupa (2007) to derive the star formation history of a galaxy from its star-cluster content.

Th. Maschberger; P. Kroupa

2007-06-11T23:59:59.000Z

69

ENERGY STAR plant certification | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

» ENERGY STAR plant certification » ENERGY STAR plant certification 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance Industrial service and product providers Earn recognition ENERGY STAR Partner of the Year Award

70

Campaigns and incentive programs that incorporate ENERGY STAR | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Campaigns and incentive programs that incorporate ENERGY STAR Campaigns and incentive programs that incorporate ENERGY STAR 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 Policies that specify the use of ENERGY STAR tools Campaigns and incentive programs that incorporate ENERGY STAR Lead by example Gather support Develop programs and policies Host a competition Use financing vehicles

71

ENERGY STAR service and product provider training series | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

service and product provider training series service and product provider training series 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 How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner ENERGY STAR service & product provider training series Service and product provider's marketing toolkit ENERGY STAR sales tools for service and product providers

72

Massive Star Outflows  

E-Print Network (OSTI)

Molecular outflows in the form of wide-angle winds and/or well-collimated jets are associated with young stellar objects of all luminosities. Independent studies have established that the mass outflow rate is proportional to L_bol^0.6 for L_bol = 0.3 to 10^5 L_sun, suggesting that there is a strong link between accretion and outflow for a wide range of source luminosity and there is reasonable evidence that accretion-related processes are responsible for generating massive molecular flows from protostars up to spectral type B0. Beyond L_bol ~ 10^4 L_sun, O stars generate powerful wide-angle, ionized winds that can dramatically affect outflow morphology and even call into question the relationship between outflow and accretion. Recently Beuther & Shepherd (2005) proposed an evolutionary scenario in which massive protostellar flows (up to early B spectral type) begin collimated. Once the star reaches the Main Sequence, ionizing radiation may affect the balance between magnetic and plasma pressure, inducing changes in the flow morphology and energetics. Here I review the properties of outflows from young OB stars, discuss implications and observational tests of this proposed evolutionary scenario, and examine differences between low-mass and massive star formation.

D. S. Shepherd

2005-06-01T23:59:59.000Z

73

Physical Processes in Stars  

Science Journals Connector (OSTI)

... : Structure and Evolution of the Stars (Princeton University Press, 1958), by M. Schwarzschild, and Physical Processes in Stellar Interiors (Israel Program for Scientific Translations, 1962), ... the years 1954-57 and there are only a few references of later date than Schwarzschild's book.

R. J. TAYLER

1964-12-05T23:59:59.000Z

74

Explosive Nucleosynthesis in Stars  

Science Journals Connector (OSTI)

... in hydrostatic equilibrium, with considerable effect on the abundances of the ejected matter. The overheating may result either from the fact that the fuels first ignite in a degenerate electron ... pressure wave propagates outward from an exploding core. In either case, large amounts of thermal energy are liberated in a time short compared with the star's ability to compensate ...

W. DAVID ARNETT; DONALD D. CLAYTON

1970-08-22T23:59:59.000Z

75

Young stars with discs  

Science Journals Connector (OSTI)

...central star. The ultraviolet excess was originally proposed to...in terms of modelling the UV excess as a contribution from a boundary...spectral features caused by lithium, calcium and iron. They report...hotspots with temperatures in excess of 5000 K, compared with the...

2000-01-01T23:59:59.000Z

76

Leading firms choose ENERGY STAR | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Leading firms choose ENERGY STAR Leading firms choose ENERGY STAR 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 Leading firms choose ENERGY STAR Why new doesn't always mean efficient Follow EPA's step-by-step process ENERGY STAR Challenge for Architects Leading firms choose ENERGY STAR Facebook data center Hundreds of leading A/E firms have already partnered

77

About ENERGY STAR for commercial and industrial buildings | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR for commercial and industrial buildings ENERGY STAR for commercial and industrial buildings 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 How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Facts and stats Climate change and buildings

78

Earn ENERGY STAR certification | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Earn ENERGY STAR certification Earn ENERGY STAR certification 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use ENERGY STAR in action Communicate and educate ENERGY STAR communications toolkit Bring Your Green to Work with ENERGY STAR

79

Lone hunger striker spurs Nepal to action  

Science Journals Connector (OSTI)

... leadership team in universities are selected by the ruling party or coalition, says Kedar Bhakta Mathema, a former vice-chancellor of TU. From executive level to department heads, ...

Smriti Mallapaty

2014-02-18T23:59:59.000Z

80

Energy Star | Open Energy Information  

Open Energy Info (EERE)

Star Star Jump to: navigation, search Energystarlogo.jpg Contents 1 What's new 2 About ENERGY STAR 3 For the Home 4 For Business 5 History 6 References What's new On March 15, 2012, the EPA released a press release announcing 2012's ENERGY STAR award winners, and celebrating the 20 year anniversary of the award. Overall, the EPA estimates that American's have saved nearly $230 billion over two decades of the award. About ENERGY STAR ENERGY STAR is a joint program of the United States Environmental Protection Agency and the United States Department of Energy helping us all save money and protect the environment through energy efficient products and practices. Results are already adding up. Americans, with the help of ENERGY STAR, saved enough energy in 2009 alone to avoid greenhouse gas emissions

Note: This page contains sample records for the topic "waha lone star" 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

Authigenic clay minerals in sandstones of the Delaware Mountain Group: Bell Canyon and Cherry Canyon Formations, Waha Field, West Texas  

E-Print Network (OSTI)

feldspars dominate over the plagioclases. Calcite is the dominant cementing mineral, though sulfate and halite cements have been observed. Hays (1992) showed that a diverse suite of authigenic minerals occurs in these sandstones, including silicate...

Walling, Suzette Denise

2012-06-07T23:59:59.000Z

82

ENERGY STAR Webinar: Financing Energy Efficient Upgrades with ENERGY STAR  

Energy.gov (U.S. Department of Energy (DOE))

Hosted by ENERGY STAR, this webinar will show how public sector organizations are improving energy efficiency with innovative solutions to financial barriers.

83

ENERGY STAR SNAPSHOT - Spring 2009  

NLE Websites -- All DOE Office Websites (Extended Search)

0 0 Snapshot data runs through June 30, 2010. Summary By mid-year 2010, commercial and industrial organizations have almost exceeded activity levels reached throughout all of 2009. From January through June 30, 2010: More than 80,000 buildings have benchmarked their energy usage with ENERGY STAR, of which 63,000 buildings received an ENERGY STAR energy performance score-nearly equivalent to the amount for all of 2009. Close to 3,200 buildings earned the ENERGY STAR label-the highest amount earned through two quarters of any year, and 80% higher than mid-year 2009. The ENERGY STAR Snapshot provides an at-a-glance summary of the latest national ENERGY STAR metrics to help you, our partners, see the impact of your efforts. The ENERGY STAR Snapshot is

84

ENERGY STAR EEPS Partnership Agreement  

NLE Websites -- All DOE Office Websites (Extended Search)

Approval expires 02/29/2016 1 EPA Form No. 5900-33 ENERGY STAR Partnership Agreement Instructions for Partnering with ENERGY STAR ® As an Energy Efficiency Program Sponsor Organizations interested in partnering with ENERGY STAR as an Energy Efficiency Program Sponsor should take the following steps: 1. Review the Energy Efficiency Program Sponsors Program Definitions and Program Requirements documents. 2. Select the area(s) of interest for a new partnership on the Participation Form. Please

85

Anisotropic charged dark energy star  

E-Print Network (OSTI)

As the stars carry electrical charges, we present in this paper a model for charged dark energy star which is singularity free. We take Krori-Barua space time. We assume that the radial pressure exerted on the system due to the presence of dark energy is proportional to the isotropic perfect fluid matter density and the difference between tangential and radial pressure is proportional to the square of the electric field intensity. The solution satisfies the physical conditions inside the star

Kanika Das; Nawsad Ali

2014-02-02T23:59:59.000Z

86

Creating a Star on Earth  

Energy.gov (U.S. Department of Energy (DOE))

At the Energy Department's Princeton Plasma Physics Lab, scientists are trying to accomplish what was once considered the realm of science fiction: creating a star on Earth.

87

Upsilon measurement in STAR  

E-Print Network (OSTI)

We present preliminary results of Upsilon production in p+p collisions at sqrt(s)=200 GeV at central rapidity. This measurement was performed at the STAR experiment through the Upsilon->e^+e^- decay channel. In this manuscript we describe the experimental details, from the development of a specially designed trigger setup to the analysis methods used to discriminate electrons from hadrons. The production cross-section obtained B*{(dsigma/dy)|(y=0)}=91(28)(22) pb is compatible with our expectations based on pQCD calculations.

Mauro R. Cosentino

2007-06-06T23:59:59.000Z

88

On Magnetized Neutron Stars  

E-Print Network (OSTI)

In this work we review the formalism normally used in the literature about the effects of density-dependent magnetic fields on the properties of neutron stars, expose some ambiguities that arise and propose a way to solve the related problem. Our approach uses a different prescription for the calculation of the pressure based on the chaotic field formalism for the stress tensor and also a different way of introducing a variable magnetic field, which depends on the energy density rather than on the baryonic density.

Lopes, Luiz L

2014-01-01T23:59:59.000Z

89

Star Canticle Issue 2  

E-Print Network (OSTI)

StA ft CANtJClt 2 * 1 1 STAR CANTICLE 2 DOTTY BARRY PRICE: P.O. BOX 921 $5.50 1st class CLAREMONT, CA 91711 4.50 book rate CON TEN TS 2 Prelude 3 Poetry ?Untitled Dotty Barry k Fiction ?"Scotty? s Decision" Joy Mancinelli 6.... .Poetry..." Rayelle Roe m Poetry ?"Shouldn't You Ask Me First?" .Susan Meek k>2 Poetry ?"Storm Haven" Ellen Kobrin ^3 Poetry ?"Fire and Ice" ? ? .Gerry Downes kk Fiction ?"Viewpoint" Kay McElvain ty Poetry ?"Threads" Susan Burr 48 Poetry ?"The Starless Sky" Liz...

Multiple Contributors

1979-01-01T23:59:59.000Z

90

Cost Update, STAR-TOFp Implementation STAR-TOFp Group  

E-Print Network (OSTI)

Cost Update, STAR-TOFp Implementation STAR-TOFp Group November 22, 1999 Abstract This document updates the cost sections of the TOFp Implementation Plan. In this update1 to the TOFp Implementation plan of Oct. 5, 1999,2 the cost estimates based on the latest quotes and the nal design are discussed

Llope, William J.

91

Physics of Neutron Star Crusts  

E-Print Network (OSTI)

The physics of neutron star crusts is vast, involving many different research fields, from nuclear and condensed matter physics to general relativity. This review summarizes the progress, which has been achieved over the last few years, in modeling neutron star crusts, both at the microscopic and macroscopic levels. The confrontation of these theoretical models with observations is also briefly discussed.

N. Chamel; P. Haensel

2008-12-20T23:59:59.000Z

92

Wind from T Tauri Stars  

Science Journals Connector (OSTI)

......December 1998 research-article Papers 8680 Wind from T Tauri Stars Masayoshi Kiguchi Shinji...was shown by DeCampli that an isothermal wind of T Tauri stars cannot explain both the...Since the assumption of an isothermal wind does not hold in general, we recalculated......

Masayoshi Kiguchi; Shinji Narita; Chushiro Hayashi

1998-12-01T23:59:59.000Z

93

Verifying the ENERGY STAR Certification Application  

Energy.gov (U.S. Department of Energy (DOE))

Do you verify commercial building applications for ENERGY STAR certification? This webinar, based on the ENERGY STAR Guide for Licensed Professionals, covers the role of the licensed professional,...

94

Christmas burst reveals neutron star collision  

NLE Websites -- All DOE Office Websites (Extended Search)

Christmas burst reveals neutron star collision Christmas burst reveals neutron star collision Called the Christmas Burst, GRB 101225A was freakishly lengthy and it produced...

95

ENERGY STAR Snapshot Spring 2012  

NLE Websites -- All DOE Office Websites (Extended Search)

Spring 2012 Spring 2012 Snapshot data runs through December 31, 2011. The ENERGY STAR Snapshot provides an at-a-glance summary of the latest national ENERGY STAR metrics to help you, our partners, see the impact of your efforts. The ENERGY STAR Snapshot is distributed twice a year and provides: * Trends in energy benchmarking of commercial and industrial buildings. * State-by-state activity along with activity for the top Designated Market Areas. * Industrial sector participation in ENERGY STAR. * Trends in ENERGY STAR certified commercial and industrial facilities. Summary By the end of calendar year 2011, commercial and industrial organizations exceeded figures for benchmarking and certification that were achieved in 2010. Since June, 2011:

96

Sample ENERGY STAR performance documents | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Existing buildings Existing buildings » Use Portfolio Manager » Verify and document your savings » Sample ENERGY STAR performance documents 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 Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit

97

ENERGY STAR Focus on Energy Efficiency in Metalcasting | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Metalcasting Metalcasting 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Tools for benchmarking energy management practices Tools for tracking and benchmarking facility energy performance ENERGY STAR Energy Performance Indicators for plants

98

ENERGY STAR certification for your building | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

certification for your building certification for your building 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 Learn the benefits Get started Use Portfolio Manager Save energy Find financing Earn recognition 20-percent recognition ENERGY STAR certification How to apply for ENERGY STAR certification Tips for low-cost verifications Submit a profile of your building

99

ENERGY STAR Building Upgrade Manual | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR Building Upgrade Manual ENERGY STAR Building Upgrade Manual 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 Learn the benefits Get started Use Portfolio Manager Save energy Stamp out energy waste Find cost-effective investments Engage occupants Purchase energy-saving products Put computers to sleep Get help from an expert Take a comprehensive approach

100

Portfolio Manager Technical Reference: ENERGY STAR Score | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR Score ENERGY STAR Score 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 Success stories Target Finder Technical documentation

Note: This page contains sample records for the topic "waha lone star" 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.


101

The evolution of star clusters: The resolved-star approach  

E-Print Network (OSTI)

We present the first results of a new technique to detect, locate, and characterize young dissolving star clusters. Using HST/ACS archival images of the nearby galaxy IC2574, we performed stellar PSF photometry and selected the most massive stars as our first test sample. We used a group-finding algorithm on the selected massive stars to find cluster candidates. We then plot the color-magnitude diagrams for each group, and use stellar evolutionary models to estimate their age. So far, we found 79 groups with ages of up to about 100 Myr, displaying various sizes and densities.

Anne Pellerin; Martin J. Meyer; Jason Harris; Daniela Calzetti

2008-02-29T23:59:59.000Z

102

ENERGY STAR Webinar: Financing Energy Efficient Upgrades with ENERGY STAR  

Energy.gov (U.S. Department of Energy (DOE))

ENERGY STAR is hosting a webinar on how public sector organizations are improving energy efficiency with innovative solutions to financial barriers on Oct. 21, 2014, from 2:00 p.m. - 3:15 p.m.

103

EPA ENERGY STAR Webinar: ENERGY STAR Portfolio Manager 201  

Energy.gov (U.S. Department of Energy (DOE))

Continue to learn about EPAs ENERGY STAR Portfolio Manager tool, with a deeper dive into more advanced functionalities such as: managing and tracking changes to your property uses over time; using...

104

EPA ENERGY STAR Webcast: Value of ENERGY STAR Certification  

Office of Energy Efficiency and Renewable Energy (EERE)

For thousands of organizations, ENERGY STAR is the simple choice for saving money and demonstrating environmental leadership to the public. Lower energy costs aren't the only financial benefit of...

105

ENERGY STAR Challenge for Industry  

NLE Websites -- All DOE Office Websites (Extended Search)

Industrial Plant Industrial Plant Certification Professional Engineers' Guide for Validating Statements of Energy Performance Office of Air and Radiation Climate Protection Partnerships Division June 2013 ii Introduction The U.S. Environmental Protection Agency's ENERGY STAR program provides guidance, tools, and recognition to help companies improve the energy performance of their facilities and strengthen the effectiveness of their energy management program. Through ENERGY STAR, the U.S. Environmental Protection Agency (EPA) offers a number of forms of recognition, including certification for facility energy efficiency. ENERGY STAR certification for industrial plants recognizes individual manufacturing plants whose

106

A Heavy Flavor Tracker for STAR  

SciTech Connect

We propose to construct a Heavy Flavor Tracker (HFT) for the STAR experiment at RHIC. The HFT will bring new physics capabilities to STAR and it will significantly enhance the physics capabilities of the STAR detector at central rapidities. The HFT will ensure that STAR will be able to take heavy flavor data at all luminosities attainable throughout the proposed RHIC II era.

Xu, Z.; Chen, Y.; Kleinfelder, S.; Koohi, A.; Li, S.; Huang, H.; Tai, A.; Kushpil, V.; Sumbera, M.; Colledani, C.; Dulinski, W.; Himmi,A.; Hu, C.; Shabetai, A.; Szelezniak, M.; Valin, I.; Winter, M.; Surrow,B.; Van Nieuwenhuizen, G.; Bieser, F.; Gareus, R.; Greiner, L.; Lesser,F.; Matis, H.S.; Oldenburg, M.; Ritter, H.G.; Pierpoint, L.; Retiere, F.; Rose, A.; Schweda, K.; Sichtermann, E.; Thomas, J.H.; Wieman, H.; Yamamoto, E.; Kotov, I.

2005-03-14T23:59:59.000Z

107

X-ray Emission from Massive Stars  

E-Print Network (OSTI)

X-ray Emission from Massive Stars David Cohen Department of Physics and Astronomy Swarthmore be related to the production of X-rays on massive stars. If so, massive stars' X-rays are much different than those found our own Sun and other cooler stars like the Sun that produce X-rays via magnetic activity

Cohen, David

108

ENERGY STAR Challenge for Industry  

NLE Websites -- All DOE Office Websites (Extended Search)

Challenge Challenge for Industry Professional Engineers' Guide for Validating Statements of Energy Improvement Office of Air and Radiation Climate Protection Partnerships Division May 2013 Revised ii Introduction The U.S. Environmental Protection Agency's (U.S. EPA) ENERGY STAR program provides guidance, tools, and recognition to help companies improve their energy performance. ENERGY STAR is a voluntary partnership program that companies choose to join. Through ENERGY STAR, U.S. EPA offers a number of forms of recognition for achievements in energy efficiency. The ENERGY STAR Challenge for Industry recognizes individual industrial sites for achieving a 10 percent reduction in energy intensity within 5 years from the conclusion of an established baseline. To be

109

Appendix 5 - STARS Architectual Overview  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Last saved by Coombs Page 1 7/27/2012 Last saved by Coombs Page 1 7/27/2012 Draft Appendix 5 - STARS Architectural Overview ARC101 - Architectural Overview for Department of Energy iManage Program - STARS Project Deliverable ID: IT0013 Version number: 1.09 Draft/Final as of: 18 Oct 2005 Printed on: 27 Jul 2012 Author: Richard Popovich, STARS System Architect Richard.Popovich@hq.doe.gov (301) 903-2223 Owner: Laura Kramer, STARS Project Manager Status of Document Draft Delivered Accepted Last saved by Coombs Page 2 7/27/2012 Draft Document information Document source This document is maintained as an online document. Contact the author for the latest version. Revision history Version number Date Summary of changes Revised By 1.01 08 Jul 03 Version 1 Richard Popovich,

110

New subdwarf B star periods  

E-Print Network (OSTI)

Subdwarf B (sdB) stars are thought to be helium burning stars with low mass hydrogen envelopes. Several evolutionary paths have been proposed to explain the formation of these systems. One of these scenarios is the evolution of the sdB progenitor within a binary system. We have looked systematically at bright sdB stars from the PG survey. By taking spectra at several different epochs we have measured the radial velocity shifts caused by the motion of the sdB star within the binary. Our data have been taken over a long time base line (2 years) which allowed us to find longer period binaries than known before. Here we present results for 29 sdB systems.

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

2002-09-26T23:59:59.000Z

111

Neutron skins and neutron stars  

Science Journals Connector (OSTI)

Background: The neutron skin of a heavy nucleus as well as many neutron-star properties are highly sensitive to the poorly constrained density dependence of the symmetry energy.Purpose: To provide for the first time meaningful theoretical errors and to assess the degree of correlation between the neutron-skin thickness of 208Pb and several neutron-star properties.Methods: A proper covariance analysis based on the predictions of an accurately calibrated relativistic functional FSUGold is used to quantify theoretical errors and correlation coefficients.Results: We find correlation coefficients of nearly 1 (or ?1) between the neutron-skin thickness of 208Pb and a host of observables of relevance to the structure, dynamics, and composition of neutron stars.Conclusions: We suggest that a follow-up Lead Radius Experiment (PREX) measurement, ideally with a 0.5% accuracy, could significantly constrain the equation of state of neutron-star matter.

F. J. Fattoyev and J. Piekarewicz

2012-07-05T23:59:59.000Z

112

ENERGY STAR Portfolio Manager 101  

Office of Energy Efficiency and Renewable Energy (EERE)

Join us as we introduce and demonstrate the core functionality of EPAs ENERGY STAR Portfolio Manager tool. Attendees will learn how to: navigate Portfolio Manager; add a property and enter details...

113

ENERGY STAR Portfolio Manager 201  

Office of Energy Efficiency and Renewable Energy (EERE)

Continue to learn about EPAs new ENERGY STAR Portfolio Manager tool, with a deeper dive into more advanced functionalities such as: managing and tracking changes to your property uses over time;...

114

Inversion of the star transform  

E-Print Network (OSTI)

We define the star transform as a generalization of the broken ray transform introduced by us in previous work. The advantages of using the star transform include the possibility to reconstruct the absorption and the scattering coefficients of the medium separately and simultaneously (from the same data) and the possibility to utilize scattered radiation which, in the case of the conventional X-ray tomography, is discarded. In this paper, we derive the star transform from physical principles, discuss its mathematical properties and analyze numerical stability of inversion. In particular, it is shown that stable inversion of the star transform can be obtained only for configurations involving odd number of rays. Several computationally-efficient inversion algorithms are derived and tested numerically.

Fan Zhao; John C. Schotland; Vadim A. Markel

2014-05-06T23:59:59.000Z

115

Shooting Star | Open Energy Information  

Open Energy Info (EERE)

Shooting Star Shooting Star Jump to: navigation, search Name Shooting Star Facility Shooting Star Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Exelon Wind Developer Infinity Wind Power Energy Purchaser Sunflower Electric Power Corporation Location Greensburg KS Coordinates 37.55019151°, -99.27585125° 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":37.55019151,"lon":-99.27585125,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

116

STAR Vertex Detector Upgrade Development  

SciTech Connect

We report on the development and prototyping efforts undertaken with the goal of producing a micro-vertex detector for the STAR experiment at the RHIC accelerator at BNL. We present the basic detector requirements and show a sensor development path, conceptual mechanical design candidates and readout architecture. Prototyping and beam test results with current generation MimoSTAR-2 sensors and a readout system featuring FPGA based on-the-fly hit finding and data sparsification are also presented.

Greiner, Leo C.; Matis, Howard S.; Stezelberger, Thorsten; Vu,Chinh Q.; Wieman, Howard; Szelezniak, Michal; Sun, Xiangming

2008-01-28T23:59:59.000Z

117

GRBs from the First Stars  

SciTech Connect

We present an estimate of the Gamma Ray Bursts which should be expected from metal-free, elusive first generation of stars known as PopulationIII (PopIII). We derive the GRB rate from these stars from the Stellar Formation Rate obtained in several Reionization scenarios available in the literature. In all of the analyzed models we find that GRBs from PopIII are subdominant with respect to the ''standard'' (PopII) ones up to z {approx} 10.

Iocco, Fabio; /Naples U. /KIPAC, Menlo Park

2007-04-16T23:59:59.000Z

118

Magnesium Isotopes in Halo Stars  

E-Print Network (OSTI)

We have determined Mg isotope ratios in halo field dwarfs and giants in the globular cluster M71 based on high S/N high spectral resolution (R = 10$^5$) Keck HIRES spectra. Unlike previous claims of an important contribution from intermediate-mass AGB stars to the Galactic halo, we find that our $^{26}$Mg/$^{24}$Mg ratios can be explained by massive stars.

Jorge Melendez; Judith G. Cohen

2007-08-29T23:59:59.000Z

119

Upsilon Productions at STAR  

E-Print Network (OSTI)

The $\\Upsilon(1S+2S+3S)\\to e^{+}e^{-}$ cross section is measured at mid-rapidity ($y$) in $p+p$ collisions and in d$+Au$ collisions at center-of-mass energy $\\sqrt{s}$ = 200 GeV with the STAR detector at RHIC. In $p+p$, the measured cross section is found to be consistent with the world data trend as a function of $\\sqrt{s}$, in agreement with the Color Evaportaion Model (CEM), and underestimated by the Color Singlet Model (CSM) up to the Next-to-Leading-Order Quantum Chromodynamics (NLO QCD) calculations. In d+$Au$, the measured cross section is in agreement with the CEM prediction with anti-shadowing effects, and the nuclear modification factor indicates that $\\Upsilon(1S+2S+3S)$ production follows binary scaling within the current uncertainties. These measurements provide a benchmark for the future measurements of $\\Upsilon$ production in $Au+Au$ collisions.

A. M. Hamed

2010-05-22T23:59:59.000Z

120

PIA - I-Manage STARS | Department of Energy  

Energy Savers (EERE)

STARS PIA - I-Manage STARS PIA - I-Manage STARS More Documents & Publications PIA - INL PeopleSoft - Human Resource System PIA - Human Resources - Personal Information Change...

Note: This page contains sample records for the topic "waha lone star" 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

Intirion: ENERGY STAR Referral (MFRA-4GF) | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

specification. Intirion: ENERGY STAR Referral (MFRA-4GF) More Documents & Publications Samsung: ENERGY STAR Referral (RF26VAB) Friedrich: ENERGY STAR Referral (CP15F10) Friedrich:...

122

DOE Verification Testing in Support of ENERGY STAR, April 22...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Verification Testing in Support of ENERGY STAR, April 22, 2011 DOE Verification Testing in Support of ENERGY STAR, April 22, 2011 This document describes ENERGY STAR verificaion...

123

ENERGY STAR Test Procedures and Verification | Department of...  

Energy Savers (EERE)

Appliance & Equipment Standards ENERGY STAR ENERGY STAR Test Procedures and Verification ENERGY STAR Test Procedures and Verification The Department of Energy (DOE) is the...

124

Wave Star Energy | Open Energy Information  

Open Energy Info (EERE)

Star Energy Star Energy Jump to: navigation, search Name Wave Star Energy Place Denmark Zip DK-2920 Product Denmark-based private wave device developer. References Wave Star Energy[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This company is listed in the Marine and Hydrokinetic Technology Database. This company is involved in the following MHK Projects: Wave Star Energy 1 10 Scale Model Test This company is involved in the following MHK Technologies: C5 WaveStar This article is a stub. You can help OpenEI by expanding it. Wave Star Energy is a company located in Denmark . References ↑ "Wave Star Energy" Retrieved from "http://en.openei.org/w/index.php?title=Wave_Star_Energy&oldid=678928" Categories: Clean Energy Organizations

125

Shear viscosity in hybrid stars  

Science Journals Connector (OSTI)

A study of the shear viscosity of hadrons and quarks in hybrid stars has been performed in the framework of the microscopic transport theory. The neutron-star structure has been determined employing the equation of state from the Brueckner theory with three-body force for the hadron phase, and the equation of state from the MIT bag model for the deconfined quark phase. The nucleon-nucleon cross sections in dense matter have been consistently calculated from the Brueckner G matrix, whereas for the quark-quark cross sections the perturbative QCD has been adopted. Despite that the quark contribution to the shear viscosity is quite small at low temperature, the transition to the deconfined phase makes the equation of state much softer with the result that the baryon viscosity turns out to be enhanced instead of reduced in hybrid stars. The damping time scale of r-modes due to the shear viscosity has been evaluated for several stable configurations of a hybrid star and compared with the neutron-star spin-down time scale induced by the emission gravitation radiation from the r-modes. The enhancement of the total viscosity makes the viscosity time scale comparable with the gravitation radiation one at low temperature.

D. Jaccarino; S. Plumari; V. Greco; U. Lombardo; A. B. Santra

2012-05-03T23:59:59.000Z

126

The Star Formation History of NGC 6822  

E-Print Network (OSTI)

Images of five fields in the Local Group dwarf irregular galaxy NGC 6822 obtained with the {\\it Hubble Space Telescope} in the F555W and F814W filters are presented. Photometry for the stars in these images was extracted using the Point-Spread-Function fitting program HSTPHOT/MULTIPHOT. The resulting color-magnitude diagrams reach down to $V\\approx26$, a level well below the red clump, and were used to solve quantitatively for the star formation history of NGC 6822. Assuming that stars began forming in this galaxy from low-metallicity gas and that there is little variation in the metallicity at each age, the distribution of stars along the red giant branch is best fit with star formation beginning in NGC 6822 12-15 Gyr ago. The best-fitting star formation histories for the old and intermediate age stars are similar among the five fields and show a constant or somewhat increasing star formation rate from 15 Gyr ago to the present except for a possible dip in the star formation rate from 3 to 5 Gyr ago. The main differences among the five fields are in the higher overall star formation rate per area in the bar fields as well as in the ratio of the recent star formation rate to the average past rate. These variations in the recent star formation rate imply that stars formed within the past 0.6 Gyr are not spatially very well mixed throughout the galaxy.

Ted K. Wyder

2001-07-31T23:59:59.000Z

127

SNAPSHOT … THE ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Fall 2008 Introduction At mid-year 2008*, commercial and industrial (C&I) leaders continued to make great progress in their efforts to improve energy efficiency and reduce greenhouse gas emissions across their buildings and facilities. In the first six months of 2008, key indicators of progress have already exceeded activity levels from 2007. More than 1,500 organizations and individuals now participate in the ENERGY STAR Challenge Close to 2 billion new square feet of commercial building floor space rated in the first half of the year bringing the total to about 9.5 billion over 71,000 buildings Labels awarded through June 2008 almost equal the 2007 total, with about 5,000 facilities now qualified as ENERGY STAR ENERGY STAR Leader activity on the rise this year; almost 60 commercial partners achieved key

128

ENERGY STAR Score for Warehouses  

NLE Websites -- All DOE Office Websites (Extended Search)

Warehouses in the United States Page 1 Warehouses in the United States Page 1 ENERGY STAR Score for Warehouses in the United States Technical Reference OVERVIEW The ENERGY STAR Score for warehouses applies to unrefrigerated or refrigerated buildings that are used to store goods, manufactured products, merchandise or raw materials. The objective of the ENERGY STAR score is to provide a fair assessment of the energy performance of a property relative to its peers, taking into account the climate, weather, and business activities at the property. To identify the aspects of building activity that are significant drivers of energy use and then normalize for those factors, a statistical analysis of the peer building population is

129

Neutron skins and neutron stars  

SciTech Connect

The neutron-skin thickness of heavy nuclei provides a fundamental link to the equation of state of neutron-rich matter, and hence to the properties of neutron stars. The Lead Radius Experiment ('PREX') at Jefferson Laboratory has recently provided the first model-independence evidence on the existence of a neutron-rich skin in {sup 208}Pb. In this contribution we examine how the increased accuracy in the determination of neutron skins expected from the commissioning of intense polarized electron beams may impact the physics of neutron stars.

Piekarewicz, J. [Department of Physics, Florida State University, Tallahassee, FL 32306-4350 (United States)

2013-11-07T23:59:59.000Z

130

Nuclear Physics of Neutron Stars  

E-Print Network (OSTI)

Understanding the equation of state (EOS) of cold nuclear matter, namely, the relation between the pressure and energy density, is a central goal of nuclear physics that cuts across a variety of disciplines. Indeed, the limits of nuclear existence, the collision of heavy ions, the structure of neutron stars, and the dynamics of core-collapse supernova, all depend critically on the equation of state of hadronic matter. In this contribution I will concentrate on the special role that nuclear physics plays in constraining the EOS of cold baryonic matter and its impact on the properties of neutron stars.

J. Piekarewicz

2009-01-28T23:59:59.000Z

131

Towards a realistic axion star  

E-Print Network (OSTI)

In this work we estimate the radius and the mass of a self-gravitating system made of axions. The quantum axion field satisfies the Klein-Gordon equation in a curved space-time and the metric components of this space-time are solutions to the Einstein equations with a source term given by the vacuum expectation value of the energy-momentum operator constructed from the axion field. As a first step towards an axion star we consider the up to the sixth term in the axion potential expansion. We found that axion stars would have masses of the order of asteroids and radius of the order of few centimeters.

J. Barranco; A. Bernal

2008-08-01T23:59:59.000Z

132

Beryllium abundances in metal-poor stars  

Science Journals Connector (OSTI)

......standard big bang nucleosynthesis. Be cannot be produced by nuclear fusion in the interiors of stars; in contrast, Be would be...model of Allen Santillan (1991) for our sample stars. Input parameters, such as radial velocities, parallaxes and......

K. F. Tan; J. R. Shi; G. Zhao

2009-01-01T23:59:59.000Z

133

Cold quark matter in compact stars  

SciTech Connect

We used an equation of state for the cold quark matter to the study of properties of quark stars. We also discuss the absolute stability of quark matter and compute the mass-radius relation for self-bound stars.

Franzon, B.; Fogaca, D. A.; Navarra, F. S. [Instituto de Fisica, Universidade de Sao Paulo Rua do Matao, Travessa R, 187, 05508-090 Sao Paulo, SP (Brazil); Horvath, J. E. [Instituto de Astronomia, Geofisica e Ciencias Atmosfericas, Universidade de Sao Paulo, Rua do Matao, 1226, 05508-090, Sao Paulo, SP (Brazil)

2013-03-25T23:59:59.000Z

134

Haier: ENERGY STAR Referral (ESA408J)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Haier room air conditioner model ESA408J to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

135

Haier: ENERGY STAR Referral (ESA3087)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Haier room air conditioner model ESA3087 to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

136

Equator Appliance: ENERGY STAR Referral (EZ 3720)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Equator Appliance clothes washer EZ 3720 to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

137

Review: Magnetic fields of O stars  

E-Print Network (OSTI)

Since 2002, strong, organized magnetic fields have been firmly detected at the surfaces of about 10 Galactic O-type stars. In this paper I will review the characteristics of the inferred fields of individual stars, as well as the overall population. I will discuss the extension of the 'magnetic desert', first inferred among the A-type stars, to O stars up to 60 solar masses. I will discuss the interaction of the winds of the magnetic stars with the fields above their surfaces, generating complex 'dynamical magnetosphere' structures detected in optical and UV lines, and in X-ray lines and continuum. Finally, I will discuss the detection of a small number of variable O stars in the LMC and SMC that exhibit spectral characteristics analogous to the known Galactic magnetic stars, and that almost certainly represent the first known examples of extra-Galactic magnetic stars.

Wade, G A

2014-01-01T23:59:59.000Z

138

ENERGY STAR Webinar: Portfolio Manager 101  

Energy.gov (U.S. Department of Energy (DOE))

ENERGY STAR is hosting a webinar on the U.S. Environmental Protection Agency's new ENERGY STAR Portfolio Manager tool on Oct. 28, 2014, from 1:00 p.m. - 2:30 p.m. Eastern Standard Time.

139

How to Apply for the ENERGY STAR  

Energy.gov (U.S. Department of Energy (DOE))

Join us to learn about applying for ENERGY STAR Certification in Portfolio Manager. Understand the value of the ENERGY STAR certification, see the step-by-step process of applying, and gain tips to...

140

Hubble Sees a Neutron Star Alone in Space Nearest Known Neutron Star  

E-Print Network (OSTI)

Hubble Sees a Neutron Star Alone in Space Nearest Known Neutron Star #12;Birth of a Neutron Star In the core, nuclei are smashed into protons & neutrons; the protons combine with electrons to make neutrons & neutrinos. The birth temperature of a neutron star is ~5?1011 K, but neutrino emission cools it to `only

Barnes, Joshua Edward

Note: This page contains sample records for the topic "waha lone star" 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

Gas & Stars Aging low-mass stars eject their outer layers.  

E-Print Network (OSTI)

Recycling Gas & Stars #12;Aging low-mass stars eject their outer layers. M57:The Ring Nebula #12;Thor's Emerald Helmet Winds from high-mass stars blow bubbles of hot gas. #12;Supernova blast waves in stars are mixed back into the gas. NGC 6992: Filaments of theVeil Nebula #12;Bubbles blown by high

Barnes, Joshua Edward

142

NuSTAR: Nuclear Spectroscopic Telescope Array  

SciTech Connect

Bill Craig, an astrophysicist at Lawrence Livermore National Laboratory, describes the NASA NuSTAR mission, launched June 13, 2012.

Craig, Bill

2012-06-13T23:59:59.000Z

143

Black Stars and Gamma Ray Bursts  

E-Print Network (OSTI)

Stars that are collapsing toward forming a black hole but are frozen near the Schwarzschild horizon are termed ``black stars''. Collisions of black stars, in contrast to black hole collisions, may be sources of gamma ray bursts, whose basic parameters are estimated quite simply and are found to be consistent with observed gamma ray bursts. Black star gamma ray bursts should be preceded by gravitational wave emission similar to that from the coalescence of black holes.

Tanmay Vachaspati

2007-06-08T23:59:59.000Z

144

ENERGY STAR Guide to Retro-Commissioning  

Energy.gov (U.S. Department of Energy (DOE))

ENERGY STAR Guide to Retro-Commissioning gives an overview of RCx and provides detailed project guidance.

145

The nuclear physics of neutron stars  

SciTech Connect

We explore the unique and fascinating structure of neutron stars. Although neutron stars are of interest in many areas of Physics, our aim is to provide an intellectual bridge between Nuclear Physics and Astrophysics. We argue against the naive perception of a neutron star as a uniform assembly of neutrons packed to enormous densities. Rather, by focusing on the many exotic phases that are speculated to exist in a neutron star, we show how the reality is different and far more interesting.

Piekarewicz, J. [Department of Physics, Florida State University, Tallahassee, FL 32306-4350 (United States)

2014-05-09T23:59:59.000Z

146

Join ENERGY STAR as a partner | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Join ENERGY STAR as a partner Join ENERGY STAR as a partner 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 How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner Service and Product Provider associations partnering with ENERGY STAR ENERGY STAR service & product provider training series Service and product provider's marketing toolkit

147

STAR Highlights on Heavy Ion Physics  

E-Print Network (OSTI)

RHIC-STAR is a mid-rapidity collider experiment for studying high energy nuclear collisions. The main physics goals of STAR experiment are 1) studying the properties of the strongly coupled Quark Gluon Plasma, 2) explore the QCD phase diagram structure. In these proceedings, we will review the recent results of heavy ion physics at STAR.

Shusu Shi

2014-09-30T23:59:59.000Z

148

Massive Stars: Their Birth Sites and Distribution  

E-Print Network (OSTI)

The stellar IMF has been found to be an invariant Salpeter power-law (alpha=2.35) above about 1 Msun, but at the same time a massive star typically has more than one companion. This constrains the possible formation scenarios of massive stars, but also implies that the true, binary-star corrected stellar IMF could be significantly steeper than Salpeter, alpha>2.7. A significant fraction of all OB stars are found relatively far from potential birth sites which is most probably a result of dynamical ejections from cores of binary-rich star clusters. Such cores form rapidly due to dynamical mass segregation, or they are primordial. Probably all OB stars thus form in stellar clusters together with low-mass stars, and they have a rather devastating effect on the embedded cluster by rapidly driving out the remaining gas leaving expanding OB associations and bound star clusters. The distributed population of OB stars has a measured IMF with alpha about 4, which however, does not necessarily constitute a different physical mode for isolated star formation. A steep field-star IMF is obtained naturally because stars form in clusters which are distributed according to a power-law cluster mass function.

Pavel Kroupa

2003-09-22T23:59:59.000Z

149

Toy stars in one dimension  

Science Journals Connector (OSTI)

......equilibrium position due to forces from much greater masses...toy star stayed in the fundamental mode regardless of the...suggested that maybe the fundamental was an exact solution...really a many-body force that Newton had used...Stegun I. A., 1972, Handbook of Mathematical Functions......

J. J. Monaghan; D. J. Price

2004-06-01T23:59:59.000Z

150

BPS Skyrmions as neutron stars  

E-Print Network (OSTI)

The BPS Skyrme model has been demonstrated already to provide a physically intriguing and quantitatively reliable description of nuclear matter. Indeed, the model has both the symmetries and the energy-momentum tensor of a perfect fluid, and thus represents a field theoretic realization of the "liquid droplet" model of nuclear matter. In addition, the classical soliton solutions together with some obvious corrections (spin-isospin quantization, Coulomb energy, proton-neutron mass difference) led to an accurate modeling of nuclear binding energies for heavier nuclei. These results lead to the rather obvious proposal to try to describe also neutron stars by the BPS Skyrme model coupled to gravity. We find that the resulting self-gravitating BPS Skyrmions provide an excellent description of neutron stars when the parameter values of the model are extracted from nuclear physics. Specifically, the maximum possible mass of a neutron star before black-hole formation sets in is a few solar masses, the precise value depending on the precise values of the model parameters, and the resulting neutron star radius is of the order of 10 km.

C. Adam; C. Naya; J. Sanchez-Guillen; R. Vazquez; A. Wereszczynski

2014-07-14T23:59:59.000Z

151

BPS Skyrmions as neutron stars  

E-Print Network (OSTI)

The BPS Skyrme model has been demonstrated already to provide a physically intriguing and quantitatively reliable description of nuclear matter. Indeed, the model has both the symmetries and the energy-momentum tensor of a perfect fluid, and thus represents a field theoretic realization of the "liquid droplet" model of nuclear matter. In addition, the classical soliton solutions together with some obvious corrections (spin-isospin quantization, Coulomb energy, proton-neutron mass difference) provide an accurate modeling of nuclear binding energies for heavier nuclei. These results lead to the rather natural proposal to try to describe also neutron stars by the BPS Skyrme model coupled to gravity. We find that the resulting self-gravitating BPS Skyrmions provide excellent results as well as some new perspectives for the description of bulk properties of neutron stars when the parameter values of the model are extracted from nuclear physics. Specifically, the maximum possible mass of a neutron star before black-hole formation sets in is a few solar masses, the precise value depending on the precise values of the model parameters, and the resulting neutron star radius is of the order of 10 km.

C. Adam; C. Naya; J. Sanchez-Guillen; R. Vazquez; A. Wereszczynski

2014-07-14T23:59:59.000Z

152

Dark Stars: the First Stars in the Universe may be powered by Dark Matter Heating  

E-Print Network (OSTI)

A new line of research on Dark Stars is reviewed, which suggests that the first stars to exist in the universe were powered by dark matter heating rather than by fusion. Weakly Interacting Massive Particles, which may be there own antipartmers, collect inside the first stars and annihilate to produce a heat source that can power the stars. A new stellar phase results, a Dark Star, powered by dark matter annihilation as long as there is dark matter fuel.

Katherine Freese; Peter Bodenheimer; Paolo Gondolo; Douglas Spolyar

2008-12-28T23:59:59.000Z

153

Building Energy Software Tools Directory: Star Perfomer  

NLE Websites -- All DOE Office Websites (Extended Search)

Star Perfomer Star Perfomer Star Perfomer logo. Outlines simple steps to help office building owners, managers and tenants improve their greenhouse and energy efficiency performance, simply by asking some straightforward questions about the size, operating hours, current performance and equipment standards of the building. Star Performer is a diagnostic tool that uses the current operational energy performance of the building measured against a national benchmark, obtained through the Australian Building Greenhouse Rating scheme (see links below), as a basis for making recommendations. The tool covers all areas of the building which affect operational energy performance, including building fabric, equipment and operational practices. Star Perfomer will point you in the right direction and give

154

Build Your Business with ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Service and Product Providers: Service and Product Providers: Build Your Business with ENERGY STAR ® Let ENERGY STAR Be Your Market Advantage Look to ENERGY STAR to help you bring value to your customers and more sales to your organization. Service and Product Providers (SPPs) are integral in helping existing commercial buildings use energy more efficiently. Partnering with ENERGY STAR provides you with access to free tools and resources to help you devise and implement energy- efficient strategies that are right for your customers: > Use the ENERGY STAR Brand to Enhance Your Credibility: Use the nationally recognized ENERGY STAR partner logo on your promotional materials to symbolize your commitment to delivering energy efficiency and financial savings to customers. Help customers build their reputation as environmental and social leaders through work with an ENERGY STAR SPP partner.

155

Supermassive black holes from supermassive stars  

NLE Websites -- All DOE Office Websites (Extended Search)

Supermassive black holes from supermassive stars Supermassive black holes from supermassive stars 1663 Los Alamos science and technology magazine Latest Issue:November 2013 All Issues » submit Supermassive black holes from supermassive stars Supermassive stars in the early universe gave supermassive black holes a head start March 25, 2013 simulations suggest that star formation conditions back then allowed the first stars to become supermassive themselves In this simulation, a black hole that was just formed by the collapse of a supermassive star is surrounded by a distribution of gas (color indicates density). Because the black hole (located at the center but too small to see) grows by consuming the available gas, simulations like this one help determine how quickly the black hole can grow. The progenitor of this black

156

ORISE: Voluntary Protection Program (VPP) Star Status  

NLE Websites -- All DOE Office Websites (Extended Search)

Voluntary Protection Program (VPP) Star Status Voluntary Protection Program (VPP) Star Status Within the U.S. Department of Energy's (DOE) Voluntary Protection Program (VPP), there are three levels of recognition: STAR, MERIT and DEMONSTRATION. Contractors' programs that meet the requirements for outstanding safety and health programs, earn VPP STAR status-the highest achievement level. In December of 2003, the Oak Ridge Institute for Science and Education (ORISE) first earned STAR distinction following a comprehensive evaluation of its application for the VPP program. At that time, ORISE was just the 21st DOE site and the first in Tennessee to earn such exemplary recognition. In 2011 ORISE received its seventh consecutive Star of Excellence award. Today, ORISE is one of more than two dozen DOE sites to achieve VPP STAR

157

Energy Star Rebate Finder | Open Energy Information  

Open Energy Info (EERE)

Energy Star Rebate Finder Energy Star Rebate Finder Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Energy Star Rebate Finder Agency/Company /Organization: United States Environmental Protection Agency Sector: Energy Focus Area: Energy Efficiency Phase: Evaluate Options, Prepare a Plan Resource Type: Online calculator User Interface: Mobile Device Website: m.epa.gov/apps/energy.html Web Application Link: m.epa.gov/apps/energy.html Cost: Free Energy Star Rebate Finder Screenshot References: EPA[1] Logo: Energy Star Rebate Finder Find special offers and rebates from Energy Star partners by entering your zip code. Overview To encourage customers to buy energy efficient products, Energy Star partners occasionally sponsor special offers, such as sales tax exemptions or credits, or rebates on qualified products. Partners also occasionally

158

Green Star Alternative Energy | Open Energy Information  

Open Energy Info (EERE)

Green Star Alternative Energy Green Star Alternative Energy Jump to: navigation, search Name Green Star Alternative Energy Place San Diego, California Zip 92108 Sector Wind energy Product A US-based wind energy project developer. References Green Star Alternative Energy[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Green Star Alternative Energy is a company located in San Diego, California . References ↑ "Green Star Alternative Energy" Retrieved from "http://en.openei.org/w/index.php?title=Green_Star_Alternative_Energy&oldid=346056" Categories: Clean Energy Organizations Companies Organizations Stubs What links here Related changes Special pages Printable version Permanent link

159

Atmospheres and radiating surfaces of neutron stars  

E-Print Network (OSTI)

The beginning of the 21st century was marked by a breakthrough in the studies of thermal radiation of neutron stars. Observations with modern space telescopes have provided a wealth of valuable information. Being correctly interpreted, this information can elucidate physics of superdense matter in the interiors of these stars. The theory of formation of thermal spectra of neutron stars is based on the physics of plasmas and radiative processes in stellar photospheres. It provides the framework for interpretation of observational data and for extracting neutron-star parameters from these data. This paper presents a review of the current state of the theory of surface layers of neutron stars and radiative processes in these layers, with the main focus on the neutron stars that possess strong magnetic fields. In addition to the conventional deep (semi-infinite) atmospheres, radiative condensed surfaces of neutron stars and "thin" (finite) atmospheres are also considered.

Potekhin, A Y

2014-01-01T23:59:59.000Z

160

Nuclear and gravitational energies in stars  

E-Print Network (OSTI)

The force that governs the evolution of stars is gravity. Indeed this force drives star formation, imposes thermal and density gradients into stars at hydrostatic equilibrium and finally plays the key role in the last phases of their evolution. Nuclear power in stars governs their lifetimes and of course the stellar nucleosynthesis. The nuclear reactions are at the heart of the changes of composition of the baryonic matter in the Universe. This change of composition, in its turn, has profound consequences on the evolution of stars and galaxies. The energy extracted from the gravitational, respectively nuclear reservoirs during the lifetimes of stars of different masses are estimated. It is shown that low and intermediate mass stars (M 8 Msol), which explode in a supernova explosion, extract more than 5 times more energy from the gravitational reservoir than from the nuclear one. We conclude by discussing a few important nuclear reactions and their link to topical astrophysical questions.

Meynet, Georges; Ekstrm, Sylvia

2013-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

ENERGY STAR SNAPSHOT - Spring 2009  

NLE Websites -- All DOE Office Websites (Extended Search)

Measuring Progress in the Measuring Progress in the Commercial and Industrial Sectors Fall 2009 Summary By mid-year 2009, key commercial and industrial organizations have already surpassed their 2008 efforts to improve energy performance and reduce greenhouse gas emissions: * More buildings have been rated at mid year 2009 than in all of last year. This brings the total number of buildings with energy performance ratings to more than 97,000. * Nearly 1,850 buildings have earned the ENERGY STAR in 2009, ahead of the 2008 mid-year total. * Almost 30 organizations, mostly among our nation's public school districts, have already achieved significant portfolio-wide energy improvements or top performance. The ENERGY STAR Snapshot provides an at-a-glance summary of the key performance indicators behind

162

$J/?$ and $?$ measurements in STAR  

E-Print Network (OSTI)

Heavy-quarkonium states are expected to evidenciate the deconfinement of the nuclear matter into a Quark-Gluon Plasma in heavy-ion collisions. To strive conclusive information from quarkonium production modification in A+A collisions, systematic measurements of the $J/\\psi$ and $\\Upsilon$ states in p+p, d+Au and Au+Au collisions are necessary. To accomplish this mission the STAR experiment has a Quarkonium program based on the development of specific trigger setups that take advantage of the large STAR acceptance. In this work we present the preliminary results of the $J/\\psi$ and $\\Upsilon$ measurement in 200 GeV p+p and the first measurements of $\\Upsilon$ in 200 GeV heavy ion collisions.

Mauro R. Cosentino; for the Star Collaboration

2008-06-02T23:59:59.000Z

163

Massive Stars and their Supernovae  

E-Print Network (OSTI)

Massive stars and their supernovae are prominent sources of radioactive isotopes, the observations of which thus can help to improve our astrophysical models of those. Our understanding of stellar evolution and the final explosive endpoints such as supernovae or hypernovae or gamma-ray bursts relies on the combination of magneto-hydrodynamics, energy generation due to nuclear reactions accompanying composition changes, radiation transport, and thermodynamic properties (such as the equation of state of stellar matter). Nuclear energy production includes all nuclear reactions triggered during stellar evolution and explosive end stages, also among unstable isotopes produced on the way. Radiation transport covers atomic physics (e.g. opacities) for photon transport, but also nuclear physics and neutrino nucleon/nucleus interactions in late phases and core collapse. Here we want to focus on the astrophysical aspects, i.e. a description of the evolution of massive stars and their endpoints, with a special emphasis ...

Thielemann, Friedrich-Karl; Liebendrfer, Matthias; Diehl, Roland; 10.1007/978-3-642-12698-7_4

2010-01-01T23:59:59.000Z

164

Home Performance with Energy Star  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

- HPwES - HPwES Home Performance with ENERGY STAR Ely Jacobsohn U.S. Department of Energy Ely.jacobsohn@ee.doe.gov, 202-287-1333 April 3, 2013 2 | Building Technologies Office eere.energy.gov Purpose and Objectives: Problem Statement Works to advance the Department's and Administration's energy-related goals in the residential sector Face challenging and often conflicting mandates to save energy, meet environmental goals, and satisfy needs of

165

Find ENERGY STAR certified buildings and plants | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

» Buildings & Plants » Buildings & Plants » About us » Find ENERGY STAR certified buildings and plants 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 How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants Registry of ENERGY STAR certified buildings and plants

166

Neutron stars and strange stars in the chiral SU(3) quark mean field model  

E-Print Network (OSTI)

We investigate the equations of state for pure neutron matter and strange hadronic matter in $\\beta$-equilibrium, including $\\Lambda$, $\\Sigma$ and $\\Xi$ hyperons. The masses and radii of pure neutron stars and strange hadronic stars are obtained. For a pure neutron star, the maximum mass is about $1.8 M_{\\mathrm{sun}}$, while for a strange hadronic star, the maximum mass is around $1.45 M_{\\mathrm{sun}}$. The typical radii of pure neutron stars and strange hadronic stars are about 11.0-12.3 km and 10.7-11.7 km, respectively.

P. Wang; S. Lawley; D. B. Leinweber; A. W. Thomas; A. G. Williams

2005-06-06T23:59:59.000Z

167

Supermassive Stars: Fact or Fiction?  

E-Print Network (OSTI)

Supermassive black holes are now realized to exist in the centers of most galaxies. The recent discoveries of luminous quasars at redshifts higher than 6 require that these black holes were assembled already when the Universe was less than a billion years old. They might originate from the collapse of supermassive stars, a scenario which could ensure a sufficiently rapid formation. Supermassive stars are dominated by photon pressure and radiate at their Eddington limit, which drives their quasi-static evolution to a final relativistic instability. Above some critical value of the metallicity, their collapse can lead to a gigantic explosion, powered by the energy release due to hydrogen burning, but below this critical metallicity their collapse inevitably ends in the formation of a black hole, accompanied by the emission of huge amounts of energy in the form of neutrinos. Although collapsing supermassive stars are the most powerful known burst sources of neutrinos, the associated conditions do not appear favorable for producing highly relativistic outflows that can explain cosmic gamma-ray bursts.

H. -Th. Janka

2002-02-01T23:59:59.000Z

168

Magnetic fields in Neutron Stars  

E-Print Network (OSTI)

Isolated neutron stars show a diversity in timing and spectral properties, which has historically led to a classification in different sub-classes. The magnetic field plays a key role in many aspects of the neutron star phenomenology: it regulates the braking torque responsible for their timing properties and, for magnetars, it provides the energy budget for the outburst activity and high quiescent luminosities (usually well above the rotational energy budget). We aim at unifying this observational variety by linking the results of the state-of-the-art 2D magneto-thermal simulations with observational data. The comparison between theory and observations allows to place two strong constraints on the physical properties of the inner crust. First, strong electrical currents must circulate in the crust, rather than in the star core. Second, the innermost part of the crust must be highly resistive, which is in principle in agreement with the presence of a novel phase of matter so-called nuclear pasta phase.

Vigan, Daniele; Miralles, Juan A; Rea, Nanda

2015-01-01T23:59:59.000Z

169

The role of low-mass star clusters in massive star formation in Orion  

E-Print Network (OSTI)

To distinguish between the different theories proposed to explain massive star formation, it is crucial to establish the distribution, the extinction, and the density of low-mass stars in massive star-forming regions. We analyzed deep X-ray observations of the Orion massive star-forming region using the Chandra Orion Ultradeep Project (COUP) catalog. We found that pre-main sequence (PMS) low-mass stars cluster toward the three massive star-forming regions: the Trapezium Cluster (TC), the Orion Hot Core (OHC), and OMC1-S. We derived low-mass stellar densities of 10^{5} stars pc^{-3} in the TC and OMC1-S, and of 10^{6} stars pc^{-3} in the OHC. The close association between the low-mass star clusters with massive star cradles supports the role of these clusters in the formation of massive stars. The X-ray observations show for the first time in the TC that low-mass stars with intermediate extinction are clustered toward the position of the most massive star, which is surrounded by a ring of non-extincted low-ma...

Rivilla, V M; Jimenez-Serra, I; Rodriguez-Franco, A

2013-01-01T23:59:59.000Z

170

Sequentially Triggered Star Formation in OB Associations  

E-Print Network (OSTI)

We discuss observational evidence for sequential and triggered star formation in OB associations. We first review the star formation process in the Scorpius-Centaurus OB association, the nearest OB association to the Sun, where several recent extensive studies have allowed us to reconstruct the star formation history in a rather detailed way. We then compare the observational results with those obtained for other OB associations and with recent models of rapid cloud and star formation in the turbulent interstellar medium. We conclude that the formation of whole OB subgroups (each consisting of several thousand stars) requires large-scale triggering mechanisms such as shocks from expanding wind and supernova driven superbubbles surrounding older subgroups. Other triggering mechanisms, like radiatively driven implosion of globules, also operate, but seem to be secondary processes, forming only small stellar groups rather than whole OB subgroups with thousands of stars.

Thomas Preibisch; Hans Zinnecker

2006-10-27T23:59:59.000Z

171

EPA ENERGY STAR Webinar: How to Apply for the ENERGY STAR  

Office of Energy Efficiency and Renewable Energy (EERE)

Join us to learn about applying for ENERGY STAR Certification in Portfolio Manager. Understand the value of the ENERGY STAR certification, see the step-by-step process of applying, and gain tips to...

172

EPA ENERGY STAR Webinar: How to Apply for the ENERGY STAR Certification  

Energy.gov (U.S. Department of Energy (DOE))

Join us to learn about applying for ENERGY STAR Certification in Portfolio Manager. Understand the value of the ENERGY STAR certification, see the step-by-step process of applying, and gain tips to...

173

ENERGY STAR Success Story: San Diego Convention Center | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

San Diego Convention Center San Diego Convention Center 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 Success stories Target Finder

174

ENERGY STAR Building Upgrade Manual Chapter 2: Benchmarking | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

2: Benchmarking 2: Benchmarking 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 Success stories Target Finder Technical documentation

175

ENERGY STAR Success Story: Verizon Wireless | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

Verizon Wireless Verizon Wireless 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 Success stories Target Finder Technical documentation

176

ENERGY STAR Guide for Licensed Professionals | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

Guide for Licensed Professionals Guide for Licensed Professionals 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 Success stories Target Finder

177

ENERGY STAR Challenge for Industry: Registration Form | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Registration Form Registration Form 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 Success stories Target Finder Technical documentation

178

ENERGY STAR Success Story: Kohl's Department Stores | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Kohl's Department Stores Kohl's Department Stores 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 Success stories Target Finder

179

ENERGY STAR Challenge for Industry: Participant Handbook | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Participant Handbook Participant Handbook 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 Success stories Target Finder Technical documentation

180

ENERGY STAR Building Upgrade Manual Chapter 6: Lighting | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

6: Lighting 6: Lighting 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 Success stories Target Finder Technical documentation

Note: This page contains sample records for the topic "waha lone star" 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

The HST contribution to neutron star astronomy  

E-Print Network (OSTI)

While isolated neutron stars (INSs) are among the brightest gamma-ray sources, they are among the faintest ones in the optical, and their study is a challenging task which require the most powerful telescopes. HST has lead neutron star optical astronomy yielding nearly all the identifications achieved since the early 1990s. Here, the major HST contributions in the optical studies of INSs and their relevance for neutron stars' astronomy are reviewed.

R. P. Mignani

2007-10-29T23:59:59.000Z

182

Neutron star properties and the symmetry energy  

E-Print Network (OSTI)

The effect of the symmetry energy on the properties of compact stars is discussed. It is shown that, for stars with masses above 1 $M_\\odot$, the radius of the star varies linearly with the symmetry energy slope $L$. The dependence of the hyperon content and onset density of the direct Urca process on the symmetry energy and meson coupling parametrization are also analyzed.

Rafael Cavagnoli; Constana Providncia; Debora P. Menezes

2011-08-08T23:59:59.000Z

183

Toward faster and more accurate star sensors using recursive centroiding and star identification  

E-Print Network (OSTI)

TOWARD FASTER AND MORE ACCURATE STAR SENSORS USING RECURSIVE CENTROIDING AND STAR IDENTIFICATION A Dissertation by MALAK ANEES SAMAAN Submitted to the O?ce of Graduate Studies of Texas A&M University in partial fulfillment of the requirements... for the degree of DOCTOR OF PHILOSOPHY August 2003 Major Subject: Aerospace Engineering TOWARD FASTER AND MORE ACCURATE STAR SENSORS USING RECURSIVE CENTROIDING AND STAR IDENTIFICATION A Dissertation by MALAK ANEES SAMAAN Submitted to Texas A&M University...

Samaan, Malak Anees

2004-09-30T23:59:59.000Z

184

ENERGY STAR Score for Wastewater Treatment Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

!! !! July 2013 ENERGY STAR Score for Wastewater Treatment Plants in the United States Page 1 ENERGY STAR Score for Wastewater Treatment Plants in the United States Technical Reference OVERVIEW ! The ENERGY STAR Score for Wastewater Treatment Plants applies to primary, secondary, and advanced treatment facilities with or without nutrient removal capacity. The objective of the ENERGY STAR score is to provide a fair assessment of the energy performance of a property relative to its peers, taking into account the climate, weather, and business activities at the property. To identify the aspects of building activity that are significant drivers of energy

185

Stars as resonant absorbers of gravitational waves  

E-Print Network (OSTI)

Quadrupole oscillation modes in stars can resonate with incident gravitational waves (GWs), and grow non-linear at the expense of GW energy. Stars near massive black hole binaries (MBHB) can act as GW-charged batteries, cooling radiatively. Mass-loss from these stars can prompt MBHB accretion at near-Eddington rates. GW opacity is independent of amplitude, so distant resonating stars can eclipse GW sources. Absorption by the Sun of GWs from Galactic white dwarf binaries may be detectable with second-generation space-based GW detectors as a shadow within a complex diffraction pattern.

B. McKernan; K. E. S. Ford; B. Kocsis; Z. Haiman

2014-08-28T23:59:59.000Z

186

Abundances of massive stars: some recent developments  

E-Print Network (OSTI)

Thanks to their usefulness in various fields of astrophysics (e.g. mixing processes in stars, chemical evolution of galaxies), the last few years have witnessed a large increase in the amount of abundance data for early-type stars. Two intriguing results emerging since the last reviews on this topic will be discussed: (a) nearby OB stars exhibit metal abundances generally lower than the solar/meteoritic estimates; (b) evolutionary models of single objects including rotation are largely unsuccessful in explaining the CNO properties of stars in the Galaxy and in the Magellanic clouds.

T. Morel

2008-11-25T23:59:59.000Z

187

A Galactic O-Star Catalog  

E-Print Network (OSTI)

We have produced a catalog of 378 Galactic O stars with accurate spectral classifications which is complete for Vweb-based version with links to online services.

J. Maz-Apellniz; N. R. Walborn; H. . Galu; L. H. Wei

2003-11-09T23:59:59.000Z

188

Residential Energy Star Appliance Rebate Program  

Energy.gov (U.S. Department of Energy (DOE))

Energy Trust of Oregon offers rebates for Energy Star refrigerators, freezers and clothes washers to Oregon residential electric service customers of Portland General Electric (PGE) and Pacific...

189

Pulsating AGB stars in the LMC  

E-Print Network (OSTI)

I give a brief review and interpretation of the evolution, mass loss and pulsation of AGB stars in the Large Magellanic Cloud.

Jacco Th. van Loon

2001-10-08T23:59:59.000Z

190

Ralf Klessen: Basel: 29. 11, 2006 Star FormationStar Formation  

E-Print Network (OSTI)

(Hubble Ultra-Deep Field, from HST Web site) #12;Ralf Klessen: Basel: 29. 11, 2006 Antennae Stars in the Milky WayStars in the Milky Way On the night sky, you see stars and dark clouds Disks in Orion (data: Mark McCaughrean)protostellar disks: dark shades in front

Klessen,Ralf

191

STARS Training Needs Assessment Learner Instructions 07/2009 1 STARS Training Needs Assessment  

E-Print Network (OSTI)

STARS Training Needs Assessment Learner Instructions 07/2009 1 STARS Training Needs Assessment. · Click the STARS (Training) tab. · Click My Training Needs in the left menu. · Click the secure link to continue to My Training Needs. On the Training Needs Assessment page, click the box to the left of every

Ford, James

192

Support for ENERGY STAR Enforcement | Department of Energy  

Energy Savers (EERE)

Support for ENERGY STAR Enforcement Support for ENERGY STAR Enforcement By offering a means for consumers to buy products more energy-efficient than required by law, ENERGY STAR...

193

ARCHEOLOGY OF AN ANCIENT STAR  

SciTech Connect

We report on the bright and late F-type star HR 3138, which, with respect to its chemistry in the [Mg/H]-[Fe/Mg] abundance plane, we identify as an old Population II member. Evolutionary tracks are, however, in conflict with this finding and instead imply an age of only {tau} = 5.6{sup -1.8}{sub +{sub 2.2}} Gyr (2{sigma}) for HR 3138. We discuss this controversy in light of existing high-precision radial velocity surveys that mostly exclude the case of a blue straggler primary and a white dwarf secondary. While it is realized that a stellar merger can principally solve the issue and there is indeed observational evidence for mass accretion on HR 3138 from the absence of lithium in its photosphere, we also consider the interesting circumstance that HR 3138 lies in the direction to the 350 pc distant, young open cluster NGC 2516. We point to the possibility that the progenitor cloud of this cluster may likewise account for former mass accretion and we argue in particular for a dynamical friction with this cloud as a plausible cause for the strikingly common Galactic rotational velocity of the field star and open cluster.

Fuhrmann, K.; Chini, R.; Haas, M.; Hackstein, M.; Ramolla, M. [Astronomisches Institut, Ruhr-Universitaet Bochum, Universitaetsstrasse 150, D-44801 Bochum (Germany); Bernkopf, J., E-mail: klaus@ing.iac.es [University of Applied Sciences Augsburg, An der Hochschule 1, D-86161 Augsburg (Germany)

2012-12-20T23:59:59.000Z

194

Path Integral on Star Graph  

E-Print Network (OSTI)

In this paper we study path integral for a single spinless particle on a star graph with N edges, whose vertex is known to be described by U(N) family of boundary conditions. After carefully studying the free particle case, both at the critical and off-critical levels, we propose a new path integral formulation that correctly captures all the scale-invariant subfamily of boundary conditions realized at fixed points of boundary renormalization group flow. Our proposal is based on the folding trick, which maps a scalar-valued wave function on star graph to an N-component vector-valued wave function on half-line. All the parameters of scale-invariant subfamily of boundary conditions are encoded into the momentum independent weight factors, which appear to be associated with the two distinct path classes on half-line that form the cyclic group Z_2. We show that, when bulk interactions are edge-independent, these weight factors are generally given by an N-dimensional unitary representation of Z_2. Generalization to momentum dependent weight factors and applications to worldline formalism are briefly discussed.

Satoshi Ohya

2011-04-28T23:59:59.000Z

195

Path Integral on Star Graph  

E-Print Network (OSTI)

In this paper we study path integral for a single spinless particle on a star graph with N edges, whose vertex is known to be described by U(N) family of boundary conditions. After carefully studying the free particle case, both at the critical and off-critical levels, we propose new path integral formulation that correctly captures all the scale-invariant subfamily of boundary conditions realized at fixed points of boundary renormalization group flow. Our proposal is based on the folding trick, which maps a scalar-valued wave function on star graph to an N-component vector-valued wave function on half-line. All the parameters of scale-invariant subfamily of boundary conditions are encoded into the momentum independent weight factors, which appear to be associated with the two distinct path classes on half-line that form the cyclic group Z_2. We show that, when bulk interactions are edge-independent, these weight factors are generally given by an N-dimensional unitary representation of Z_2. Generalization to ...

Ohya, Satoshi

2011-01-01T23:59:59.000Z

196

Neutron Star Crustal Interface Waves  

Science Journals Connector (OSTI)

The eigenfrequencies of nonradial oscillations are a powerful probe of a star's interior structure. This is especially true when there exist discontinuities such as at the neutron star (NS) ocean/crust boundary, as first noted by McDermott, Van Horn, & Hansen. The interface mode associated with this boundary has subsequently been neglected in studies of stellar nonradial oscillations. We revisit this mode, investigating its properties both analytically and numerically for a simple NS envelope model. We find that it acts like a shallow surface ocean wave, but with a large radial displacement at the ocean/crust boundary due to flexing of the crust with shear modulus ? P, the pressure. This displacement lowers the mode's frequency by a factor of ~(?/P)1/2 ~ 0.1 in comparison to a shallow surface wave frequency on a hard surface. The interface mode may be excited on accreting or bursting NSs, and future work on nonradial oscillations should consider this mode. Our work also implies an additional mode on massive and/or cold white dwarfs with crystalline cores, which may have a frequency between the f-mode and g-modes, an otherwise empty part of the frequency domain.

Anthony L. Piro; Lars Bildsten

2005-01-01T23:59:59.000Z

197

North Star Refrigerator: Order (2013-CE-5355)  

Energy.gov (U.S. Department of Energy (DOE))

DOE ordered North Star Refrigerator Co., Inc. to pay a $8,000 civil penalty after finding North Star Refrigerator had failed to certify that any basic models of walk-in cooler and freezer components comply with the applicable energy conservation standards.

198

Long Baseline Interferometry of Be Stars  

E-Print Network (OSTI)

We give an introduction to interferometrical concepts and their applicability to Be stars. The first part of the paper concentrates on a short historic overview and basic principles of two-beam interferometric observations. In the second part, the VLTI/MIDI instrument is introduced and its first results on Be stars, obtained on alpha Ara and delta Cen, are outlined.

Olivier Chesneau; Thomas Rivinius

2005-10-24T23:59:59.000Z

199

X-ray Spectroscopy of Cool Stars  

E-Print Network (OSTI)

High-resolution X-ray spectroscopy has addressed not only various topics in coronal physics of stars, but has also uncovered important features relevant for our understanding of stellar evolution and the stellar environment. I summarize recent progress in coronal X-ray spectroscopy and in particular also discuss new results from studies of X-rays from pre-main sequence stars.

M. Guedel

2006-09-11T23:59:59.000Z

200

X-ray Emission from Massive Stars  

E-Print Network (OSTI)

X-ray Emission from Massive Stars David Cohen Department of Physics and Astronomy Swarthmore #12;What is the mechanism by which massive stars produce x-rays? New results from the Chandra X-ray Observatory ­ high-resolution x-ray spectroscopy: measuring Doppler broadening in emission lines Testing

Cohen, David

Note: This page contains sample records for the topic "waha lone star" 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

Nuclear and gravitational energies in stars  

SciTech Connect

The force that governs the evolution of stars is gravity. Indeed this force drives star formation, imposes thermal and density gradients into stars at hydrostatic equilibrium and finally plays the key role in the last phases of their evolution. Nuclear power in stars governs their lifetimes and of course the stellar nucleosynthesis. The nuclear reactions are at the heart of the changes of composition of the baryonic matter in the Universe. This change of composition, in its turn, has profound consequences on the evolution of stars and galaxies. The energy extracted from the gravitational, respectively nuclear reservoirs during the lifetimes of stars of different masses are estimated. It is shown that low and intermediate mass stars (M < 8 M{sub ?}) extract roughly 90 times more energy from their nuclear reservoir than from their gravitational one, while massive stars (M > 8 M{sub ?}), which explode in a supernova explosion, extract more than 5 times more energy from the gravitational reservoir than from the nuclear one. We conclude by discussing a few important nuclear reactions and their link to topical astrophysical questions.

Meynet, Georges; Ekstrm, Sylvia [Astronomical Observatory of Geneva University (Switzerland); Courvoisier, Thierry [ISDC, Astronomical Observatory of Geneva University (Switzerland)

2014-05-09T23:59:59.000Z

202

The role of low-mass star clusters in massive star formation. The Orion Case  

E-Print Network (OSTI)

To distinguish between the different theories proposed to explain massive star formation, it is crucial to establish the distribution, the extinction, and the density of low-mass stars in massive star-forming regions. We analyze deep X-ray observations of the Orion massive star-forming region using the Chandra Orion Ultradeep Project (COUP) catalog. We studied the stellar distribution as a function of extinction, with cells of 0.03 pc x 0.03 pc, the typical size of protostellar cores. We derived stellar density maps and calculated cluster stellar densities. We found that low-mass stars cluster toward the three massive star-forming regions: the Trapezium Cluster (TC), the Orion Hot Core (OHC), and OMC1-S. We derived low-mass stellar densities of 10^{5} stars pc^{-3} in the TC and OMC1-S, and of 10^{6} stars pc^{-3} in the OHC. The close association between the low-mass star clusters with massive star cradles supports the role of these clusters in the formation of massive stars. The X-ray observations show for ...

Rivilla, V M; Jimenez-Serra, I; Rodriguez-Franco, A

2013-01-01T23:59:59.000Z

203

Step 6: Complete the ENERGY STAR lifecycle | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

6: Complete the ENERGY STAR lifecycle 6: 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 design to earn ENERGY STAR Design to earn ENERGY STAR Step 1: Include efficiency in your project specs Step 2: Meet with your team and set a goal Step 3: Apply for Designed to Earn the ENERGY STAR recognition Step 4: Market your project as Designed to Earn the ENERGY STAR

204

Win ENERGY STAR Partner of the Year | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Win ENERGY STAR Partner of the Year Win ENERGY STAR Partner of the Year 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use ENERGY STAR in action Communicate and educate ENERGY STAR communications toolkit Bring Your Green to Work with ENERGY STAR

205

Why you should design to earn the ENERGY STAR | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

Why you should design to earn the ENERGY STAR Why you should design to earn the ENERGY STAR 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 Leading firms choose ENERGY STAR Why new doesn't always mean efficient Follow EPA's step-by-step process ENERGY STAR Challenge for Architects Why you should design to earn the ENERGY STAR

206

DOE Defends Decision to Revoke Energy Star Designation for Certain...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Decision to Revoke Energy Star Designation for Certain LG Refrigerators DOE Defends Decision to Revoke Energy Star Designation for Certain LG Refrigerators December 23, 2009 -...

207

ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program...  

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

National Program Requirements ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program Requirements ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program...

208

ENERGY STAR Certified Homes, Version 3 (Rev. 07) Inspection Checklists...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Inspection Checklists for National Program Requirements ENERGY STAR Certified Homes, Version 3 (Rev. 07) Inspection Checklists for National Program Requirements ENERGY STAR...

209

Webinar: ENERGY STAR Hot Water Systems for High Performance Homes...  

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

Webinar: ENERGY STAR Hot Water Systems for High Performance Homes Webinar: ENERGY STAR Hot Water Systems for High Performance Homes This presentation is from the Building America...

210

Energy Department and AHAM Partner to Streamline ENERGY STAR...  

Energy Savers (EERE)

Energy Department and AHAM Partner to Streamline ENERGY STAR Testing for Washers, Dryers, Refrigerators Energy Department and AHAM Partner to Streamline ENERGY STAR Testing for...

211

Home Performance with ENERGY STAR -- 10 Years of Continued Growth...  

Energy Savers (EERE)

More Documents & Publications Home Performance with Energy Star Home Performance with ENERGY STAR - 2014 BTO Peer Review Residential Building Audits and Retrofits...

212

Green Star Products Inc GSPI | Open Energy Information  

Open Energy Info (EERE)

"Green Star Products Inc (GSPI)" Retrieved from "http:en.openei.orgwindex.php?titleGreenStarProductsIncGSPI&oldid782343" Categories: Organizations Companies Stubs What...

213

ENERGY STAR SNAPSHOT … Spring 2010  

NLE Websites -- All DOE Office Websites (Extended Search)

10 10 Summary In 2009, commercial and industrial organizations continued their impressive efforts to improve their energy performance and reduce greenhouse emissions. As a result: * More than 65,000 buildings received an ENERGY STAR energy performance score in 2009, a 50 percent increase over 2008 * Nearly 3,900 buildings earned the ENERGY STAR, a 20 percent increase over the record- breaking activity of the previous year * Almost 60 organizations achieved ENERGY STAR Leader recognition providing the greatest single year of savings since the program began in 2004 The ENERGY STAR Snapshot provides an at-a-glance summary of the key performance indicators behind these impressive results. The Snapshot reports the latest national ENERGY STAR metrics to help

214

ENERGY STAR SNAPSHOT … Spring 2009  

NLE Websites -- All DOE Office Websites (Extended Search)

Snapshot data runs through December 31, 2010. Snapshot data runs through December 31, 2010. The ENERGY STAR Snapshot provides an at-a-glance summary of the latest national ENERGY STAR metrics to help you, our partners, see the impact of your efforts. The ENERGY STAR Snapshot is distributed twice a year and provides: Trends in energy benchmarking of commercial and industrial buildings. State-by-state activity along with activity for the top Designated Market Areas. Industrial sector participation in ENERGY STAR. Trends in ENERGY STAR certified buildings and plants. Summary By end-of-year 2010, commercial and industrial organizations nearly exceeded activity levels reached throughout all of 2009 for benchmarking and certification. Since June 30, 2010: The number of benchmarked buildings has grown to 185,000 buildings, representing over 21

215

ENERGY STAR SNAPSHOT … Spring 2009  

NLE Websites -- All DOE Office Websites (Extended Search)

1 1 Snapshot data runs through June 30, 2011. The ENERGY STAR Snapshot provides an at-a-glance summary of the latest national ENERGY STAR metrics to help you, our partners, see the impact of your efforts. The ENERGY STAR Snapshot is distributed twice a year and provides: * Trends in energy benchmarking of commercial and industrial buildings. * State-by-state activity along with activity for the top Designated Market Areas. * Industrial sector participation in ENERGY STAR. * Trends in ENERGY STAR labeled commercial and industrial facilities. Summary By mid-year 2011, commercial and industrial organizations were on track to, or were already exceeding, figures for benchmarking and labeling that were set by end of year 2010. Since December, 2010:

216

The breaking strain of neutron star crust  

SciTech Connect

Mountains on rapidly rotating neutron stars efficiently radiate gravitational waves. The maximum possible size of these mountains depends on the breaking strain of neutron star crust. With multimillion ion molecular dynamics simulations of Coulomb solids representing the crust, we show that the breaking strain of pure single crystals is very large and that impurities, defects, and grain boundaries only modestly reduce the breaking strain to around 0.1. Due to the collective behavior of the ions during failure found in our simulations, the neutron star crust is likely very strong and can support mountains large enough so that their gTavitational wave radiation could limit the spin periods of some stars and might be detectable in large scale interferometers. Furthermore, our microscopic modeling of neutron star crust material can help analyze mechanisms relevant in Magnetar Giant and Micro Flares.

Kadau, Kai [Los Alamos National Laboratory; Horowitz, C J [INDIANA UNIV

2009-01-01T23:59:59.000Z

217

Home Energy Yardstick : ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Home > Home Improvement > Home Energy Yardstick Home > Home Improvement > Home Energy Yardstick Home Energy Yardstick Assess the energy efficiency of your home and see how it measures up: EPA's Home Energy Yardstick provides a simple assessment of your home's annual energy use compared to similar homes. By answering a few basic questions about your home, you can get: Your home's Home Energy Yardstick score (on a scale of 1 to 10); Insights into how much of your home's energy use is related to heating and cooling versus other everyday uses like appliances, lighting, and hot water; Links to guidance from ENERGY STAR on how to increase your home's score, improve comfort, and lower utility bills; and An estimate of your home's annual carbon emissions. Learn more about how the Home Energy Yardstick works.

218

Bulk viscosity in hybrid stars  

Science Journals Connector (OSTI)

We compute the bulk viscosity of a mixed quark-hadron phase. In the first scenario to be discussed, the mixed phase occurs at large densities and we assume that it is composed of a mixing of hyperonic matter and quarks in the Color Flavor Locked phase. In a second scenario, the mixed phase occurs at lower densities and it is composed of a mixing of nucleons and unpaired quark matter. We have also investigated the effect of a nonvanishing surface tension at the interface between hadronic and quark matter. In both scenarios, the bulk viscosity is large when the surface tension is absent, while the value of the viscosity reduces in the second scenario when a finite value for the surface tension is taken into account. In all cases, the r-mode instabilities of the corresponding hybrid star are suppressed.

A. Drago; A. Lavagno; G. Pagliara

2005-05-16T23:59:59.000Z

219

Chromospherically Active Stars in the Galactic Bulge  

E-Print Network (OSTI)

We present the results from the discovery and study of ~3000 chromospherically active giant and subgiant stars toward the Galactic bulge. We find that these stars are predominantly RS CVn binaries with rotation periods between 10 and 100 days. We discover that the average rotational period of these stars decreases with their distance from the Galactic plane. We find that the primary stars in the RS CVn systems are predominantly first-ascent giants. Our research also suggests that, if these stars have spot cycles like the sun, then the cycle period must be longer than 10 years on average. We confirm that the amplitude of the spot-induced modulations observed in the light curves of these objects is generally larger at minimum light than at maximum. Furthermore, we confirm that the amplitudes of the modulations due to stellar spots generally increases as the observed change in average brightness increases. We find no evidence for a relationship between a CA star's brightness and its rotational period. However, the average period does increase with colour for stars with periods >~30 days.

A. J. Drake

2005-10-17T23:59:59.000Z

220

Anisotropic pressure and hyperons in neutron stars  

E-Print Network (OSTI)

We study the effects of anisotropic pressure on properties of the neutron stars with hyperons inside its core within the framework of extended relativistic mean field. It is found that the main effects of anisotropic pressure on neutron star matter is to increase the stiffness of the equation of state, which compensates for the softening of the EOS due to the hyperons. The maximum mass and redshift predictions of anisotropic neutron star with hyperonic core are quite compatible with the result of recent observational constraints if we use the parameter of anisotropic pressure model $h \\le 0.8$[1] and $\\Lambda \\le -1.15$ [2]. The radius of the corresponding neutron star at $M$=1.4 $M_\\odot$ is more than 13 km, while the effect of anisotropic pressure on the minimum mass of neutron star is insignificant. Furthermore, due to the anisotropic pressure in the neutron star, the maximum mass limit of higher than 2.1 $M_\\odot$ cannot rule out the presence of hyperons in the neutron star core.

A. Sulaksono

2014-12-23T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Supernova Explosions and Neutron Star Formation  

E-Print Network (OSTI)

The current picture of the collapse and explosion of massive stars and the formation of neutron stars is reviewed. According to the favored scenario, however by no means proven and undisputed, neutrinos deposit the energy of the explosion in the stellar medium which surrounds the nascent neutron star. Observations, in particular of Supernova~1987A, suggest that mixing processes play an important role in the expanding star, and multi-dimensional simulations show that these are linked to convective instabilities in the immediate vicinity of the neutron star. Convectively enhanced energy transport inside the neutron star can have important consequences for the neutrino emission and thus the neutrino-heating mechanism. This also holds for a suppression of the neutrino interactions at nuclear densities. Multi-dimensional hydrodynamics, general relativity, and a better understanding of the neutrino interactions in neutron star matter may be crucial to resolve the problem that state-of-the-art spherical models do not yield explosions even with a very accurate treatment of neutrino transport by solving the Boltzmann equation.

H. -Th. Janka; K. Kifonidis; M. Rampp

2001-03-01T23:59:59.000Z

222

Wave-Based Subsurface Guide Star  

SciTech Connect

Astronomical or optical guide stars are either natural or artificial point sources located above the Earth's atmosphere. When imaged from ground-based telescopes, they are distorted by atmospheric effects. Knowing the guide star is a point source, the atmospheric distortions may be estimated and, deconvolved or mitigated in subsequent imagery. Extending the guide star concept to wave-based measurement systems to include acoustic, seismo-acoustic, ultrasonic, and radar, a strong artificial scatterer (either acoustic or electromagnetic) may be buried or inserted, or a pre-existing or natural sub-surface point scatterer may be identified, imaged, and used as a guide star to determine properties of the sub-surface volume. That is, a data collection is performed on the guide star and the sub-surface environment reconstructed or imaged using an optimizer assuming the guide star is a point scatterer. The optimization parameters are the transceiver height and bulk sub-surface background refractive index. Once identified, the refractive index may be used in subsequent reconstructions of sub-surface measurements. The wave-base guide star description presented in this document is for a multimonostatic ground penetrating radar (GPR) but is applicable to acoustic, seismo-acoustic, and ultrasonic measurement systems operating in multimonostatic, multistatic, multibistatic, etc., modes.

Lehman, S K

2011-07-26T23:59:59.000Z

223

Star Formation from Galaxies to Globules  

E-Print Network (OSTI)

The empirical laws of star formation suggest that galactic-scale gravity is involved, but they do not identify the actual triggering mechanisms for clusters in the final stages. Many other triggering processes satisfy the empirical laws too, including turbulence compression and expanding shell collapse. The self-similar nature of the gas and associated young stars suggests that turbulence is more directly involved, but the small scale morphology of gas around most embedded clusters does not look like a random turbulent flow. Most clusters look triggered by other nearby stars. Such a prominent local influence makes it difficult to understand the universality of the Kennicutt and Schmidt laws on galactic scales. A unified view of multi-scale star formation avoids most of these problems. Ambient self-gravity produces spiral arms and drives much of the turbulence that leads to self-similar structures, while localized energy input from existing clusters and field supernovae triggers new clusters in pre-existing clouds. The hierarchical structure in the gas made by turbulence ensures that the triggering time scales with size, giving the Schmidt law over a wide range of scales and the size-duration correlation for young star fields. The efficiency of star formation is determined by the fraction of the gas above a critical density of around 10^5 m(H2)/cc. Star formation is saturated to its largest possible value given the fractal nature of the interstellar medium.

Bruce G. Elmegreen

2002-07-04T23:59:59.000Z

224

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

225

Comment on "Three-dimensional hydrodynamic simulations of the combustion of a neutron star into a quark star"  

E-Print Network (OSTI)

If strange matter is absolutely stable, the ordinary nuclei decay to strangelets, while neutron stars convert into strange stars. Lifetimes of the ordinary nuclei are constrained experimentally to be above $\\sim 10^{33}$ years, while lifetimes of the metastable neutron stars depend on the neutron star masses and can exceed the age of the Universe. As a consequence, the neutron stars and strange stars can coexist in the Universe. We point out that numerical simulations of the conversion of neutron stars to strange stars, performed by M. Herzog and F. K. Roepke in Phys. Rev. D 84, 083002 (2011) [arXiv:rXiv:1109.0539], are focused on a region in the parameter space of strange matter, in which low-massive neutron stars and strange stars are coexistent, whereas massive neutron stars are unstable and short lived on an astronomical timescale.

Krivoruchenko, M I

2014-01-01T23:59:59.000Z

226

ENERGY STAR Guidelines for Energy Management  

NLE Websites -- All DOE Office Websites (Extended Search)

Guidelines for Energy Guidelines for Energy Management ENERGY STAR is a U.S. Environmental Protection Agency Program helping organizations and individuals fight climate change through superior energy efficiency. Learn more at energystar.gov/buildings. 2 ENERGY STAR Guidelines for Energy Management Overview Continuous improvement of energy performance requires establishing effective energy management practices and processes to guide the energy program. Any organization, regardless of size, function, or mission can develop an effective energy program if they are willing to make the commitment. The US EPA's ENERGY STAR Guidelines for Energy Management provides a proven strategy for creating an energy management program focused on continuous improvement of energy performance. The

227

Creative graphics | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

How can we help you? How can we help you? » Communicate and educate » ENERGY STAR communications toolkit » Motivate with a competition » ENERGY STAR National Building Competition » Competitor resources » Creative graphics 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 How can we help you? Build an energy program Improve building and plant performance

228

Energy guides | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

guides guides 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance ENERGY STAR industrial partnership Energy guides Energy efficiency and air regulation Plant energy auditing Industrial service and product providers

229

NorthStar Medical Technologies LLC  

National Nuclear Security Administration (NNSA)

Environmental Assessment for Environmental Assessment for NorthStar Medical Technologies LLC Commercial Domestic Production of the Medical Isotope Molybdenum-99 (DOE/EA-1929) Prepared for U.S. Department of Energy National Nuclear Security Administration Defense Nuclear Nonproliferation/ Global Threat Reduction Initiative August 2012 EA for NorthStar Medical Technologies LLC Commercial Domestic Production of the Medical Isotope Mo-99 i COVER SHEET ENVIRONMENTAL ASSESSMENT FOR NORTHSTAR MEDICAL TECHNOLOGIES LLC COMMERCIAL DOMESTIC PRODUCTION OF THE MEDICAL ISOTOPE MOLYBDENUM-99 Proposed Action: The Department of Energy (DOE) National Nuclear Security Administration (NNSA) proposes to provide funding to NorthStar to accelerate the establishment of the commercial production of

230

ENERGY STAR Score for Senior Care Communities  

NLE Websites -- All DOE Office Websites (Extended Search)

Senior Care Communities in the United States Page 1 Senior Care Communities in the United States Page 1 ENERGY STAR Score for Senior Care Communities in the United States Technical Reference OVERVIEW The ENERGY STAR Score for Senior Care Communities applies to buildings that house and provide care and assistance for elderly residents. The objective of the ENERGY STAR score is to provide a fair assessment of the energy performance of a property relative to its peers, taking into account the climate, weather, and business activities at the property. To identify the aspects of building activity that are significant drivers of energy use and then

231

Neutron stars and the equation of state  

Science Journals Connector (OSTI)

The static properties of neutron stars are probed using phenomenological equations of state. These properties include the maximum mass, radii, central densities, and binding energies. It is found that quite different equations of state can produce similar neutron stars. Likewise, it is also found that equations of state which are quite similar near saturation density can produce very different neutron stars, since it is the high density behavior which is most important. Symmetric matter results cannot be used to uniquely constrain neutron matter because of model dependence on the symmetry energy.

J. Cooperstein

1988-02-01T23:59:59.000Z

232

Lone Tree, Colorado: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

Tree, Colorado: Energy Resources Tree, Colorado: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 39.5360997°, -104.8963682° 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":39.5360997,"lon":-104.8963682,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

233

Combustion of a neutron star into a strange quark star: the neutrino signal  

E-Print Network (OSTI)

There are strong indications that the process of conversion of a neutron star into a strange quark star proceeds as a strong deflagration implying that in a few milliseconds almost the whole star is converted. Starting from the three-dimensional hydrodynamic simulations of the combustion process which provide the temperature profiles inside the newly born strange star, we calculate for the first time the neutrino signal that is to be expected if such a conversion process takes place. The neutrino emission is characterized by a luminosity and a duration that is typical for the signal expected from protoneutron stars and represents therefore a powerful source of neutrinos which could be possibly directly detected in case of events occurring close to our galaxy. We discuss moreover possible connections between the birth of strange stars and explosive phenomena such as Supernovae and Gamma-Ray-Bursts.

Pagliara, G; Ropke, F K

2013-01-01T23:59:59.000Z

234

Passive load follow analysis of the STAR-LM and STAR-H2 systems.  

E-Print Network (OSTI)

Braun for making it possible to work on this dissertation in Argonne National Laboratory. I would also like to thank Dr. Richard Doctor, Dr. Diana Matonis, Dr. Ron Kulak, and Dr. Ike Therios of the Argonne National laboratory for their cooperation... for STAR-H2 ..................................................................127 1 INTRODUCTION STAR Systems The Secure Transportable Autonomous Reactor (STAR) was designed by Argonne National Laboratory (Sienicki et al., 1999; Sienicki...

Moisseytsev, Anton

2004-09-30T23:59:59.000Z

235

Federal Energy Management Program: Covered Product Category: ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Covered Product Covered Product Category: ENERGY STAR Displays to someone by E-mail Share Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on Facebook Tweet about Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on Twitter Bookmark Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on Google Bookmark Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on Delicious Rank Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on Digg Find More places to share Federal Energy Management Program: Covered Product Category: ENERGY STAR Displays on AddThis.com... Energy-Efficient Products Federal Requirements Covered Product Categories

236

CFL Manufacturers: ENERGY STAR Letters | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

CFL Manufacturers: ENERGY STAR Letters CFL Manufacturers: ENERGY STAR Letters CFL Manufacturers: ENERGY STAR Letters January 25, 2010 DOE issued letters to 25 manufacturers of compact fluorescent lamps (CFLs) involving various models after PEARL Cycle 9 testing indicated that the models do not meet the ENERGY STAR specification and, therefore, are disqualified from the ENERGY STAR Program. When a product is disqualified from the ENERGY STAR Program, all corresponding packaging and supplier's products will be disqualified as well. CFL Manufacturers: ENERGY STAR Letters More Documents & Publications Ex Parte Communication Memo Identifying Cost-Effective Residential Energy Efficiency Opportunities for the Kauai Island Utility Cooperative Realizing Building End-Use Efficiency with Ermerging Technologies

237

CFL Manufacturers: ENERGY STAR Letters | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

CFL Manufacturers: ENERGY STAR Letters CFL Manufacturers: ENERGY STAR Letters CFL Manufacturers: ENERGY STAR Letters January 25, 2010 DOE issued letters to 25 manufacturers of compact fluorescent lamps (CFLs) involving various models after PEARL Cycle 9 testing indicated that the models do not meet the ENERGY STAR specification and, therefore, are disqualified from the ENERGY STAR Program. When a product is disqualified from the ENERGY STAR Program, all corresponding packaging and supplier's products will be disqualified as well. CFL Manufacturers: ENERGY STAR Letters More Documents & Publications Ex Parte Communication Memo Realizing Building End-Use Efficiency with Ermerging Technologies Identifying Cost-Effective Residential Energy Efficiency Opportunities for the Kauai Island Utility Cooperative

238

Magic Valley Electric Cooperative - ENERGY STAR Builders Program (Texas) |  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Magic Valley Electric Cooperative - ENERGY STAR Builders Program Magic Valley Electric Cooperative - ENERGY STAR Builders Program (Texas) Magic Valley Electric Cooperative - ENERGY STAR Builders Program (Texas) < Back Eligibility Construction Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Appliances & Electronics Water Heating Program Info State Texas Program Type Utility Rebate Program Rebate Amount ENERGY STAR Home: $150-$600 ENERGY STAR Home with Version 3.0 Checklist: $200 Marathon Water Heater Installation: $150 ENERGY STAR Heat Pump Water Heater: $250 Provider Magic Valley Electric Cooperative Magic Valley Electric Cooperative's (MVEC) ENERGY STAR Builders Program offers a variety of incentives to builders of energy efficiency homes

239

The new ENERGY STAR Portfolio Manager | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

The new ENERGY STAR Portfolio Manager The new ENERGY STAR Portfolio Manager 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 Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit Identify your property type Enter data into Portfolio Manager The data quality checker

240

Double Neutron Stars: Evidence For Two Different Neutron-Star Formation Mechanisms  

E-Print Network (OSTI)

Six of the eight double neutron stars known in the Galactic disk have low orbital eccentricities (neutron stars received only very small velocity kicks at birth. This is similar to the case of the B-emission X-ray binaries, where a sizable fraction of the neutron stars received hardly any velocity kick at birth (Pfahl et al. 2002). The masses of the second-born neutron stars in five of the six low-eccentricity double neutron stars are remarkably low (between 1.18 and 1.30 Msun). It is argued that these low-mass, low-kick neutron stars were formed by the electron-capture collapse of the degenerate O-Ne-Mg cores of helium stars less massive than about 3.5 Msun, whereas the higher-mass, higher kick-velocity neutron stars were formed by the collapses of the iron cores of higher initial mass. The absence of low-velocity single young radio pulsars (Hobbs et al. 2005) is consistent with the model proposed by Podsiadlowski et al. (2004), in which the electron-capture collapse of degenerate O-Ne-Mg cores can only occur in binary systems, and not in single stars.

E. P. J. van den Heuvel

2007-04-10T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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
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241

William Fowler and Elements in the Stars  

NLE Websites -- All DOE Office Websites (Extended Search)

William Fowler and Elements in the Stars Resources with Additional Information William A. Fowler Courtesy AIP Emilio Segrè Visual Archives 'William A. Fowler ... shared the 1983 Nobel Prize in physics for his research into the creation of chemical elements inside stars ... . During his career in nuclear physics and nuclear astrophysics, which spanned more that 60 years, Fowler was primarily concerned with studies of fusion reactions--how the nuclei of lighter chemical elements fuse to create the heavier ones in a process known as nucleosynthesis. In 1957, Fowler coauthored ... the seminal paper "Synthesis of the Elements in the Stars", [which] showed that all of the elements from carbon to uranium could be produced by nuclear processes in stars, starting only with the hydrogen and helium produced in the Big Bang.

242

ENERGY STAR SNAPSHOT … Spring 2009  

NLE Websites -- All DOE Office Websites (Extended Search)

09 09 Introduction In 2008, leading commercial and industrial organizations outpaced their 2007 efforts to improve energy efficiency and reduce greenhouse gas emissions. Rating activity continued to be strong, particularly for offices and schools; and new organizations partnering with ENERGY STAR nearly tripled. Recognition for improvement and top performance grew significantly in 2008. Almost 3,300 buildings earned the ENERGY STAR, bringing the overall total to more than 6,200 facilities representing over 1 billion square feet. Twenty-seven partners reduced overall energy use to be designated as an ENERGY STAR Leader, 14 for the first time. By the end of the year, a total of 65 partners had demonstrated reaching such milestones. The ENERGY STAR Snapshot provides an at-a-glance summary of the key performance indicators

243

StarTex Power | Open Energy Information  

Open Energy Info (EERE)

StarTex Power StarTex Power Jump to: navigation, search Name StarTex Power Place Texas Utility Id 55875 Utility Location Yes Ownership R NERC ERCOT Yes Activity Retail Marketing Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png No rate schedules available. Average Rates Residential: $0.1150/kWh Commercial: $0.1260/kWh Industrial: $0.1210/kWh References ↑ "EIA Form EIA-861 Final Data File for 2010 - File1_a" Retrieved from "http://en.openei.org/w/index.php?title=StarTex_Power&oldid=411605" Categories: EIA Utility Companies and Aliases Utility Companies

244

Blue Star Energy Services | Open Energy Information  

Open Energy Info (EERE)

BlueStar) BlueStar) Jump to: navigation, search Name Blue Star Energy Services Place Illinois Utility Id 55722 Utility Location Yes Ownership R NERC Location RFC NERC RFC Yes Activity Retail Marketing Yes References EIA Form EIA-861 Final Data File for 2010 - File1_a[1] LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! This article is a stub. You can help OpenEI by expanding it. Utility Rate Schedules Grid-background.png No rate schedules available. Average Rates Residential: $0.1180/kWh Commercial: $0.0687/kWh References ↑ "EIA Form EIA-861 Final Data File for 2010 - File1_a" Retrieved from "http://en.openei.org/w/index.php?title=Blue_Star_Energy_Services&oldid=409064" Categories: EIA Utility Companies and Aliases

245

Haier: ENERGY STAR Referral (PRTS21SAC*)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred the matter of Haier refrigerator model PRTS21SAC* to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

246

Hadronic matter and rapidly rotating compact stars  

SciTech Connect

In part one of this paper the authors review the present status of neutron star matter calculations, and introduce a representative collection of realistic nuclear equations of state which are derived for different assumptions about the physical behavior of dense matter (baryon populations, pion condensation, possible transition of baryon matter to quark matter). Part two deals with the theoretical determination of the minimum possible rotational periods of neutron stars, performed in the framework of general relativity, whose knowledge serves to distinguish between pulsars that can be understood as rotating neutron stars and those that cannot. Likely candidates for the latter are hypothetical strange stars. Their properties are discussed in the third part of this contribution.

Weber, F.; Kettner, C. [Univ. of Munich (Germany). Inst. for Theoretical Physics; Glendenning, N.K. [Lawrence Berkeley Lab., CA (United States). Nuclear Science Div.

1994-03-01T23:59:59.000Z

247

Electron stars for holographic metallic criticality  

E-Print Network (OSTI)

We refer to the ground state of a gravitating, charged ideal fluid of fermions held at a finite chemical potential as an `electron star'. In a holographic setting, electron stars are candidate gravity duals for strongly interacting finite fermion density systems. We show how electron stars develop an emergent Lifshitz scaling at low energies. This IR scaling region is a consequence of the two way interaction between emergent quantum critical bosonic modes and the finite density of fermions. By integrating from the IR region to an asymptotically AdS_4 spacetime, we compute basic properties of the electron stars, including their electrical conductivity. We emphasize the challenge of connecting UV and IR physics in strongly interacting finite density systems.

Sean A. Hartnoll; Alireza Tavanfar

2011-01-06T23:59:59.000Z

248

Simulations Reveal Unusual Death for Ancient Stars  

NLE Websites -- All DOE Office Websites (Extended Search)

Certain primordial stars-those between 55,000 and 56,000 times the mass of our Sun, or solar masses-may have died unusually. In death, these objects-among the Universe's...

249

Transport coefficients in superfluid neutron stars  

E-Print Network (OSTI)

We study the shear and bulk viscosity coefficients as well as the thermal conductivity as arising from the collisions among phonons in superfluid neutron stars. We use effective field theory techniques to extract the allowed phonon collisional processes, written as a function of the equation of state and the gap of the system. The shear viscosity due to phonon scattering is compared to calculations of that coming from electron collisions. We also comment on the possible consequences for r-mode damping in superfluid neutron stars. Moreover, we find that phonon collisions give the leading contribution to the bulk viscosities in the core of the neutron stars. We finally obtain a temperature-independent thermal conductivity from phonon collisions and compare it with the electron-muon thermal conductivity in superfluid neutron stars.

Tolos, Laura; Sarkar, Sreemoyee; Tarrus, Jaume

2014-01-01T23:59:59.000Z

250

Neutron stars in Einstein-aether theory  

E-Print Network (OSTI)

As current and future experiments probe strong gravitational regimes around neutron stars and black holes, it is desirable to have theoretically sound alternatives to general relativity against which to test observations. Here we study the consequences of one such generalization, Einstein-aether theory, for the properties of non-rotating neutron stars. This theory has a parameter range that satisfies all current weak-field tests. We find that within this range it leads to lower maximum neutron star masses, as well as larger surface redshifts at a particular mass, for a given nuclear equation of state. For non-rotating black holes and neutron stars, the innermost stable circular orbit is only slightly modified in this theory.

Christopher Eling; Ted Jacobson; M. Coleman Miller

2007-05-10T23:59:59.000Z

251

Midea: ENERGY STAR Referral (MWF-08CR)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred the matter of Westpointe-brand room air conditioner model MWF-08CR to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

252

ASKO: ENERGY STAR Referral (D5122XXLB)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred the matter of ASKO dishwasher model D5122XXLB to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

253

Danby: ENERGY STAR Referral (DAC10507EE)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred the matter of Danby room air conditioner model DAC10507EE to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

254

Bill Nye (Energy All Stars Presentation)  

Energy.gov (U.S. Department of Energy (DOE))

Bill Nye the Science Guy delivered this presentation on space and the lessons about climate change that can be gleaned from the other planets in our solar system at the Energy All Stars event on...

255

ENERGY STAR Webinar: Portfolio Manager 101  

Office of Energy Efficiency and Renewable Energy (EERE)

Join us as we introduce and demonstrate the core functionality of EPAs new ENERGY STAR Portfolio Manager tool. Attendees will learn how to: navigate the new Portfolio Manager; add a property and...

256

Beryllium Abundances of Solar-Analog Stars  

Science Journals Connector (OSTI)

......from our recent research project on a large homogeneous sample of solar analog stars, which aims...comparison of the observed solar flux energy distribution at the Earth...from Kuruczs (1993) ATLAS9 solar model atmosphere (reduced......

Yoichi Takeda; Akito Tajitsu; Satoshi Honda; Satoshi Kawanomoto; Hiroyasu Ando; Takashi Sakurai

2011-06-25T23:59:59.000Z

257

Samsung: ENERGY STAR Referral (RF26VAB)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred the matter of Samsung refrigerator-freezer model RF26VAB to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

258

Dara Enterprises 1974 Star Trek Trivia Quiz  

E-Print Network (OSTI)

DARA ENTERPRISES 1974 STAR TREK TRIVIA QUIZ FILL OUT THE ENCLOSED ANSWER SHEET TO THE BEST OF YOUR KNOWLEDGE, AND RETURN IT TO THE DARA ENTERPRISES TABLE BEFORE CLOSING ON SUNDAY, FEBRUARY 17. WINNERS WILL BE ANNOUNCED AND PRIZES AWARDED...

259

ENERGY STAR Solid-State Lighting Workshop  

Energy.gov (U.S. Department of Energy (DOE))

Workshop Purpose: To prepare manufacturers for the launch of the ENERGY STAR SSL program in late September by sharing information on the state of the SSL market, status of relevant test procedures,...

260

Thread-leaf Blue Star Amsonia hubrichtii  

E-Print Network (OSTI)

-20 inches tall. Upright. 8-14 inches tall. HABIT Early flowering. Light blue star- shaped flowers. Fine perennial for the right place. Right Perennial, Right Place Cornell University Department of Horticulture

Note: This page contains sample records for the topic "waha lone star" 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

EPA ENERGY STAR Webcast- Portfolio Manager 201  

Energy.gov (U.S. Department of Energy (DOE))

Continue to learn about EPAs new ENERGY STAR Portfolio Manager tool, with a deeper dive into more advanced functionalities such as: managing and tracking changes to your property uses over time;...

262

EPA ENERGY STAR Webcast- Portfolio Manager 101  

Office of Energy Efficiency and Renewable Energy (EERE)

Join us as we introduce and demonstrate the core functionality of EPAs new ENERGY STAR Portfolio Manager tool. Attendees will learn how to: navigate the new Portfolio Manager; add a property and...

263

Condensation temperature trends among stars with planets  

E-Print Network (OSTI)

Results from detailed spectroscopic analyses of stars hosting massive planets are employed to search for trends between abundances and condensation temperatures. The elements C, S, Na, Mg, Al, Ca, Sc, Ti, V, Cr, Mn, Fe, Ni and Zn are included in the analysis of 64 stars with planets and 33 comparison stars. No significant trends are evident in the data. This null result suggests that accretion of rocky material onto the photospheres of stars with planets is not the primary explanation for their high metallicities. However, the differences between the solar photospheric and meteoritic abundances do display a weak but significant trend with condensation temperature. This suggests that the metallicity of the sun's envelope has been enriched relative to its interior by about 0.07 dex.

Guillermo Gonzalez

2005-12-08T23:59:59.000Z

264

Michael Liebreich (Energy All Stars Presentation)  

Energy.gov (U.S. Department of Energy (DOE))

Michael Liebreich, CEO of Bloomberg New Energy Finance, delivered this presentation on the energy economy at the Energy All Stars event on January 19, 2013, at the US Department of Energy in...

265

Alliance Star Energy LLC | Open Energy Information  

Open Energy Info (EERE)

Alliance Star Energy LLC Place: California References: EIA Form EIA-861 Final Data File for 2010 - File220101 EIA Form 861 Data Utility Id 56929 This article is a stub. You can...

266

Energy Star for Hospitals 2011 Update: Progression or Regression?  

E-Print Network (OSTI)

Energy Star for Hospitals 2011 Update: Progression or Regression? Brandon E. Travis1 1 Project Manager, SSRCx, 2995 Sidco Drive, Nashville, TN 37204, U.S.A. Email: btravis@ssr-inc.com Abstract: The Energy Star performance rating system...ENERGY STAR for Hospitals 2011 Update: Progression or Regression? Brandon E. Travis October 24, 2012 History of Energy Star Energy Star for Hospitals Critique & Conclusions Outline ? Benchmarks are important ? Energy efficiency void...

Travis, B.

2012-01-01T23:59:59.000Z

267

On surface tension for compact stars  

E-Print Network (OSTI)

In an earlier treatment it was demonstrated that general relativity gives higher values of surface tension in strange stars with quark matter than neutron stars.We generate the modified Tolman-Oppenheimer-Volkoff equation to incorporate anisotropic matter and use this to show that pressure anisotropy provides for a wide range of behaviour in the surface tension than is the case with isotropic pressures. In particular it is possible that anisotropy drastically decreases the value of the surface tension.

R. Sharma; S. D. Maharaj

2007-08-24T23:59:59.000Z

268

Xenon in Mercury-Manganese Stars  

E-Print Network (OSTI)

Previous studies of elemental abundances in Mercury-Manganese (HgMn) stars have occasionally reported the presence of lines of the ionized rare noble gas Xe II, especially in a few of the hottest stars with Teff ~ 13000--15000 K. A new study of this element has been undertaken using observations from Lick Observatory's Hamilton Echelle Spectrograph. In this work, the spectrum synthesis program UCLSYN has been used to undertake abundance analysis assuming LTE. We find that in the Smith & Dworetsky sample of HgMn stars, Xe is vastly over-abundant in 21 of 22 HgMn stars studied, by factors of 3.1--4.8 dex. There does not appear to be a significant correlation of Xe abundance with Teff. A comparison sample of normal late B stars shows no sign of Xe II lines that could be detected, consistent with the expected weakness of lines at normal abundance. The main reason for the previous lack of widespread detection in HgMn stars is probably due to the strongest lines being at longer wavelengths than the photographic blue. The lines used in this work were 4603.03A, 4844.33A and 5292.22A.

M. M. Dworetsky; J. L. Persaud; K. Patel

2008-01-16T23:59:59.000Z

269

An Overview of STAR Experimental Results  

E-Print Network (OSTI)

With large acceptance and excellent particle identification, STAR is one of the best mid-rapidity collider experiments for studying high-energy nuclear collisions. The STAR experiment provides full information on initial conditions, properties of the hot and dense medium as well as the properties at freeze-out. In Au+Au collisions at $\\sqrt{s_{NN}} = 200$ GeV, STAR's focus is on the nature of the sQGP produced at RHIC. In order to explore the properties of the QCD phase diagram, since 2010, the experiment has collected sizable data sets of Au+Au collisions at the lower collision energy region where the net-baryon density is large. At the 2014 Quark Matter Conference, the STAR experiment made 16 presentations that cover physics topics including {\\it collective dynamics}, {\\it electromagnetic probes}, {\\it heavy flavor}, {\\it initial state physics}, {\\it jets}, {\\it QCD phase diagram}, {\\it thermodynamics and hadron chemistry}, and {\\it future experimental facilities, upgrades, and instrumentation} [1-16]. In this overview we will highlight a few results from the STAR experiment, especially those from the recent measurements of the RHIC beam energy scan program. At the end, instead of a summary, we will discuss STAR's near future physics programs at RHIC.

N. Xu

2014-08-15T23:59:59.000Z

270

Observational Cosmology With Semi-Relativistic Stars  

E-Print Network (OSTI)

Galaxy mergers lead to the formation of massive black hole binaries which can accelerate background stars close to the speed of light. We estimate the comoving density of ejected stars with a peculiar velocity in excess of $0.1c$ or $0.5c$ to be $\\sim 10^{10}$ and $10^5$ Gpc$^{-3}$ respectively, in the present-day Universe. Semi-relativistic giant stars will be detectable with forthcoming telescopes out to a distance of a few Mpc, where their proper motion, radial velocity, and age, can be spectroscopically measured. In difference from traditional cosmological messengers, such as photons, neutrinos, or cosmic-rays, these stars shine and so their trajectories need not be directed at the observer for them to be detected. Tracing the stars to their parent galaxies as a function of speed and age will provide a novel test of the equivalence principle and the standard cosmological parameters. Semi-relativistic stars could also flag black hole binaries as gravitational wave sources for the future eLISA observatory.

Loeb, Abraham

2014-01-01T23:59:59.000Z

271

Astronomy 9603B -Star Formation Star Formation: Astronomy 9603B (Winter 2012)  

E-Print Network (OSTI)

Astronomy 9603B - Star Formation Star Formation: Astronomy 9603B (Winter 2012) Lecturer: Prof below. Contact information: Martin Houde Associate Professor Department of Physics and Astronomy Room 207, Physics and Astronomy Building E-mail: mhoude2@uwo.ca Phone: (519) 661-2111 x: 86711 (office) Fax

Lennard, William N.

272

Magnetism in Herbig Ae/Be stars and the link to the Ap/Bp stars  

E-Print Network (OSTI)

Among the A/B stars, about 5% host large-scale organised magnetic fields. These magnetic stars show also abundance anomalies in their spectra, and are therefore called the magnetic Ap/Bp stars. Most of these stars are also slow rotators compared to the normal A and B stars. Today, one of the greatest challenges concerning the Ap/Bp stars is to understand the origin of their slow rotation and their magnetic fields. The favoured hypothesis for the latter is that the fields are fosils, which implies that the magnetic fields subsist throughout the different evolutionary phases, and in particular during the pre-main sequence phase. The existence of magnetic fields at the pre-main sequence phase is also required to explain the slow rotation of Ap/Bp stars. During the last 3 years we performed a spectropolarimetric survey of the Herbig Ae/Be stars in the field and in young clusters, in order to investigate their magnetism and rotation. These investigations have resulted in the detection and/or confirmation of magnet...

Alecian, E; Wade, G A; Bagnulo, S; Bhm, T; Bouret, J -C; Donati, J -F; Folsom, C; Grunhut, J; Landstreet, J D; Marsden, S C; Petit, P; Ramrez, J; Silvester, J

2008-01-01T23:59:59.000Z

273

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

274

E-Print Network 3.0 - a-type hyper-velocity star Sample Search...  

NLE Websites -- All DOE Office Websites (Extended Search)

Magnetic fields in A stars Summary: to emerge. Keywords. stars: magnetic fields, MHD, stars: A-type 1. Introduction After several decades... ) explicitly addresses A-type...

275

EPA ENERGY STAR: Tackling Growth in Home Electronics and Small Appliances  

E-Print Network (OSTI)

ICF Consulting. 2003. Energy Star Market Penetration ReportConsulting. . 2004. Energy Star Market Penetration Reportmarket data. Figure 4. ENERGY STAR Market Penetration ENERGY

Sanchez, Marla Christine

2008-01-01T23:59:59.000Z

276

E-Print Network 3.0 - applied research star Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

stars. A single ... Source: Pols, Onno - Sterrenkundig Instituut, Universiteit Utrecht Collection: Physics 6 Star clusters near intermediate and high mass young stars...

277

Herbig Ae/Be Stars in the Magellanic Bridge  

Science Journals Connector (OSTI)

We have found Herbig Ae/Be star candidates in the western region of the Magellanic Bridge. Using the near-infrared camera SIRIUS and the 1.4 m telescope IRSF, we surveyed ~3.0 ? 1.3 (24 ? 36, -75.0 ? -73.7) in the J, H, and Ks bands. On the basis of colors and magnitudes, about 200 Herbig Ae/Be star candidates are selected. Considering the contaminations by miscellaneous sources, such as foreground stars and early-type dwarfs in the Magellanic Bridge, we estimate that about 80 (?40%) of the candidates are likely to be Herbig Ae/Be stars. We also found one concentration of the candidates at the young star cluster NGC 796, strongly suggesting the existence of pre-main-sequence (PMS) stars in the Magellanic Bridge. This is the first detection of PMS star candidates in the Magellanic Bridge, and if they are genuine PMS stars, this could be direct evidence of recent star formation. However, the estimate of the number of Herbig Ae/Be stars depends on the fraction of classical Be stars, and thus a more precise determination of the Be star fraction or observations to differentiate between the Herbig Ae/Be stars and classical Be stars are required.

Shogo Nishiyama; Yasuaki Haba; Daisuke Kato; Daisuke Baba; Hirofumi Hatano; Motohide Tamura; Yasushi Nakajima; Akika Ishihara; Tetsuya Nagata; Koji Sugitani; Noriyuki Matsunaga; Hinako Fukushi; Nobuhiko Kusakabe; Shuji Sato

2007-01-01T23:59:59.000Z

278

ENERGY STAR portfolio-wide recognition | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR portfolio-wide recognition ENERGY STAR portfolio-wide recognition 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Earn recognition for your building or plant Earn recognition for your commercial construction project ENERGY STAR portfolio-wide recognition

279

ENERGY STAR sales tools for service and product providers | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

sales tools for service and product providers sales tools for service and product providers 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 How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner ENERGY STAR service & product provider training series Service and product provider's marketing toolkit ENERGY STAR sales tools for service and product providers

280

Quasiuniversal properties of neutron star mergers  

E-Print Network (OSTI)

Binary neutron star mergers are studied using nonlinear 3+1 numerical relativity simulations and the analytical effective-one-body (EOB) model. The EOB model predicts quasiuniversal relations between the mass-rescaled gravitational wave frequency and the binding energy at the moment of merger, and certain dimensionless binary tidal coupling constants depending on the stars Love numbers, compactnesses and the binary mass ratio. These relations are quasiuniversal in the sense that, for a given value of the tidal coupling constant, they depend significantly neither on the equation of state nor on the mass ratio, though they do depend on stars spins. The spin dependence is approximately linear for small spins aligned with the orbital angular momentum. The quasiuniversality is a property of the conservative dynamics; nontrivial relations emerge as the binary interaction becomes tidally dominated. This analytical prediction is qualitatively consistent with new, multi-orbit numerical relativity results for the relevant case of equal-mass irrotational binaries. Universal relations are thus expected to characterize neutron star mergers dynamics. In the context of gravitational wave astronomy, these universal relations may be used to constrain the neutron star equation of state using waveforms that model the merger accurately.

Sebastiano Bernuzzi; Alessandro Nagar; Simone Balmelli; Tim Dietrich; Maximiliano Ujevic

2014-02-25T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Stars and statistical physics: A teaching experience  

Science Journals Connector (OSTI)

The physics of stars their workings and their evolution is a goldmine of problems in statistical mechanics and thermodynamics. We discuss many examples that illustrate the possibility of deepening students knowledge of statistical mechanics by an introductory study of stars. The matter constituting the various stellar objects provides examples of equations of state for classical or quantal and relativistic or non-relativistic gases. Maximum entropy can be used to characterize thermodynamic and gravitational equilibrium which determines the structure of stars and predicts their instability above a certain mass. Contraction accompanying radiation induces either heating or cooling which explains the formation of stars above a minimum mass. The characteristics of the emitted light are understood from blackbody radiation and more precisely from the BoltzmannLorentz kinetic equation for photons. The luminosity is governed by the transport of heat by photons from the center to the surface. Heat production by thermonuclear fusion is determined by microscopic balance equations. The stability of the steady state of stars is controlled by the interplay of thermodynamics and gravitation.

Roger Balian; Jean-Paul Blaizot

1999-01-01T23:59:59.000Z

282

Magnetism of Herbig Ae/Be stars  

E-Print Network (OSTI)

Observations of magnetic fields of stars at the pre-main sequence phase can provide important new insights into the complex physics of the late stages of star formation. This is especially true at intermediate stellar masses, where magnetic fields are strong and globally organised, and therefore most amenable to direct study. Recent circularly-polarised spectroscopic observations of pre-main sequence Herbig Ae/Be stars have revealed the presence of organised magnetic fields in the photospheres of a small fraction of these objects. To date, 9 magnetic HAeBe stars have been detected, and those detections confirmed by repeated observations. The morphology and variability of their Stokes V signatures indicates that their magnetic fields have important dipole components of kG strength, and that the dipole is stable on timescales ofat least years. These magnetic stars exhibit a large range of stellar mass, from about 2-13 solar masses, and diverse rotational properties, with vsini from a few km/s to 200 km/s. Most ...

Wade, G A; Grunhut, J; Catala, C; Bagnulo, S; Folsom, C P; Landstreet, J D

2009-01-01T23:59:59.000Z

283

Tidal Love Numbers of Neutron Stars  

SciTech Connect

For a variety of fully relativistic polytropic neutron star models we calculate the star's tidal Love number k{sub 2}. Most realistic equations of state for neutron stars can be approximated as a polytrope with an effective index n {approx} 0.5-1.0. The equilibrium stellar model is obtained by numerical integration of the Tolman-Oppenheimer-Volkhov equations. We calculate the linear l = 2 static perturbations to the Schwarzschild spacetime following the method of Thorne and Campolattaro. Combining the perturbed Einstein equations into a single second-order differential equation for the perturbation to the metric coefficient g{sub tt} and matching the exterior solution to the asymptotic expansion of the metric in the star's local asymptotic rest frame gives the Love number. Our results agree well with the Newtonian results in the weak field limit. The fully relativistic values differ from the Newtonian values by up to {approx}24%. The Love number is potentially measurable in gravitational wave signals from inspiralling binary neutron stars.

Hinderer, Tanja [Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853 (United States)], E-mail: tph25@cornell.edu

2008-04-20T23:59:59.000Z

284

Young Neutron Stars and Their Wind Nebulae  

E-Print Network (OSTI)

With Teragauss magnetic fields, surface gravity sufficiently strong to significantly modify light paths, central densities higher than that of a standard nucleus, and rotation periods of only hundredths of a second, young neutron stars are sites of some of the most extreme physical conditions known in the Universe. They generate magnetic winds with particles that are accelerated to energies in excess of a TeV. These winds form synchrotron-emitting bubbles as the particle stream is eventually decelerated to match the general expansion caused by the explosion that formed the neutron stars. The structure of these pulsar wind nebulae allow us to infer properties of the winds and the pulsating neutron stars themselves. The surfaces of the the stars radiate energy from the rapidly cooling interiors where the physical structure is basically unknown because of our imprecise knowledge of the strong interaction at ultrahigh densities. Here I present a summary of recent measurements that allow us to infer the birth properties of neutron stars and to probe the nature of their winds, the physics of their atmospheres, and the structure of their interiors.

Patrick Slane

2005-05-24T23:59:59.000Z

285

CalStar Products | Open Energy Information  

Open Energy Info (EERE)

CalStar Products CalStar Products Jump to: navigation, search Name CalStar Products Place Newark, California Zip 94560 Product California-based environmentally friendly brick and paving stone manufacturer. Coordinates 44.690435°, -71.951685° 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":44.690435,"lon":-71.951685,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

286

Ms. Leslie Jones ENERGY STAR Program  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

December 21,2010 December 21,2010 U.S. Environmental Protection Agency 1200 Pennsylvania Avenue, NW Room 62023 Washington, DC 20460 Dear Ms. Jones: On November 24, 2010, the United States Department of Energy (DOE) notified Haier that DOE had tested the Haier room air conditioner model ESA3087 as part of the ENERGY STAR Testing Pilot Program, and that, according to Stage I testing, this model exceeded allowable ENERGY STAR energy-efficiency requirements by 18 percent. DOE gave Haier until December 3, 2010, to request additional testing or have this matter referred to the United States Environmental Protection Agency (EPA) for disqualification from the ENERGY STAR program. On December 2, Haier notified DOE that it was in the process of voluntarily removing model

287

Five Star Technologies | Open Energy Information  

Open Energy Info (EERE)

Star Technologies Star Technologies Jump to: navigation, search Name Five Star Technologies Place Independence, Ohio Zip 44131 Sector Solar Product US manufacturer of inks and pastes for the electronics industry; in solar, manufactures silver paste for screen printing PV cells. Coordinates 44.356672°, -91.421315° 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":44.356672,"lon":-91.421315,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

288

ENERGY STAR Homes Program | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

ENERGY STAR Homes Program ENERGY STAR Homes Program ENERGY STAR Homes Program < Back Eligibility Installer/Contractor Multi-Family Residential Residential Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Maximum Rebate Single-Family: $26,000 per unit Multiple Single-Family (townhomes): $17,000 per unit Multi-Family Buildings: $12,000 per unit Program Info Funding Source New Jersey Societal Benefits Charge (public benefits fund) State New Jersey Program Type State Rebate Program Rebate Amount Varies by efficiency level and type of residence Provider New Jersey Clean Energy Program : Note: The Smart Growth requirement for incentive eligibility has been removed in areas affected by Hurricane Sandy, for projects enrolled from

289

STATE AND LOCAL GOVERNMENTS LEVERAGING ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Federal agencies and state and local governments across the country are taking bold steps to protect the environment and lower energy costs by adopting Federal agencies and state and local governments across the country are taking bold steps to protect the environment and lower energy costs by adopting policies that leverage EPA's ENERGY STAR tools to reduce energy use in commercial buildings, through both required policy measures and voluntary campaigns. This document provides a summary of federal, state, and local efforts that refer to ENERGY STAR tools. Download an interactive copy at www.energystar.gov/government. POLICIES LEVERAGING ENERGY STAR TOOLS Jurisdiction Policy Summary Alabama Executive Order 25 December 2011 By December Fiscal Year 2015, all state departments and agencies will implement energy efficiency measures in order to achieve a 30 percent reduction in energy consumption relative to Fiscal Year 2005

290

Ms. Leslie Jones ENERGY STAR Program  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

September 20, 2011 September 20, 2011 U.S. Environmental Protection Agency 1200 Pennsylvania Avenue, NW Room 62023 Washington, DC 20460 Dear Ms. Jones: On March 7, 2011, the United States Depmiment of Energy (DOE) notified Baier America Trading, L.L.C. (Baier) that DOE had completed testing of Baier refrigerator model PRTS21SAC* under the ENERGY STAR Verification Testing Pilot Program and confirmed that the model did not meet ENERGY STAR energy efficiency requirements. DOE gave Baier until March 28, 2011, to provide conclusive manufacturing or design evidence or quality assurance information to rebut DOE testing results, which showed that this product did not meet the ENERGY STAR Program's energy efficiency requirement. Baier responded to DOE in a letter dated March 22, 2011, contending that the results of

291

ENERGY STAR Score for Data Centers  

NLE Websites -- All DOE Office Websites (Extended Search)

Data Centers in the United States Page 1 Data Centers in the United States Page 1 ENERGY STAR Score for Data Centers in the United States Technical Reference OVERVIEW The ENERGY STAR Score for Data Centers applies to spaces specifically designed and equipped to meet the needs of high density computing equipment such as server racks, used for data storage and processing. The objective of the ENERGY STAR score is to provide a fair assessment of the energy performance of a property relative to its peers, taking into account the climate, weather, and business activities at the property. To identify the aspects of building activity that are significant drivers of energy use and then normalize for those factors, a statistical analysis of

292

ENERGY STAR Success Story: Staples, Inc.  

NLE Websites -- All DOE Office Websites (Extended Search)

STAR Success Story: STAR Success Story: Staples, Inc. Staples, the world's largest office products company, has been an energy management and environmental leader in the retail industry for several years. Staples first partnered with the U.S. Environmental Protection Agency's (EPA) Green Lights Program, the predecessor to ENERGY STAR, and in 1999, won the Green Lights Partner of the Year recognition. Staples also has the distinction of being one of the first retailers to benchmark its entire portfolio of over 1,500 retail stores and 200 distribution centers. Even as the company's building portfolio has grown, with total square footage increasing by over 6 percent in just the past three years, Staples has reduced its building portfolio-wide energy usage by more than 11.4%, and recently became the first retailer

293

DarkStar VI | Open Energy Information  

Open Energy Info (EERE)

DarkStar VI DarkStar VI Jump to: navigation, search Name DarkStar VI Place Collinsville, Illinois Zip 62234-2022 Sector Services Product Manufacturer of biodiesel processing equipment and supplier of accessories, information and services. Coordinates 36.720014°, -79.91284° 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":36.720014,"lon":-79.91284,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

294

Ms. Leslie Jones ENERGY STAR Program  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

June 6, 2012 June 6, 2012 U.S. Environmental Protection Agency 1200 Pennsylvania Avenue, NW Room62023 Washington, DC 20460 Dear Ms. Jones: On October 28, 2011, the United States Depatiment of Energy (DOE) notified Friedrich Air Conditioning Company (Friedrich) that DOE had completed testing of Friedrich room air conditioner models WS12Cl0 and WS13C30 under the ENERGY STAR Testing Pilot Program and confirmed that these models do not meet the ENERGY STAR energy efficiency requirement of9.4 EER. On November 3, 201 I, DOE notified Friedrich that its room air conditioner model USI2C30 does not meet the ENERGY STAR energy efficiency requirement of9.4 EER. In each notice, DOE gave Friedrich twenty days to provide conclusive manufacturing or design evidence or quality assurance information on why DOE testing showed that these models do not

295

TRAN-STAR EXECUTIVE LIMOUSINE COMPANY  

NLE Websites -- All DOE Office Websites (Extended Search)

TRAN-STAR EXECUTIVE LIMOUSINE COMPANY TRAN-STAR EXECUTIVE LIMOUSINE COMPANY http://www.tranexec.com 20% off published rates for BNL Our reservation center is open 24 hours a day, 365 days a year, so you will always talk to a live agent who has direct contact with our chauffeurs. You can make reservations via phone, website or a simple e-mail to customerservice@tranexec.com once a profile has been established. Our advanced reservation system will track any flight and you can rest assured someone will always be there to meet the arriving passenger, no matter what time the flight arrives. http://www.tranexec.com/TranStarSalesBrochure.pdf These rates are inclusive rates, meaning they include gratuity, taxes....everything. They do not include parking or tolls

296

Christmas burst reveals neutron star collision  

NLE Websites -- All DOE Office Websites (Extended Search)

Christmas burst reveals neutron star collision Christmas burst reveals neutron star collision Christmas burst reveals neutron star collision Called the Christmas Burst, GRB 101225A was freakishly lengthy and it produced radiation at unusually varying wavelengths. December 1, 2011 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Contact

297

On Star Formation Rates in Dwarf Galaxies  

E-Print Network (OSTI)

We present evolutionary synthesis models of starbursts on top of old stellar populations to investigate in detailed time evolution the relation between Ha luminosity and star formation rate (SFR). The models show that several effects have an impact on the ratio between L(Ha) and SFR. Metallicity different from solar abundance, a time delay between star formation and maximum Ha-luminosity, and a varying stellar initial mass function give rise to strong variations in the ratio of Ha luminosity to SFR and can cause large errors in the determination of the SFR when employing well-known calibrations. When studying star-bursting dwarf galaxies, and sub-galactic fragments at high redshift, which show SFR fluctuating on short timescales, these effects can add up to errors of two orders of magnitude compared with the calibrations. To accurately determine the true current SFR additional data in combination with models for the spectral energy distribution are needed.

Peter M. Weilbacher; Uta Fritze-v. Alvensleben

2001-05-16T23:59:59.000Z

298

Star Formation in Las Campanas Compact Groups  

E-Print Network (OSTI)

Compact groups (CGs) of galaxies offer an exceptional laboratory for the study of dense galaxian environments --- where interactions, tidally induced activity, and mergers are expected to be at their highest rate of occurrence. Here, we present first results from a new catalogue of compact groups, one based upon the Las Campanas Redshift Survey (LCRS). Using the equivalent width of [OII]3727, we have studied the star formation activity in LCRS CGs: we find strong evidence of depressed star formation in CGs relative to that in loose groups or the field. Although much of this effect can be ascribed to morphological mix (CGs contain a high fraction of early-type galaxies), there is some evidence that the star formation rate in late-type galaxies is particularly deficient --- perhaps only one-half to one-third that of field spirals. We conclude that gas stripping mechanisms may play a role in CG environments.

Sahar S. Allam; Douglas L. Tucker; Huan Lin; Yasuhiro Hashimoto

1999-07-11T23:59:59.000Z

299

Exploring the magnetic topologies of cool stars  

E-Print Network (OSTI)

Magnetic fields of cool stars can be directly investigated through the study of the Zeeman effect on photospheric spectral lines using several approaches. With spectroscopic measurement in unpolarised light, the total magnetic flux averaged over the stellar disc can be derived but very little information on the field geometry is available. Spectropolarimetry provides a complementary information on the large-scale component of the magnetic topology. With Zeeman-Doppler Imaging (ZDI), this information can be retrieved to produce a map of the vector magnetic field at the surface of the star, and in particular to assess the relative importance of the poloidal and toroidal components as well as the degree of axisymmetry of the field distribution. The development of high-performance spectropolarimeters associated with multi-lines techniques and ZDI allows us to explore magnetic topologies throughout the Hertzsprung-Russel diagram, on stars spanning a wide range of mass, age and rotation period. These observations b...

Morin, J; Petit, P; Albert, L; Auriere, M; Cabanac, R; Catala, C; Delfosse, X; Dintrans, B; Fares, R; Forveille, T; Gastine, T; Jardine, M; Konstantinova-Antova, R; Lanoux, J; Lignieres, F; Morgenthaler, A; Paletou, F; Velez, J C Ramirez; Solanki, S K; Theado, S; Van Grootel, V

2010-01-01T23:59:59.000Z

300

SED modeling of Young Massive Stars  

E-Print Network (OSTI)

In this contribution, I review the applications and potential limitations of the spectral energy distribution fitting tool that I have developed, with a strong emphasis on the limits to which this tool can be used to improve our understanding of massive star formation. I discuss why our current grid of models cannot be used to distinguish between the several competing theories of massive star formation. I also discuss stellar mass determinations, artificial correlations between parameters in the grid of models, multiplicity, confusion, dust assumptions, and unique fits. I briefly review the improvements we intend to carry out for our next grid of models, which will eliminate many of these limitations. Finally, I show examples of applications of this tool to massive young stars.

Thomas P. Robitaille

2007-11-27T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Energy Star Product Rebates | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Energy Star Product Rebates Energy Star Product Rebates Energy Star Product Rebates < Back Eligibility General Public/Consumer Residential Savings Category Appliances & Electronics Commercial Lighting Lighting Program Info Funding Source New Jersey Societal Benefits Charge (public benefits fund) State New Jersey Program Type State Rebate Program Rebate Amount Lighting: varies Refrigerator: $50 Clothes washers: $50 Provider c/o Honeywell The New Jersey Office of Clean Energy (OCE) offers rebates to state residents who purchase certain energy efficient home appliances. As of April 2, 2013, active rebates exist for energy efficient clothes washers and refrigerators. The program website has a search engine where consumers can look up local retailers offering discounts on compact fluorescent

302

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

303

A new method to derive star formation histories of galaxies from their star cluster distributions  

E-Print Network (OSTI)

Star formation happens in a clustered way which is why the star cluster population of a particular galaxy is closely related to the star formation history of this galaxy. From the probabilistic nature of a mass function follows that the mass of the most-massive cluster of a complete population, M_max, has a distribution with the total mass of the population as a parameter. The total mass of the population is connected to the star formation rate (SFR) by the length of a formation epoch. Since due to evolutionary effects only massive star clusters are observable up to high ages it is convenient to use this M_max(SFR) relation for the reconstruction of a star formation history. The age-distribution of the most-massive clusters can therefore be used to constrain the star formation history of a galaxy. The method, including an assessment of the inherent uncertainties, is introduced with this contribution, while following papers will apply this method to a number of galaxies.

Thomas Maschberger; Pavel Kroupa

2007-05-07T23:59:59.000Z

304

PRECISE DOPPLER MONITORING OF BARNARD'S STAR  

SciTech Connect

We present 248 precise Doppler measurements of Barnard's Star (Gl 699), the second nearest star system to Earth, obtained from Lick and Keck Observatories during the 25 years between 1987 and 2012. The early precision was 20 m s{sup -1} but was 2 m s{sup -1} during the last 8 years, constituting the most extensive and sensitive search for Doppler signatures of planets around this stellar neighbor. We carefully analyze the 136 Keck radial velocities spanning 8 years by first applying a periodogram analysis to search for nearly circular orbits. We find no significant periodic Doppler signals with amplitudes above {approx}2 m s{sup -1}, setting firm upper limits on the minimum mass (Msin i) of any planets with orbital periods from 0.1 to 1000 days. Using a Monte Carlo analysis for circular orbits, we determine that planetary companions to Barnard's Star with masses above 2 M {sub Circled-Plus} and periods below 10 days would have been detected. Planets with periods up to 2 years and masses above 10 M {sub Circled-Plus} (0.03 M {sub Jup}) are also ruled out. A similar analysis allowing for eccentric orbits yields comparable mass limits. The habitable zone of Barnard's Star appears to be devoid of roughly Earth-mass planets or larger, save for face-on orbits. Previous claims of planets around the star by van de Kamp are strongly refuted. The radial velocity of Barnard's Star increases with time at 4.515 {+-} 0.002 m s{sup -1} yr{sup -1}, consistent with the predicted geometrical effect, secular acceleration, that exchanges transverse for radial components of velocity.

Choi, Jieun; Marcy, Geoffrey W.; Howard, Andrew W.; Isaacson, Howard [Department of Astronomy, University of California, Berkeley, CA 94720 (United States)] [Department of Astronomy, University of California, Berkeley, CA 94720 (United States); McCarthy, Chris [Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132 (United States)] [Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132 (United States); Fischer, Debra A. [Department of Astronomy, Yale University, New Haven, CT 06520-8101 (United States)] [Department of Astronomy, Yale University, New Haven, CT 06520-8101 (United States); Johnson, John A. [Department of Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)] [Department of Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States); Wright, Jason T., E-mail: jieun_eb@berkeley.edu [Department of Astronomy, The Pennsylvania State University, University Park, PA 16802 (United States)

2013-02-20T23:59:59.000Z

305

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

306

LANL/Green Star spectrometer tests  

SciTech Connect

The US and Russia have agreed to the joint development of a nondestructive assay system for use to support the dismantlement of nuclear weapons in Russia. This nondestructive assay system will be used to measure plutonium produced by the conversion of Russian nuclear weapons. The NDA system for Russia will be patterned after the ARIES NDA system being constructed at Los Alamos. One goal of the program is to produce an NDA system for use in Russia that maximizes the use of Russian resources to facilitate maintenance and future upgrades. The Green Star SBS50 Single Board Spectrometer system (Green Star Ltd., Moscow, Russia) has been suggested for use as the data acquisition component for gamma ray instruments in the system. Possible uses are for plutonium isotopic analysis and also segmented gamma scanning. Green Star has also developed analysis software for the SBS50. This software, both plutonium isotopic analysis and uranium enrichment analysis, was developed specifically for customs/border inspection applications (low counting rate applications and identification as opposed to quantification) and was not intended for MC and A applications. Because of the relative immaturity of the Green Star plutonium isotopic analysis software (it has been under development for only one year and is patterned after US development circa 1980), it was tentatively agreed, before the tests, that the Russian NDA system would use the Los Alamos PC/FRAM software for plutonium isotopic analysis. However, it was also decided to include the Green Star plutonium isotopic software in the testing, both to quantify its performance for MC and A applications and also to provide additional data to Green Star for further development of their software. The main purpose of the testing was to evaluate the SBS-50 spectrometer as a data acquisition device for use with LANL software.

Sampson, T.E.; Cremers, T.L.; Vo, D.T. [Los Alamos National Lab., NM (United States); Seldiakov, Y.P.; Dorin, A.B.; Kondrashov, M.V. [Green Star, Moscow (Russian Federation); Timoshin, V.I. [VNIINM, Moscow (Russian Federation)

1997-12-01T23:59:59.000Z

307

Mathematical Modelling of Tyndall Star Initiation  

E-Print Network (OSTI)

The superheating that usually occurs when a solid is melted by volumetric heating can produce irregular solid/liquid interfaces. Such interfaces can be visualised in ice, where they are sometimes known as Tyndall stars. This paper describes some of the experimental observations of Tyndall stars and a mathematical model for the early stages of their evolution. The modelling is complicated by the strong crystalline anisotropy, which results in an anisotropic kinetic undercooling at the interface, and it leads to an interesting class of codimension-2 free boundary problems.

Harvey, Peter; Katz, Richard F; Lacey, Andrew A

2015-01-01T23:59:59.000Z

308

Heavy flavor production in the STAR experiment  

E-Print Network (OSTI)

In this paper, recent STAR heavy flavor measurements in proton-proton and heavy-ion collisions are highlighted. We report studies of open charm mesons, reconstructed directly from hadronic decay products, and studies of electrons from semi-leptonic decays of heavy flavor hadrons. We also present J/$\\psi$ measurements via the di-electron decay channel at various collision systems and energies. In Au+Au collisions the energy dependence of J/$\\psi$ production measured at $\\sqrt{s_{NN}}$ = 39, 62.4 and 200 GeV is shown. Finally, prospects of heavy flavor measurements with the STAR detector upgrades are discussed.

Barbara Trzeciak; for the STAR Collaboration

2014-09-11T23:59:59.000Z

309

Multiwavelength Phenomenology of Isolated Neutron Stars  

E-Print Network (OSTI)

After reviewing the multifrequency behaviour of the Isolated Neutron Stars detected so far, we analyze for each object the efficiency of conversion of the star's rotational energy loss into optical, X and gamma radiation. Although the number of pulsars detected at different wavelengths is rather limited, a pattern is seen to emerge from our analysis pointing towards the period derivative as the leading parameter to describe the multifrequency emission of INS. One object in particular, PSR 1509-58, stands out as archetypal for the Pdot-dependence of its luminosity at different wavelengths.

P. Goldoni; C. Musso; P. A. Caraveo; G. F. Bignami

1995-02-07T23:59:59.000Z

310

Detectable Signals from Mergers of Compact Stars  

E-Print Network (OSTI)

Merging neutron stars and neutron star-black holes binaries are powerful sources of gravitational waves. They have also been suggested as possible sources of cosmic gamma-ray bursts and are discussed as sites for the formation of r-process elements. Whereas the first aspect is undoubtable, the latter two are very uncertain. The current status of our knowledge and of the numerical modeling is briefly reviewed and the results of simulations are critically discussed concerning their significance and implications for potentially observable signals.

H. -Th. Janka; M. Ruffert

2001-01-20T23:59:59.000Z

311

[Your Industrial Plant] Earns the ENERGY STAR | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

Industrial Plant] Earns the ENERGY STAR Industrial Plant] Earns the ENERGY STAR 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 Success stories

312

ENERGY STAR Focus on Energy Efficiency in Food Processing | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Food Processing Food Processing 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Tools for benchmarking energy management practices Tools for tracking and benchmarking facility energy performance ENERGY STAR Energy Performance Indicators for plants

313

DataTrends: ENERGY STAR Certification | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR Certification ENERGY STAR Certification 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 Success stories Target Finder

314

Build Your Business with ENERGY STAR | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Build Your Business with ENERGY STAR Build Your Business with ENERGY STAR 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 Success stories

315

Gamma-Ray Bursts and Afterglows from Rotating Strange Stars and Neutron Stars  

E-Print Network (OSTI)

We here discuss a new model of $\\gamma$-ray bursts (GRBs) based on differentially rotating strange stars. Strange stars in this model and differentially rotating neutron stars in the Klu\\'zniak-Ruderman model can produce extremely relativistic, variable fireballs required by GRBs and then become millisecond pulsars. The effect of such pulsars on expansion of the postburst fireballs through magnetic dipole radiation is studied. We show that these two models can explain naturally not only various features of GRBs but also light curves of afterglows.

Z. G. Dai; T. Lu

1998-10-21T23:59:59.000Z

316

Conversion of neutron stars to strange stars as the central engine of gamma-ray bursts  

E-Print Network (OSTI)

We study the conversion of a neutron star to a strange star as a possible energy source for gamma-ray bursts. We use different recent models for the equation of state of neutron star matter and strange quark matter. We show that the total amount of energy liberated in the conversion is in the range of (1-4) 10^{53} ergs (one order of magnitude larger than previous estimates) and is in agreement with the energy required to power gamma-ray burst sources at cosmological distances.

Ignazio Bombaci; Bhaskar Datta

2000-01-27T23:59:59.000Z

317

DOE Energy Star Testing Reveals Inefficient ASKO Dishwasher | Department of  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Energy Star Testing Reveals Inefficient ASKO Dishwasher Energy Star Testing Reveals Inefficient ASKO Dishwasher DOE Energy Star Testing Reveals Inefficient ASKO Dishwasher June 1, 2010 - 2:07pm Addthis DOE testing in support of the Energy Star program has revealed that an ASKO dishwasher (model D5122XXLB), which the company had claimed was Energy Star compliant, consumes more energy than permitted by the Energy Star program. Test results for the ASKO model at issue show that, when tested in accordance with DOE's test procedure, it consumed 12 percent more energy than the Energy Star requirement. Based on this testing, DOE is referring ASKO Model D5122XXLB to the U.S. Environmental Protection Agency for appropriate action with respect to the Energy Star program. DOE's testing revealed that dishwasher model D5122XXLB also may not meet

318

Support for ENERGY STAR Enforcement | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Support for ENERGY STAR Enforcement Support for ENERGY STAR Enforcement Support for ENERGY STAR Enforcement By offering a means for consumers to buy products more energy-efficient than required by law, ENERGY STAR has huge potential to save money for consumers by offering buyers more options in energy-efficient products. In a new initiative, the Department is expanding verification and supporting enforcement of ENERGY STAR to preserve the viability and effectiveness of the ENERGY STAR program. Through independent testing, we are working to verify manufacturer certifications of the efficiency or energy use ratings of their appliances and ensuring manufacturers provide the increased energy and cost savings they advertise. Learn more about ENERGY STAR and DOE's ENERGY STAR Verification Testing

319

Electrolux: ENERGY STAR Referral (FFN09M5HW*)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Electrolux chest freezer model FFN09M5HW* to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

320

Friedrich: ENERGY STAR Referral (YM18M34-A)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Friedrich room air conditioner YM18M34-A to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

Note: This page contains sample records for the topic "waha lone star" 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

Electrolux: ENERGY STAR Referral (EW26SS70I*)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Electrolux room air conditioner model EW26SS70I* to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

322

Perlick: ENERGY STAR Referral (HP48RO-S)  

Energy.gov (U.S. Department of Energy (DOE))

DOE referred Perlick refrigerator HP48RO-S to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

323

Search for Earth-like planets includes LANL star analysis  

NLE Websites -- All DOE Office Websites (Extended Search)

Search for earth-like planets Search for Earth-like planets includes LANL star analysis The mission will not only be able to search for planets around other stars, but also yield...

324

Five ENERGY STAR Room Air Conditioners Fail Testing | Department...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Five ENERGY STAR Room Air Conditioners Fail Testing Five ENERGY STAR Room Air Conditioners Fail Testing August 22, 2011 - 2:00pm Addthis The U.S. Department of Energy's Office of...

325

CORONAL ABUNDANCES IN ORION NEBULA CLUSTER STARS A. Maggio,1  

E-Print Network (OSTI)

pattern of abundances for all stars, although a weak dependence on flare loop size may be present. The abundance of calcium is the only one which appears to vary substantially between stars, but this quantity

Micela, Giusi

326

Hitting the Target: ENERGY STAR SSL Outdoor Area Lighting Webcast  

Energy.gov (U.S. Department of Energy (DOE))

In this October 8, 2009 webcast, ENERGY STAR Program Manager Richard Karney gave an overview of ENERGY STAR criteria covering SSL-based outdoor area and roadway lighting, outdoor wall packs,...

327

Home Performance with ENERGY STAR - 2014 BTO Peer Review | Department...  

Energy Savers (EERE)

ENERGY STAR - 2014 BTO Peer Review Home Performance with ENERGY STAR - 2014 BTO Peer Review Presenter: Ely Jacobsohn, U.S. Department of Energy The goal of Home Performance with...

328

Protoneutron stars within the Brueckner-Bethe-Goldstone theory  

E-Print Network (OSTI)

We study the structure of newly born neutron stars (protoneutron stars) within the finite temperature Brueckner-Bethe-Goldstone theoretical approach including also hyperons. We find that for purely nucleonic stars both finite temperature and neutrino trapping reduce the value of the maximum mass. For hyperonic stars the effect is reversed, because neutrino trapping shifts the appearance of hyperons to larger baryon density and stiffens considerably the equation of state.

O. E. Nicotra; M. Baldo; G. F. Burgio; H. -J. Schulze

2005-06-22T23:59:59.000Z

329

Lithium-rich stars in the Sloan Digital Sky Survey  

E-Print Network (OSTI)

We report the discovery of 23 lithium-rich post-main-sequence stars, identified from moderate-resolution SDSS spectroscopy and confirmed with high-resolution spectra taken at the Hobby-Eberly Telescope. These new Li-rich stars cover a broad range in mass and evolutionary phase, including bright giants and post-AGB stars. The process responsible for preserving or producing excess lithium in a small fraction of evolved stars remains unclear.

Martell, Sarah L

2012-01-01T23:59:59.000Z

330

Generalized equation of state for cold superfluid neutron stars  

SciTech Connect

Mature neutron stars are expected to contain various kinds of superfluids in their interiors. Modeling such stars requires the knowledge of the mutual entrainment couplings between the different condensates. We present a unified equation of state describing the different regions of a neutron star with superfluid neutrons and superconducting protons in its core.

Chamel, N.; Goriely, S. [Institut d'Astronomie et d'Astrophysique, Universite Libre de Bruxelles, B-1050 Brussels (Belgium); Pearson, J. M. [Departement de Physique, Universite de Montreal, Montreal (Quebec), H3C 3J7 (Canada)

2011-09-21T23:59:59.000Z

331

Herbig Ae/Be Stars in the Magellanic Bridge  

E-Print Network (OSTI)

We have found Herbig Ae/Be star candidates in the western region of the Magellanic Bridge. Using the near infrared camera SIRIUS and the 1.4 m telescope IRSF, we surveyed about 3.0 deg x 1.3 deg (24 deg Bridge, we estimate that about 80 (about 40%) of the candidates are likely to be Herbig Ae/Be stars. We also found one concentration of the candidates at the young star cluster NGC 796, strongly suggesting the existence of pre-main-sequence (PMS) stars in the Magellanic Bridge. This is the first detection of PMS star candidates in the Magellanic Bridge, and if they are genuine PMS stars, this could be direct evidence of recent star formation. However, the estimate of the number of Herbig Ae/Be stars depends on the fraction of classical Be stars, and thus a more precise determination of the Be star fraction or observations to differentiate between the Herbig Ae/Be stars and classical Be stars are required.

Shogo Nishiyama; Yasuaki Haba; Daisuke Kato; Daisuke Baba; Hirofumi Hatano; Motohide Tamura; Yasushi Nakajima; Akika Ishihara; Tetsuya Nagata; Koji Sugitani; Noriyuki Matsunaga; Hinako Fukushi; Nobuhiko Kusakabe; Shuji Sato

2007-02-20T23:59:59.000Z

332

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

333

STAR-FREE GEODESIC LANGUAGES FOR GROUPS SUSAN HERMILLER1  

E-Print Network (OSTI)

STAR-FREE GEODESIC LANGUAGES FOR GROUPS SUSAN HERMILLER1 , DEREK F. HOLT, AND SARAH REES Abstract cancellation con- ditions C (1/6) and C (1/4) - T (4) has the property that the set of all geodesics (over the same generating set) is a star-free regular language. Star-free regularity of the geodesic set is shown

Logan, David

334

Comparing infrared star formation rate indicators with optically derived quantities  

Science Journals Connector (OSTI)

......infrared star formation rate indicators with optically...USA 4 School of Physics, Astronomy, and...Spitzer 24-mum band pass and Halpha-measured star formation rate varies from galaxy...Spitzer 8.0-mum band pass, ultraviolet-excited...track star formation rate (SFR; e.g. Calzetti......

J. E. Young; C. Gronwall; J. J. Salzer; J. L. Rosenberg

2014-01-01T23:59:59.000Z

335

On column density thresholds and the star formation rate  

Science Journals Connector (OSTI)

......cloud affect the rate at which stars form...model of the thermal physics of the clouds. However...candidate particle passes a number of tests...shown to reduce the rate of star formation...lower the overall rate of star formation...can capture all the physics required to create......

Paul C. Clark; Simon C. O. Glover

2014-01-01T23:59:59.000Z

336

Hot neutron star in generalized thermo-statistics  

E-Print Network (OSTI)

Hot neutron star in generalized thermo-statistics K. Miyazaki E-mail: miyazakiro@rio.odn.ne.jp Abstract The hot neutron star (NS) is investigated for the ...rst time in the generalized thermo-statistics. The study of neutron star (NS) is an important subject in nuclear physics and astro- physics. The equation

337

Physics of neutron star surface layers and their thermal radiation  

E-Print Network (OSTI)

Physics of neutron star surface layers and their thermal radiation Alexander Y. Potekhin Ioffe review the physical properties of neutron star surface layers, important for the stellar thermal radiation, taking into consideration the effects of strong magnetic fields. Keywords: Neutron stars

338

Proto-neutron star in generalized thermo-statistics  

E-Print Network (OSTI)

Proto-neutron star in generalized thermo-statistics K. Miyazaki E-mail: miyazakiro@rio.odn.ne.jp Abstract The proto-neutron star (PNS) is investigated for the ...rst time in the generalized thermo. A proto-neutron star (PNS) [1,2] is born during 0.1-1s after the core bounce of successful supernova

339

ENERGY STAR Jeopardy History Facts Universities Products Other  

E-Print Network (OSTI)

ENERGY STAR Jeopardy History Facts Universities Products Other 10 10 10 10 10 20 20 20 20 20 30 30 30 30 30 40 40 40 40 40 50 50 50 50 50 #12;In what year did ENERGY STAR start? A)2002 B)2008 C)1992 D)1999 #12;Answer: C) 1992! In 1992 the US Environmental Protection Agency (EPA) introduced ENERGY STAR

Brownstone, Rob

340

The G305 star-forming complex: embedded massive star formation discovered by Herschel Hi-GAL  

Science Journals Connector (OSTI)

......investigate the environmental impact this may have on...formation of future generations of stars (Elmegreen...until the next generation of star formation...cloud mass, in solar masses, above...both low-mass solar neighbourhood clouds......

A. Faimali; M. A. Thompson; L. Hindson; J. S. Urquhart; M. Pestalozzi; S. Carey; S. Shenoy; M. Veneziani; S. Molinari; J. S. Clark

2012-10-11T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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.


341

Eligibility criteria for the 1-100 ENERGY STAR score | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Eligibility criteria for the 1-100 ENERGY STAR score Eligibility criteria for the 1-100 ENERGY STAR score 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 Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit Identify your property type Enter data into Portfolio Manager The data quality checker

342

Property types eligible to receive a 1-100 ENERGY STAR score | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

Identify your property type Identify your property type » Property types eligible to receive a 1-100 ENERGY STAR score 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 Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit Identify your property type Property types eligible to receive a 1-100 ENERGY STAR score

343

EPA ENERGY STAR Webinar: The Federal Guiding Principles Checklist in ENERGY STAR Portfolio  

Energy.gov (U.S. Department of Energy (DOE))

Hosted by the EPA, this webinar will focus on how to use the ENERGY STAR measurement and tracking tool, Portfolio Manager, to help ensure compliance with the Guiding Principles for High Performance Sustainable Buildings.

344

"The Stars Tonight" LIVE Planetarium Show  

E-Print Network (OSTI)

wasn't turning around us, rather the Earth is turning on its axis. S B5: Conservation of Energy and city lights. Many NASM visitors have never had the chance to see a dark sky, with the stars on display of technology to enhance gathering and manipulation of data, the accuracy/precision of data gathering

Mathis, Wayne N.

345

EPA Natural Gas STAR Program Accomplishments  

E-Print Network (OSTI)

Established in 1993, the Natural Gas STAR program is a partnership between the U.S. EPA and the oil and natural gas industry designed to cost-effectively reduce methane emissions from voluntary activities undertaken at oil and natural gas operations both

unknown authors

346

Neutron star interiors and topology change  

E-Print Network (OSTI)

Quark matter is believed to exist in the center of neutron stars. A combined model consisting of quark matter and ordinary matter is used to show that the extreme conditions existing in the center could result in a topology change, that is, in the formation of wormholes.

Peter K. F. Kuhfittig

2012-07-27T23:59:59.000Z

347

Galactic structure studies with BATC star counts  

E-Print Network (OSTI)

We report the first results of star counts carried out with the National Astronomical Observatories (NAOC) 60/90 cm Schmidt Telescope in 15 intermediate-band filters from 3000 to 10000 {\\AA} in the BATC survey. We analyze a sample of over 1400 main sequence stars ($14\\le$V$\\le21$), which lie in the field with central coordinates R.A.=$09^h53^m13^s.30$ and DEC=47$^\\circ49^{\\prime}00^{\\prime\\prime}.0$ (J2000). The field of view is 0.95 deg$^{2}$, and the spatial scale was $1\\arcsec.67$. In our model, the distribution of stars perpendicular to the plane of the Galaxy is given by two exponential disks (thin disk plus thick disk) and a de Vaucouleurs halo. Based on star counts, we derive the scale heights of the thin disk to be $320^{+14}_{-15}$ pc and of the thick disk to be $640^{+30}_{-32}$ pc, respectively, with a local density of $7.0\\pm1%$ of the thin disk. We find that the observed counts support an axial ratio of $c/a\\le0.6$ for a de Vaucouleurs $r^{1/4}$ law, implying a more flattened halo. We also derive...

Du, C; Ma, J; Chen, A B C; Yang, Y; Li, J; Wu, H; Jiang, Z; Chen, J; Du, Cuihua; Zhou, Xu; Ma, Jun; Chen, Alfred B-C; Yang, Yanbin; Li, Jiuli; Wu, Hong; Jiang, Zhaoji; Chen, Jiansheng

2003-01-01T23:59:59.000Z

348

ANALYTICAL STAR FORMATION RATE FROM GRAVOTURBULENT FRAGMENTATION  

SciTech Connect

We present an analytical determination of the star formation rate (SFR) in molecular clouds, based on a time-dependent extension of our analytical theory of the stellar initial mass function. The theory yields SFRs in good agreement with observations, suggesting that turbulence is the dominant, initial process responsible for star formation. In contrast to previous SFR theories, the present one does not invoke an ad hoc density threshold for star formation; instead, the SFR continuously increases with gas density, naturally yielding two different characteristic regimes, thus two different slopes in the SFR versus gas density relationship, in agreement with observational determinations. Besides the complete SFR derivation, we also provide a simplified expression, which reproduces the complete calculations reasonably well and can easily be used for quick determinations of SFRs in cloud environments. A key property at the heart of both our complete and simplified theory is that the SFR involves a density-dependent dynamical time, characteristic of each collapsing (prestellar) overdense region in the cloud, instead of one single mean or critical freefall timescale. Unfortunately, the SFR also depends on some ill-determined parameters, such as the core-to-star mass conversion efficiency and the crossing timescale. Although we provide estimates for these parameters, their uncertainty hampers a precise quantitative determination of the SFR, within less than a factor of a few.

Hennebelle, Patrick [Laboratoire de Radioastronomie, UMR CNRS 8112, Ecole Normale Superieure et Observatoire de Paris, 24 rue Lhomond, 75231 Paris Cedex 05 (France); Chabrier, Gilles [Ecole Normale Superieure de Lyon, CRAL, UMR CNRS 5574, 69364 Lyon Cedex 07 (France)

2011-12-20T23:59:59.000Z

349

Model study of a quark star  

SciTech Connect

In this paper we apply the equation of state (EOS) of QCD at finite chemical potential and zero temperature proposed in H. S. Zong and W. M. Sun [Int. J. Mod. Phys. A 23, 3591 (2008)] to the study of properties of quark star. This EOS contains only one adjustable parameter m{sub D} which sets the scale of chiral symmetry breaking (in our calculation we have chosen two values of m{sub D}: m{sub D}=244 MeV and m{sub D}=239 MeV, which is fitted from the value of f{sub {pi}} and determined by e{sup +}e{sup -} annihilation experiment, respectively). From this EOS a model of quark star is established by applying the Tolman-Oppenheimer-Volkoff equation under two conditions: with the P({mu}=0) term and without the P({mu}=0) term. Our results show clearly that the P({mu}=0) term is an important quantity in the study of quark star. A comparison between our model and other models of quark star is made. In particular, we have compared our results with the most recent observational data measured using Shapiro delay reported in P. B. Demorest et al.[Nature (London) 467, 1081 (2010)].

Li Hua; Jiang Yu [Department of Physics, Nanjing University, Nanjing 210093 (China); Luo Xinlian [Department of Astronomy, Nanjing University, Nanjing 210093 (China); Zong Hongshi [Department of Physics, Nanjing University, Nanjing 210093 (China); Joint Center for Particle, Nuclear Physics and Cosmology, Nanjing 210093 (China)

2011-01-15T23:59:59.000Z

350

Proper Motions of 25,000 Stars  

Science Journals Connector (OSTI)

... motion, the apex of the solar motion, and the vertex and axes of the Schwarzschild ellipsoid, have been found for stars 9-0-14-0 m. and those fainter ... and those fainter than 14-1 m. It is pointed out that the vertex of Schwarzschild's ellipsoid is the only one of these quantities which can be satisfactorily derived from ...

F. W. D.

1935-03-09T23:59:59.000Z

351

Constraints in the coupling Star-Life  

E-Print Network (OSTI)

If life is sustained by a process of photosynthesis, not necessarily the same existing on Earth, the surface temperature of the star and the orbit of the host planet cannot be whatsoever. In fact the global life cycle, no matter how complicated, must contain in general an upper photochemical branch and a lower dark branch, characterized by a higher and a lower temperature. These two temperatures are star-orbit related. The velocity along the cycle or, in other words, the power of the life machine, depends in general on several other parameters. First of all the Gibbs photon availability, which is a star-orbit parameter and is the input for the upper branch. Then follows the energy cascade that develops along the organic web with a large number of interactions and typical times that must match the typical times generated by the combination of spin value and orientation, eccentricity and precession. Finally, the capacity of the web to keep the global life cycle running along the life span of the star, comes from some inner form of self-endurance and self-balance. The property of not being transient could be the right way of introducing the concept of intelligent life.

L. Sertorio; G. Tinetti

2001-10-01T23:59:59.000Z

352

Hypersonic Molecular Shocks in Star Forming Regions  

E-Print Network (OSTI)

Much emission from star forming regions is from shock-excited gas. Shocks in molecular clouds are still not fully understood, as magnetic fields, dust and chemistry all play significant roles. I review the history, physics and current work in understanding these shocks, and in their possible use as diagnostics of local conditions.

Brand, P W J L

2006-01-01T23:59:59.000Z

353

Hypersonic Molecular Shocks in Star Forming Regions  

E-Print Network (OSTI)

Much emission from star forming regions is from shock-excited gas. Shocks in molecular clouds are still not fully understood, as magnetic fields, dust and chemistry all play significant roles. I review the history, physics and current work in understanding these shocks, and in their possible use as diagnostics of local conditions.

Peter W. J. L. Brand

2006-09-08T23:59:59.000Z

354

Coronal structure of low-mass stars  

Science Journals Connector (OSTI)

......structure of low-mass stars Pauline Lang...loss in the stellar wind and X-ray emission...use reconstructed maps of the radial magnetic...strong as the stellar mass decreases, while...magnitude of the open (wind-bearing) magnetic...either rotational velocity or Rossby number......

Pauline Lang; Moira Jardine; Jean-Franois Donati; Julien Morin; Aline Vidotto

2012-08-01T23:59:59.000Z

355

Anisotropic thermal emission from magnetized neutron stars  

E-Print Network (OSTI)

The thermal emission from isolated neutron stars is not well understood. The X-ray spectrum is very close to a blackbody but there is a systematic optical excess flux with respect to the extrapolation to low energy of the best blackbody fit. This fact, in combination with the observed pulsations in the X-ray flux, can be explained by anisotropies in the surface temperature distribution.We study the thermal emission from neutron stars with strong magnetic fields in order to explain the origin of the anisotropy. We find (numerically) stationary solutions in axial symmetry of the heat transportequations in the neutron star crust and the condensed envelope. The anisotropy in the conductivity tensor is included consistently. The presence of magnetic fields of the expected strength leads to anisotropy in the surface temperature. Models with toroidal components similar to or larger than the poloidal field reproduce qualitatively the observed spectral properties and variability of isolated neutron stars. Our models also predict spectral features at energies between 0.2 and 0.6 keV.

J. F. Perez-Azorin; J. A. Miralles; J. A. Pons

2005-10-24T23:59:59.000Z

356

Singularity-free dark energy star  

E-Print Network (OSTI)

We propose a model for an anisotropic dark energy star where we assume that the radial pressure exerted on the system due to the presence of dark energy is proportional to the isotropic perfect fluid matter density. We discuss various physical features of our model and show that the model satisfies all the regularity conditions and stable as well as singularity-free.

Farook Rahaman; Anil Kumar Yadav; Saibal Ray; Raju Maulick; Ranjan Sharma

2011-08-25T23:59:59.000Z

357

Quantum vacuum instability near rotating stars  

SciTech Connect

We discuss the Starobinskii-Unruh process for the Kerr black hole. We show how this effect is related to the theory of squeezed states. We then consider a simple model for a highly relativistic rotating star and show that the Starobinskii-Unruh effect is absent.

Matacz, A.L. (Physics Department, University of Adelaide, P.O. Box 498, Adelaide, 5001 (Australia)); Davies, P.C.W. (Physics Department, University of Adelaide, P.O. Box 498, Adelaide, 5001 (Australia)); Ottewill, A.C. (Mathematical Institute, 24-29 St. Giles, Oxford OX13LB (United Kingdom))

1993-02-15T23:59:59.000Z

358

Molecular Gas and Star Formation in Voids  

E-Print Network (OSTI)

We present the detection of molecular gas using CO(1-0) line emission and follow up Halpha imaging observations of galaxies located in nearby voids. The CO(1-0) observations were done using the 45m telescope of the Nobeyama Radio Observatory (NRO) and the optical observations were done using the Himalayan Chandra Telescope (HCT). Although void galaxies lie in the most under dense parts of our universe, a significant fraction of them are gas rich, spiral galaxies that show signatures of ongoing star formation. Not much is known about their cold gas content or star formation properties. In this study we searched for molecular gas in five void galaxies using the NRO. The galaxies were selected based on their relatively higher IRAS fluxes or Halpha line luminosities. CO(1--0) emission was detected in four galaxies and the derived molecular gas masses lie between (1 - 8)E+9 Msun. The H$\\alpha$ imaging observations of three galaxies detected in CO emission indicates ongoing star formation and the derived star forma...

Das, M; Iono, D; Honey, M; Ramya, S

2014-01-01T23:59:59.000Z

359

Predictions from star formation in the multiverse  

SciTech Connect

We compute trivariate probability distributions in the landscape, scanning simultaneously over the cosmological constant, the primordial density contrast, and spatial curvature. We consider two different measures for regulating the divergences of eternal inflation, and three different models for observers. In one model, observers are assumed to arise in proportion to the entropy produced by stars; in the others, they arise at a fixed time (5 or 10x10{sup 9} years) after star formation. The star formation rate, which underlies all our observer models, depends sensitively on the three scanning parameters. We employ a recently developed model of star formation in the multiverse, a considerable refinement over previous treatments of the astrophysical and cosmological properties of different pocket universes. For each combination of observer model and measure, we display all single and bivariate probability distributions, both with the remaining parameter(s) held fixed and marginalized. Our results depend only weakly on the observer model but more strongly on the measure. Using the causal diamond measure, the observed parameter values (or bounds) lie within the central 2{sigma} of nearly all probability distributions we compute, and always within 3{sigma}. This success is encouraging and rather nontrivial, considering the large size and dimension of the parameter space. The causal patch measure gives similar results as long as curvature is negligible. If curvature dominates, the causal patch leads to a novel runaway: it prefers a negative value of the cosmological constant, with the smallest magnitude available in the landscape.

Bousso, Raphael; Leichenauer, Stefan [Center for Theoretical Physics, Department of Physics, University of California, Berkeley, California 94720-7300 (United States) and Lawrence Berkeley National Laboratory, Berkeley, California 94720-8162 (United States)

2010-03-15T23:59:59.000Z

360

A CATALOG OF GALACTIC INFRARED CARBON STARS  

SciTech Connect

We collected almost all of the Galactic infrared carbon stars (IRCSs) from literature published up to the present to organize a catalog of 974 Galactic IRCSs in this paper. Some of their photometric properties in the near-, mid-, and far-infrared are discussed.

Chen, P. S. [National Astronomical Observatories/Yunnan Observatory and Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011 (China); Yang, X. H., E-mail: iraspsc@yahoo.com.cn, E-mail: yangxh@cqu.edu.cn [Department of Physics, Chongqing University, Chongqing 400044 (China)

2012-02-15T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" from the National Library of EnergyBeta (NLEBeta).
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361

Boson stars from a gauge condensate  

E-Print Network (OSTI)

The boson star filled with two interacting scalar fields is investigated. The scalar fields can be considered as a gauge condensate formed by SU(3) gauge field quantized in a non-perturbative manner. The corresponding solution is regular everywhere, has a finite energy and can be considered as a quantum SU(3) version of the Bartnik - McKinnon particle-like solution.

V. Dzhunushaliev; K. Myrzakulov; R. Myrzakulov

2006-12-28T23:59:59.000Z

362

DayStar Technologies | Open Energy Information  

Open Energy Info (EERE)

DayStar Technologies DayStar Technologies Jump to: navigation, search Logo: DayStar Technologies Name DayStar Technologies Address 2972 Stender Way Place Santa Clara, California Zip 95054 Sector Solar Product Manufacturer of low-cost, high performance, CIGS thin film photovoltaic products Year founded 1997 Number of employees 51-200 Phone number 408-582-7100 Website http://www.daystartech.com/ Coordinates 37.375996°, -121.970815° 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":37.375996,"lon":-121.970815,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

363

Silver Star Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Silver Star Wind Farm Silver Star Wind Farm Jump to: navigation, search Name Silver Star Wind Farm Facility Silver Star Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner BP Alternative Energy/Clipper Developer BP Alternative Energy/Clipper Energy Purchaser Market Location Eastland and Erath Counties TX Coordinates 32.332058°, -98.466783° 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":32.332058,"lon":-98.466783,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

364

Star wars: US pressure on Japan  

Science Journals Connector (OSTI)

... US Strategic Defense Initiative ("star wars") seems to have found a fan in Japan's Prime Minister Yasuhiro Nakasone, who has been extolling its virtues in recent Diet ... after his meeting with President Ronald Reagan in Los Angeles earlier this year. Pressure for Japan to make its support official is being kept up by a series of visits from ...

David Swinbanks

1985-04-25T23:59:59.000Z

365

Gamma Ray Bursts from delayed collapse of neutron stars to quark matter stars  

E-Print Network (OSTI)

We propose a model to explain how a Gamma Rays Burst can take place days or years after a supernova explosion. Our model is based on the conversion of a pure hadronic star (neutron star) into a star made at least in part of deconfined quark matter. The conversion process can be delayed if the surface tension at the interface between hadronic and deconfined-quark-matter phases is taken into account. The nucleation time (i.e. the time to form a critical-size drop of quark matter) can be extremely long if the mass of the star is small. Via mass accretion the nucleation time can be dramaticaly reduced and the star is finally converted into the stable configuration. A huge amount of energy, of the order of 10$^{52}$--10$^{53}$ erg, is released during the conversion process and can produce a powerful Gamma Ray Burst. The delay between the supernova explosion generating the metastable neutron star and the new collapse can explain the delay proposed in GRB990705 and in GRB011211.

Z. Berezhiani; I. Bombaci; A. Drago; F. Frontera; A. Lavagno

2002-09-13T23:59:59.000Z

366

Climate change and buildings | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Climate change and buildings Climate change and buildings 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 How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Facts and stats Climate change and buildings Climate change and buildings

367

The Evolution of Dusty Debris Disks around Solar Type Stars  

Science Journals Connector (OSTI)

We used chromospheric activity to determine the ages of 2820 field stars. We searched these stars for excess emission at 22 ?m with the Wide-Field Infrared Survey Explorer. Such excess emission is indicative of a dusty debris disk around a star. We investigated how disk incidence trends with various stellar parameters, and how these parameters evolve with time. We found 22 ?m excesses around 98 stars (a detection rate of 3.5%). Of these 98 excess sources, 74 are presented here for the first time. We also measured the abundance of lithium in eight dusty stars in order to test our stellar age estimates.

Laura Vican; Adam Schneider

2014-01-01T23:59:59.000Z

368

ENERGY STAR Test Procedures and Verification | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

ENERGY STAR » ENERGY STAR Test ENERGY STAR » ENERGY STAR Test Procedures and Verification ENERGY STAR Test Procedures and Verification The Department of Energy (DOE) is the lead agency in the development and revision of all test procedures for products in the ENERGY STAR® program, including those products that are also subject to DOE's Energy Conservation Standards program. As specifications are updated and new products or metrics are added to the ENERGY STAR program, DOE is responsible for developing and revising methods, responding to stakeholder comments, and answering any testing-related questions that arise as a result of the procedures being utilized. To simplify the process for interested parties, more information on the test procedure development for ENERGY STAR products can be found on each of

369

Laser Guide Star Adaptive Optics without Tip-tilt  

E-Print Network (OSTI)

Adaptive optics (AO) systems allow a telescope to reach its diffraction limit at near infrared wavelengths. But to achieve this, a bright natural guide star (NGS) is needed for the wavefront sensing, severely limiting the fraction of the sky over which AO can be used. To some extent this can be overcome with a laser guide star (LGS). While the laser can be pointed anywhere in the sky, one still needs to have a natural star, albeit fainter, reasonably close to correct the image motion (tip-tilt) to which laser guide stars are insensitive. There are in fact many astronomical targets without suitable tip-tilt stars, but for which the enhanced resolution obtained with the Laser Guide Star Facility (LGSF) would still be very beneficial. This article explores what adaptive optics performance one might expect if one dispenses with the tip-tilt star, and in what situations this mode of observing might be needed.

R. Davies; S. Rabien; C. Lidman; M. Le Louarn; M. Kasper; N. M. Forster Schreiber; V. Roccatagliata; N. Ageorges; P. Amico; C. Dumas; F. Mannucci

2008-01-24T23:59:59.000Z

370

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

371

The abundance pattern of the lambda Bootis stars  

E-Print Network (OSTI)

Within a project to investigate the properties of lambda Bootis stars, we report on their abundance pattern. High resolution spectra have been obtained for a total of twelve candidate lambda Bootis stars, four of them being contained in spectroscopic binary systems, and detailed abundance analyses have been performed. All program stars show a characteristic lambda Bootis abundance pattern (deficient heavy elements and solar abundant light elements) and an enhanced abundance of Na. This work raises the fraction of lambda Bootis stars with known abundances to 50%. The resulting abundances complemented by literature data are used to construct a "mean lambda Bootis abundance pattern", which exhibits, apart from general underabundances of heavy elements (about -1 dex) and solar abundances of C, N, O, Na and S, a star-to-star scatter which is up to twice as large as for a comparable sample of normal stars.

U. Heiter

2001-12-07T23:59:59.000Z

372

Magnetic topologies of the Herbig Ae/Be stars  

E-Print Network (OSTI)

Our recent discoveries of magnetic fields in a small number of Herbig Ae/Be (HAeBe) stars, the evolutionary progenitors of main sequence A/B stars, raise new questions about the origin of magnetic fields in the intermediate mass stars. The favoured fossil field hypothesis suggests that a few percent of magnetic pre-main sequence A/B stars should exhibit similar magnetic strengths and topologies to the magnetic Ap/Bp stars. In this talk I will present the methods that we have used to characterise the magnetic fields of the Herbig Ae/Be stars, as well as our first conclusions on the origin of magnetism in intermediate-mass stars.

Alecian, E; Catala, C; Bagnulo, S; Bhm, T; Bouret, J -C; Donati, J -F; Folsom, C; Grunhut, J; Landstreet, J D; Petit, P; Silvester, J

2008-01-01T23:59:59.000Z

373

Two ENERGY STAR Products Fail Testing | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Two ENERGY STAR Products Fail Testing Two ENERGY STAR Products Fail Testing Two ENERGY STAR Products Fail Testing August 9, 2011 - 4:42pm Addthis DOE testing has identified two additional models of home appliances that do not meet the ENERGY STAR Program's energy efficiency requirements. A refrigerator manufactured by the Perlick Corporation and a room air conditioner manufactured by Electrolux Home Products, Inc. were selected for testing as part of the DOE's ENERGY STAR Verification Testing Pilot Program. DOE testing revealed that Electrolux air conditioner (model FRA256ST2) and Perlick refrigerator (model HP48RO-S), both of which claimed ENERGY STAR ratings, do not meet the ENERGY STAR requirements. Multiple test results for the Electrolux model show that, when tested in accordance with DOE's

374

Relativistic tidal properties of neutron stars  

E-Print Network (OSTI)

We study the various linear responses of neutron stars to external relativistic tidal fields. We focus on three different tidal responses, associated to three different tidal coefficients: (i) a gravito-electric-type coefficient G\\mu_\\ell=[length]^{2\\ell+1} measuring the \\ell^{th}-order mass multipolar moment GM_{a_1... a_\\ell} induced in a star by an external \\ell^{th}-order gravito-electric tidal field G_{a_1... a_\\ell}; (ii) a gravito-magnetic-type coefficient G\\sigma_\\ell=[length]^{2\\ell+1} measuring the \\ell^{th} spin multipole moment G S_{a_1... a_\\ell} induced in a star by an external \\ell^{th}-order gravito-magnetic tidal field H_{a_1... a_\\ell}; and (iii) a dimensionless ``shape'' Love number h_\\ell measuring the distortion of the shape of the surface of a star by an external \\ell^{th}-order gravito-electric tidal field. All the dimensionless tidal coefficients G\\mu_\\ell/R^{2\\ell+1}, G\\sigma_\\l/R^{2\\ell+1} and h_\\ell (where R is the radius of the star) are found to have a strong sensitivity to the value of the star's ``compactness'' c\\equiv GM/(c_0^2 R) (where we indicate by c_0 the speed of light). In particular, G\\mu_\\l/R^{2\\l+1}\\sim k_\\ell is found to strongly decrease, as c increases, down to a zero value as c is formally extended to the ``black-hole (BH) limit'' c^{BH}=1/2. The shape Love number h_\\ell is also found to significantly decrease as c increases, though it does not vanish in the formal limit c\\to c^{BH}. The formal vanishing of \\mu_\\ell and \\sigma_\\ell as c\\to c^{BH} is a consequence of the no-hair properties of black holes; this suggests, but in no way proves, that the effective action describing the gravitational interactions of black holes may not need to be augmented by nonminimal worldline couplings.

Thibault Damour; Alessandro Nagar

2009-05-30T23:59:59.000Z

375

Green Star Energy LLC | Open Energy Information  

Open Energy Info (EERE)

Star Energy LLC Star Energy LLC Place Houston, Texas Zip 77002 Product Houston-based producer of sugar cane processed ethanol, with additional electricity generation activities from agricultural waste. Coordinates 29.76045°, -95.369784° 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":29.76045,"lon":-95.369784,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

376

Ms. Leslie Jones ENERGY STAR Program  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

July 7, 2011 July 7, 2011 U.S. Environmental Protection Agency 1200 Pennsylvania Avenue NW Room62023 Washington, DC 20460 Dear Ms. Jones: Electrolux Home Products, Inc. (Electro lux) room air conditioner model FRA256ST2 was selected for testing as part of the U.S. Department of Energy's (DOE) ENERGY STAR® Verification Testing Pilot Program. DOE's initial testing, performed on a unit of this model, indicated that it may not meet ENERGY STAR requirements. After testing three additional units of this model, and finding that each fell short of the minimum standard of9.4 EER, DOE asked Electrolux to provide conclusive manufacturing or design evidence or quality assurance information on why this product should be viewed as meeting the ENERGY STAR Program's energy efficiency

377

Star Energy Systems | Open Energy Information  

Open Energy Info (EERE)

Star Energy Systems Star Energy Systems Place Ahmedabad, Gujarat, India Zip 380 009 Sector Solar Product Solar PV product distributor. Coordinates 26.93077°, 80.66416° 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":26.93077,"lon":80.66416,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

378

Star Point Wind Farm | Open Energy Information  

Open Energy Info (EERE)

Point Wind Farm Point Wind Farm Jump to: navigation, search Name Star Point Wind Farm Facility Star Point Wind Farm Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Iberdrola Renewables Developer Iberdrola Renewables Energy Purchaser Modesto Irrigation District Location Near Moro OR Coordinates 45.474734°, -120.704412° 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":45.474734,"lon":-120.704412,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

379

Spectral Synthesis of Massive Stars in Clusters  

E-Print Network (OSTI)

Stellar clusters are thought to be the simplest stellar systems and the closest observational counterparts to theoretical models for single stellar populations. Progress in our understanding of the atmospheres and evolution of massive stars has led to generally reliable synthesis models. The future release of new evolution models with rotation, however, will require non-trivial updates to previously published synthesis models, in particular for all Wolf-Rayet and red supergiant related quantities. Cluster synthesis work is currently progressing from a purely stellar approach to a more comprehensive stellar+cluster perspective. The photometric evolution of stars and the dynamical evolution of clusters are delicately interwoven. Recent work attempts to combine these seemingly related fields.

Claus Leitherer

2006-08-31T23:59:59.000Z

380

Thermal radiation from magnetic neutron star surfaces  

E-Print Network (OSTI)

We investigate the thermal emission from magnetic neutron star surfaces in which the cohesive effects of the magnetic field have produced the condensation of the atmosphere and the external layers. This may happen for sufficiently cool atmospheres with moderately intense magnetic fields. The thermal emission from an isothermal bare surface of a neutron star shows no remarkable spectral features, but it is significantly depressed at energies below some threshold energy. However, since the thermal conductivity is very different in the normal and parallel directions to the magnetic field lines, the presence of the magnetic field is expected to produce a highly anisotropic temperature distribution, depending on the magnetic field geometry. In this case, the observed flux of such an object looks very similar to a BB spectrum, but depressed in a nearly constant factor at all energies. This results in a systematic underestimation of the area of the emitter (and therefore its size) by a factor 5-10 (2-3).

J. F. Perez--Azorin; J. A. Miralles; J. A. Pons

2004-10-27T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Supergiant Pulses from Extragalactic Neutron Stars  

E-Print Network (OSTI)

We evaluate the hypothesis that extragalactic radio bursts originate from neutron stars. These could be active pulsars or dormant, slowly spinning objects, but the different population distances for these two classes require correspondingly different contributions to burst dispersion measures from any host or intervening galaxies combined with the intergalactic medium. The large, apparent burst rate $\\sim 10^4~$ sky$^{-1}~$ day$^{-1}$ is comparable to the core-collapse supernova rate in a Hubble volume and can be accommodated by a single burst per object in the resulting large reservoir of $\\sim 10^{17}~$ neutron stars. A smaller population distance requires more bursts per object but the likelihood of seeing repeated bursts from any single object is extremely low on human timescales. Gravitational microlensing could play a role for high redshift sources. Extrapolation of the Crab pulsar's giant pulses --- exemplars of coherent, high brightness temperature radiation --- to a rate of one per $10^3~$yr yields a...

Cordes, J M

2015-01-01T23:59:59.000Z

382

Reconstructing the Star Formation Histories of Galaxies  

E-Print Network (OSTI)

We present a methodological study to find out how far back and to what precision star formation histories of galaxies can be reconstructed from CMDs, from integrated spectra and Lick indices, and from integrated multi-band photometry. Our evolutionary synthesis models GALEV allow to describe the evolution of galaxies in terms of all three approaches and we have assumed typical observational uncertainties for each of them and then investigated to what extent and accuracy different star formation histories can be discriminated. For a field in the LMC bar region with both a deep CMD from HST observations and a trailing slit spectrum across exactly the same field of view we could test our modelling results against real data.

Uta Fritze; Thomas Lilly

2007-01-15T23:59:59.000Z

383

Star, Idaho: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

Star, Idaho: Energy Resources Star, Idaho: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 43.6921071°, -116.4934631° 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":43.6921071,"lon":-116.4934631,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

384

Analysis and demonstration: a proof-of-concept compass star tracker  

E-Print Network (OSTI)

vectors in the camera?s reference frame. The second step of the star identification process is the comparison of the cen- troiding output to a catalog of reference star vectors. Although there are many different techniques to compare the digitally imaged... stars to the catalog stars, all of the techniques should output the desired result ? a set of reference star vectors that correspond to the star vectors generated by the centroiding code. Once the star identification process is complete, the attitude...

Swanzy, Michael John

2007-04-25T23:59:59.000Z

385

Model Atmospheres for Low Field Neutron Stars  

E-Print Network (OSTI)

We compute model atmospheres and emergent spectra for low field (Bsolar abundance and iron atmospheres. We compare our results to high field magnetic atmospheres, available only for hydrogen. An application to apparently thermal flux from the low field millisecond pulsar PSR J0437--4715 shows that H atmospheres fit substantially better than Fe models. We comment on extension to high fields and the implication of these results for neutron star luminosities and radii.

Mohan Rajagopal; Roger Romani

1995-10-19T23:59:59.000Z

386

The Dark Energy Star and Stability analysis  

E-Print Network (OSTI)

We have proposed a new model of dark energy star consisting of five zones namely, solid core of constant energy density, the thin shell between core and interior, an inhomogeneous interior region with anisotropic pressures, thin shell and the exterior vacuum region. We have discussed various physical properties. The model satisfies all the physical requirements. The stability condition under small linear perturbation has also been discussed.

Piyali Bhar; Farook Rahaman

2015-01-12T23:59:59.000Z

387

Neutron Star Superfluidity, Dynamics and Precession  

E-Print Network (OSTI)

Basic rotational and magnetic properties of neutron superfluids and proton superconductors in neutron stars are reviewed. The modes of precession of the neutron superfluid are discussed in detail. We emphasize that at finite temperature, pinning of superfluid vortices does not offer any constraint on the precession. Any pinning energies can be surmounted by thermal activation and there exists a dynamical steady state in which the superfluid follows the precession of the crust at a small lag angle between the crust and superfluid rotation velocity vectors. At this small lag the system is far from the critical conditions for unpinning, even if the observed precession of the crust may entail a large angle between the figure axis and the crust's rotation velocity vector. We conclude that if long period modulations of pulse arrival times and pulse shapes observed in a pulsar like the PSR B1828-11 are due to the precession of the neutron star, this does not have any binding implications about the existence of pinning by flux lines or the existence of Type II superconductivity in the neutron star.

M. Ali Alpar

2005-05-04T23:59:59.000Z

388

Gravitational waves from rapidly rotating neutron stars  

E-Print Network (OSTI)

Rapidly rotating neutron stars in Low Mass X-ray Binaries have been proposed as an interesting source of gravitational waves. In this chapter we present estimates of the gravitational wave emission for various scenarios, given the (electromagnetically) observed characteristics of these systems. First of all we focus on the r-mode instability and show that a 'minimal' neutron star model (which does not incorporate exotica in the core, dynamically important magnetic fields or superfluid degrees of freedom), is not consistent with observations. We then present estimates of both thermally induced and magnetically sustained mountains in the crust. In general magnetic mountains are likely to be detectable only if the buried magnetic field of the star is of the order of $B\\approx 10^{12}$ G. In the thermal mountain case we find that gravitational wave emission from persistent systems may be detected by ground based interferometers. Finally we re-asses the idea that gravitational wave emission may be balancing the accretion torque in these systems, and show that in most cases the disc/magnetosphere interaction can account for the observed spin periods.

Brynmor Haskell; Nils Andersson; Caroline D`Angelo; Nathalie Degenaar; Kostas Glampedakis; Wynn C. G. Ho; Paul D. Lasky; Andrew Melatos; Manuel Oppenoorth; Alessandro Patruno; Maxim Priymak

2014-07-31T23:59:59.000Z

389

Star Formation Histories in the Local Group  

E-Print Network (OSTI)

Deep color magnitude diagrams extending to the main sequence provide the most direct measure of the detailed star formation history in a stellar population. With large investments of observing time, HST can obtain such data for populations out to 1 Mpc, but its field of view is extremely small in comparison to the size of Local Group galaxies. This limitation severely constrains our understanding of galaxy formation. For example, the largest galaxy in the Local Group, Andromeda, offers an ideal laboratory for studying the formation of large spiral galaxies, but the galaxy shows substructure on a variety of scales, presumably due to its violent merger history. Within its remaining lifetime, HST can only sample a few sight-lines through this complex galaxy. In contrast, a wide field imager could provide a map of Andromeda's halo, outer disk, and tidal streams, revealing the spatially-dependent star formation history in each structure. The same data would enable many secondary studies, such as the age variation in Andromeda's globular cluster system, gigantic samples of variable stars, and microlensing tracers of the galaxy's dark matter distribution.

Thomas M. Brown

2004-07-09T23:59:59.000Z

390

Statistical theory of thermal evolution of neutron stars  

E-Print Network (OSTI)

Thermal evolution of neutron stars is known to depend on the properties of superdense matter in neutron star cores. We suggest a statistical analysis of isolated cooling middle-aged neutron stars and old transiently accreting quasi-stationary neutron stars warmed up by deep crustal heating in low-mass X-ray binaries. The method is based on simulations of the evolution of stars of different masses and on averaging the results over respective mass distributions. This gives theoretical distributions of isolated neutron stars in the surface temperature--age plane and of accreting stars in the photon thermal luminosity--mean mass accretion rate plane to be compared with observations. This approach permits to explore not only superdense matter but also the mass distributions of isolated and accreting neutron stars. We show that the observations of these stars can be reasonably well explained by assuming the presence of the powerful direct Urca process of neutrino emission in the inner cores of massive stars, introd...

Beznogov, M V

2014-01-01T23:59:59.000Z

391

Find an ENERGY STAR service and product provider | ENERGY STAR Buildings &  

NLE Websites -- All DOE Office Websites (Extended Search)

Find an ENERGY STAR service and product provider Find an ENERGY STAR service and product provider 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 Learn the benefits Get started Use Portfolio Manager Save energy Stamp out energy waste Find cost-effective investments Engage occupants Purchase energy-saving products Put computers to sleep Get help from an expert SPP success stories

392

Step 3: Evaluate your target using ENERGY STAR tools | ENERGY STAR  

NLE Websites -- All DOE Office Websites (Extended Search)

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 Comparing Target Finder and Portfolio Manager EPA's Target Finder calculator Step 4: Design to be energy efficient

393

PNM - Energy Star Home Builder Rebate Program | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

PNM - Energy Star Home Builder Rebate Program PNM - Energy Star Home Builder Rebate Program PNM - Energy Star Home Builder Rebate Program < Back Eligibility Construction Residential Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Program Info Expiration Date 12/31/2012 State New Mexico Program Type Utility Rebate Program Rebate Amount Energy Star for Homes Version 2.5: $750/home Provider PNM PNM is offering home builders a rebate for each Energy Star-qualified home they build in PNM service areas. Every Energy Star-qualified home must include effective insulation and air sealing, high performance windows, doors and skylights, tight construction and ducts, and independent testing and inspection. The builder must arrange for a qualified Home Energy Rater

394

General Electric: ENERGY STAR Referral (PFSF5NFZ****) | Department of  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

General Electric: ENERGY STAR Referral (PFSF5NFZ****) General Electric: ENERGY STAR Referral (PFSF5NFZ****) General Electric: ENERGY STAR Referral (PFSF5NFZ****) August 29, 2012 DOE referred the matter of General Electric ("GE") refrigerator-freezer model PFSF5NFZ**** to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. After referring this matter, DOE determined that GE was also correct that the test report calculations were incorrect given that the tested model had a variable anti-sweat heater. DOE revised its test reports accordingly; however the corrections did not impact the final determination. General Electric: ENERGY STAR Referral (PFSF5NFZ****) More Documents & Publications

395

Webinar: ENERGY STAR Hot Water Systems for High Performance Homes  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Star Hot Water Systems for High Performance Homes Star Hot Water Systems for High Performance Homes 1 | Building America Program www.buildingamerica.gov Buildings Technologies Program Date: September 30, 2011 ENERGY STAR ® Hot Water Systems for High Performance Homes Welcome to the Webinar! We will start at 11:00 AM Eastern. There is no call in number. The audio will be sent through your computer speakers. All questions will be submitted via typing. Video of presenters Energy Star Hot Water Systems for High Performance Homes 2 | Building America Program www.buildingamerica.gov Energy Star Hot Water Systems for High Performance Homes 3 | Building America Program www.buildingamerica.gov Building America Program: Introduction Building Technologies Program Energy Star Hot Water Systems for High Performance Homes

396

DOE Testing Reveals Samsung Refrigerator Does Not Meet Energy Star  

NLE Websites -- All DOE Office Websites (Extended Search)

Testing Reveals Samsung Refrigerator Does Not Meet Energy Star Testing Reveals Samsung Refrigerator Does Not Meet Energy Star Requirements DOE Testing Reveals Samsung Refrigerator Does Not Meet Energy Star Requirements March 16, 2010 - 4:28pm Addthis DOE-initiated testing has revealed that a Samsung refrigerator (model RF26VAB), which the company had claimed was Energy Star compliant, consumed more energy than permitted by the Energy Star program. Test results for the Samsung model at issue show that, when tested in accordance with DOE's test procedure, it consumed between 7 and 11.4 percent more energy than the Energy Star requirement. Samsung is no longer manufacturing this model, although it may still be available from some retail outlets. Based on this testing, DOE is referring Samsung Model RF26VAB to the U.S.

397

Entergy Texas - Energy Star Homes Program for Builders | Department of  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Entergy Texas - Energy Star Homes Program for Builders Entergy Texas - Energy Star Homes Program for Builders Entergy Texas - Energy Star Homes Program for Builders < Back Eligibility Construction Residential Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Program Info State Texas Program Type Utility Rebate Program Rebate Amount Single-Family Homes - Tier I (ENERGY STAR V-2.0): $150 per home Single-Family Homes - Tier II (ENERGY STAR V-2.5): $300 per home Attached Homes: 50% of single-family incentive per housing unit Advanced Lighting Package: $50 per single-family home ENERGY STAR V-3.0 HVAC Check Lists: $150 per single-family home Provider Entergy Texas Entergy Texas offers an incentive to builders in its service territory for

398

MHK Technologies/OceanStar | Open Energy Information  

Open Energy Info (EERE)

OceanStar OceanStar < MHK Technologies Jump to: navigation, search << Return to the MHK database homepage OceanStar.jpg Technology Profile Primary Organization Bourne Energy Technology Resource Click here Wave Technology Type Click here Overtopping Technology Readiness Level Click here TRL 4 Proof of Concept Technology Description The OceanStar device captures the underlying pressure wave through a series of small turbine generators The OceanStar relies upon a proprietary energy efficient process to smooth out the pulse characteristics common to wave energy in order to be electrical grid friendly The OceanStars high level of scalability is essential to reach the large surface areas required to reach utility scale ocean power generation Technology Dimensions

399

ENERGY STAR Labeled Buildings and Plants | Open Energy Information  

Open Energy Info (EERE)

STAR Labeled Buildings and Plants STAR Labeled Buildings and Plants Jump to: navigation, search Name ENERGY STAR Labeled Buildings and Plants Data Format Excel Spreadsheet Geographic Scope United States TODO: Import actual dataset contents into OpenEI The ENERGY STAR Labeled Buildings and Plants is "a list of facilities that measurably cost less to operate and improve the quality of our environment."[1] It is produced by the United States Environmental Protection Agency. External links Dataset in Excel Format References ↑ "ENERGY STAR Labeled Buildings and Plants" Retrieved from "http://en.openei.org/w/index.php?title=ENERGY_STAR_Labeled_Buildings_and_Plants&oldid=298127" Categories: Datasets Articles with outstanding TODO tasks What links here Related changes

400

Portfolio Manager DataTrends | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Portfolio Manager DataTrends Portfolio Manager DataTrends 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 How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Portfolio Manager DataTrends ENERGY STAR Snapshot Energy strategy for the future

Note: This page contains sample records for the topic "waha lone star" 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

General Electric: ENERGY STAR Referral (PFSF5NFZ****) | Department of  

NLE Websites -- All DOE Office Websites (Extended Search)

General Electric: ENERGY STAR Referral (PFSF5NFZ****) General Electric: ENERGY STAR Referral (PFSF5NFZ****) General Electric: ENERGY STAR Referral (PFSF5NFZ****) August 29, 2012 DOE referred the matter of General Electric ("GE") refrigerator-freezer model PFSF5NFZ**** to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. After referring this matter, DOE determined that GE was also correct that the test report calculations were incorrect given that the tested model had a variable anti-sweat heater. DOE revised its test reports accordingly; however the corrections did not impact the final determination. General Electric: ENERGY STAR Referral (PFSF5NFZ****) More Documents & Publications

402

Vectren Energy Delivery of Ohio (Gas) - Energy Star Home Rebate |  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Vectren Energy Delivery of Ohio (Gas) - Energy Star Home Rebate Vectren Energy Delivery of Ohio (Gas) - Energy Star Home Rebate Vectren Energy Delivery of Ohio (Gas) - Energy Star Home Rebate < Back Eligibility Construction Installer/Contractor Residential Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Program Info State Ohio Program Type Utility Rebate Program Rebate Amount Full Adoption of Energy Star (Version 2.5) Standards: $750 Vectren Gold Star - HERS rating of 70 or less: $750 Furnace: $300 Boiler: $500 Tankless Water Heater: $150 Storage Water Heater: $50-$150 Programmable Thermostat: $20 Provider Vectren Energy Delivery of Ohio Vectren Energy Delivery of Ohio offers a flat rebate to builders of residential single-family Energy Star certified homes that receive gas

403

Stellar wind signatures in sdB stars?  

E-Print Network (OSTI)

Subdwarf B (sdB) stars form the blue end of the horizonal branch. Their peculiar atmospheric abundance patterns are due to diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous H alpha and HeI 6678Ang line profiles, i.e, the lines are too broad and shallow and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass loss may also explain the peculiar abundance patterns seen in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds.

U. Heber; P. F. L. Maxted; T. R. Marsh; C. Knigge; J. E. Drew

2002-12-20T23:59:59.000Z

404

Herbig AeBe stars: Multiplicity and consequences  

E-Print Network (OSTI)

By virtue of their young age and intermediate mass, Herbig AeBe stars represent a cornerstone for our understanding of the mass-dependency of both the stellar and planetary formation processes. In this contribution, I review the current state-of-the-art multiplicity surveys of Herbig AeBe stars to assess both the overall frequency of companions and the distribution of key orbital parameters (separation, mass ratio and eccentricity). In a second part, I focus on the interplay between the multiplicity of Herbig AeBe stars and the presence and properties of their protoplanetary disks. Overall, it appears that both star and planet formation in the context of intermediate-mass stars proceeds following similar mechanisms as lower-mass stars.

Duchene, Gaspard

2014-01-01T23:59:59.000Z

405

Rotational and magnetic field instabilities in neutron stars  

SciTech Connect

In this short review we present recent results on the dynamics of neutron stars and their magnetic fields. We discuss the progress that has been made, during the last 5 years, in understanding the rotational instabilities with emphasis to the one due to the f-mode, the possibility of using gravitational wave detection in constraining the parameters of neutron stars and revealing the equation of state as well as the detectability of gravitational waves produced during the unstable phase of a neutron stars life. In addition we discuss the dynamics of extremely strong magnetic fields observed in a class of neutron stars (magnetars). Magnetic fields of that strength are responsible for highly energetic phenomena (giant flares) and we demonstrate that the analysis of the emitted electromagnetic radiation can lead in constraining the parameters of neutron stars. Furthermore, we present our results from the study of such violent phenomena in association with the emission of gravitational radiation.

Kokkotas, Kostas D. [Theoretical Astrophysics, IAAT, Eberhard Karls University of Tbingen, Tbingen 72076 (Germany)

2014-01-14T23:59:59.000Z

406

The Cosmic Near Infrared Background: Remnant Light from Early Stars  

E-Print Network (OSTI)

The redshifted ultraviolet light from early stars at z ~ 10 contributes to the cosmic near infrared background. We present detailed calculations of its spectrum with various assumptions about metallicity and mass spectrum of early stars. We show that if the near infrared background has a stellar origin, metal-free stars are not the only explanation of the excess near infrared background; stars with metals (e.g. Z=1/50 Z_sun) can produce the same amount of background intensity as the metal-free stars. We quantitatively show that the predicted average intensity at 1-2 microns is essentially determined by the efficiency of nuclear burning in stars, which is not very sensitive to metallicity. We predict \

Elizabeth Fernandez; Eiichiro Komatsu

2005-08-08T23:59:59.000Z

407

Ivermectin: a potent new antiparasitic agent  

Science Journals Connector (OSTI)

...ACARI, IXODIDAE) SYSTEMICALLY WITH MERCK MK-933, AN AVERMECTIN, JOURNAL OF ECONOMIC...L., SYSTEMATIC EFFICACY OF IVERMECTIN MK-933 AGAINST THE LONE STAR TICK (ACARI...batches lacked a number of characteristic, ultra-violet light-absorbing components...

WC Campbell; MH Fisher; EO Stapley; G Albers-Schonberg; TA Jacob

1983-08-26T23:59:59.000Z

408

Stability of thin-shell interfaces inside compact stars  

E-Print Network (OSTI)

We use the thin-shell Darmois-Israel formalism to model and assess the stability of the interfaces separating phases, e.g. the core and the crust, within compact stars. We exemplify the relevance and non-triviality of this treatment in the simplest case of an incompressible star, in constant pressure phase transitions, and in the case of strange quark stars with crust.

Jonas P. Pereira; Jaziel G. Coelho; Jorge A. Rueda

2015-01-05T23:59:59.000Z

409

THE SUN AS AN XRAY STAR: OVERVIEW OF THE METHOD  

E-Print Network (OSTI)

THE SUN AS AN X­RAY STAR: OVERVIEW OF THE METHOD G. PERES, S. ORLANDO AND F. REALE Istituto ed.e., the close similarity of the physical phenomena occurring on the Sun and on late­type active stars, by taking­ray instruments aimed at stars other than the Sun. Here we illustrate the application of this method to ROSAT

410

Industries in focus | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

ENERGY STAR Energy Performance Indicators for plants ENERGY STAR Energy Performance Indicators for plants » Industries in focus 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 Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Tools for benchmarking energy management practices Tools for tracking and benchmarking facility energy performance

411

Orbital periods of twenty two subdwarf B stars  

E-Print Network (OSTI)

Subdwarf B (sdB) stars are thought to be core helium burning stars with low mass hydrogen envelopes. In recent years it has become clear that many sdB stars lose their hydrogen through interaction with a binary companion and continue to reside in binary systems today. In this paper we present the results of a programme to measure orbital parameters of binary sdB stars. We determine the orbits of 22 binary sdB stars from 424 radial velocity measurements, raising the sample of sdBs with known orbital parameters to 38. We calculate lower limits for the masses of the companions of the sdB stars which, when combined with the orbital periods of the systems, allow us to discuss approximate evolutionary constraints. We find that a formation path for sdB stars consisting of mass transfer at the tip of the red giant branch followed by a common envelope phase explains most, but not all of the observed systems. It is particularly difficult to explain both long period systems and short period, massive systems. We present new measurements of the effective temperature, surface density and surface helium abundance for some of the sdB stars by fitting their blue spectra. We find that two of them (PG0839+399 and KPD1946+4340) do not lie in the Extreme Horizontal Branch (EHB) band indicating that they are post-EHB stars.

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

2002-09-23T23:59:59.000Z

412

Neutron stars is focus of Los Alamos National Laboratory Frontiers...  

NLE Websites -- All DOE Office Websites (Extended Search)

Frontiers in Science lectures Neutron stars is focus of Los Alamos National Laboratory Frontiers in Science lectures Lectures are intended to increase local public awareness of the...

413

Neutron superfluidity and unusual nuclear shapes in neutron stars crusts  

Science Journals Connector (OSTI)

We calculate in the frame-work of a semiclassical model the neutron superfluidity in the crust of neutron stars, accounting for the presence of unusual....

G. Lazzari; F. V. De Blasio

1994-01-01T23:59:59.000Z

414

Calendar Year 2009 Program Benefits for ENERGY STAR Labeled Products  

E-Print Network (OSTI)

Administration, Office of Energy Markets and End Use.Administration, Office of Energy Markets and End Use.ICF Consulting. 2003. Energy Star Market Penetration Report

Homan, Gregory K

2011-01-01T23:59:59.000Z

415

Calendar Year 2008 Program Benefits for ENERGY STAR Labeled Products  

E-Print Network (OSTI)

Administration, Office of Energy Markets and End Use.Administration, Office of Energy Markets and End Use.Protection Agency: ENERGY STAR Market Share of computers,

Homan, GregoryK

2010-01-01T23:59:59.000Z

416

Caby Photometry of the Hyades Comparisons to the Field Stars  

E-Print Network (OSTI)

Intermediate-band photometry of the Hyades cluster on the Caby system is presented for dwarf stars ranging from spectral type A through late K. A mean hk, b-y relation is constructed using only single stars without anomalous atmospheres and compared to the field stars of the solar neighborhood. For the F dwarfs, the Hyades relation defines an approximate LOWER bound in the two-color diagram, consistent with an [Fe/H] between +0.10 and +0.15. These index-color diagrams follow the common convention of presenting stars with highest abundance at the bottom of the plot although the index values for the metal-rich stars are numerically larger. For field F dwarfs in the range [Fe/H] between +0.4 and -1.0, [Fe/H] = -5.6 delta-hk + 0.125, with no evidence for a color dependence in the slope. For the G and K dwarfs, the Hyades mean relation crosses the field star distribution in the two-color diagram, defining an approximate UPPER bound for the local disk stars. Stars found above the Hyades stars fall in at least one o...

Anthony-Twarog, B J; Yu, J

2002-01-01T23:59:59.000Z

417

The Metallicity Distribution of Intracluster Stars in Virgo  

E-Print Network (OSTI)

We have used the Hubble Space Telescope's Advanced Camera for Surveys (ACS) to detect and measure ~5300 stars in a single intracluster field in the Virgo Cluster. By performing F606W and F814W photometry on these stars, we have determined their metallicity distribution function, and constrained the types of stars present in this portion of Virgo's intracluster space. Based on the small number of stars detected brighter than the red giant branch (RGB) tip, we suggest that in this region, Virgo's intracluster stars are mostly old (>~10 Gyr). Through analysis of the RGB stars themselves, we determine that the population contains the full range of metallicities probed (-2.3-0.5. The spatial distribution of the most metal-poor stars in the field shows significantly more structure than that of the metal-rich stars, indicating that the intracluster population is not well-mixed. We discuss the implications these observations have for the production of intracluster stars and the dynamical evolution of the Virgo Cluster.

Benjamin F. Williams; Robin Ciardullo; Patrick R. Durrell; Matt Vinciguerra; John J. Feldmeier; George H. Jacoby; Steinn Sigurdsson; Ted von Hippel; Henry C. Ferguson; Nial R. Tanvir; Magda Arnaboldi; Ortwin Gerhard; J. Alfonso L. Aguerri; Ken Freeman

2006-10-12T23:59:59.000Z

418

Neutron stars in f(R) gravity with perturbative constraints  

SciTech Connect

We study the structure of neutron stars in f(R) gravity theories with perturbative constraints. We derive the modified Tolman-Oppenheimer-Volkov equations and solve them for a polytropic equation of state. We investigate the resulting modifications to the masses and radii of neutron stars and show that observations of surface phenomena alone cannot break the degeneracy between altering the theory of gravity versus choosing a different equation of state of neutron-star matter. On the other hand, observations of neutron-star cooling, which depends on the density of matter at the stellar interior, can place significant constraints on the parameters of the theory.

Cooney, Alan; DeDeo, Simon; Psaltis, Dimitrios [Department of Physics, University of Arizona, Tucson, Arizona 85721 (United States); Santa Fe Institute, 1399 Hyde Park Road, Santa Fe, New Mexico 87501 (United States); Departments of Astronomy and Physics, University of Arizona, Tucson, Arizona 85721 (United States)

2010-09-15T23:59:59.000Z

419

PROPERTIES OF OSCILLATION MODES IN SUBGIANT STARS OBSERVED BY KEPLER  

SciTech Connect

Mixed modes seen in evolved stars carry information on their deeper layers that can place stringent constraints on their physics and on their global properties (mass, age, etc.). In this study, we present a method to identify and measure all oscillatory mode characteristics (frequency, height, width). Analyzing four subgiant stars, we present the first measure of the effect of the degree of mixture on the l = 1 mixed mode characteristics. We also show that some stars have measurable l = 2 mixed modes and discuss the interest of their measure to constrain the deeper layers of stars.

Benomar, O.; Bedding, T. R.; Stello, D.; White, T. R.; Kuehn, C. A. [Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006 (Australia); Mosser, B.; Belkacem, K. [LESIA, Observatoire de Paris, CNRS UMR 8109, Universite Paris Diderot, 5 Place J. Janssen, F-92195 Meudon (France); Garcia, R. A. [Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot (France); IRFU/SAp, Centre de Saclay, F-91191 Gif-sur-Yvette Cedex (France); Deheuvels, S. [Institut de Recherche en Astrophysique et Planetologie, Universite de Toulouse, UPS-OMP, CNRS, 14 Avenue Edouard Belin, F-31400 Toulouse (France); Christensen-Dalsgaard, J. [Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C (Denmark)

2013-04-20T23:59:59.000Z

420

Carbon and Strontium Abundances of Metal-Poor Stars  

E-Print Network (OSTI)

We present carbon and strontium abundances for 100 metal-poor stars measured from R$\\sim $7000 spectra obtained with the Echellette Spectrograph and Imager at the Keck Observatory. Using spectral synthesis of the G-band region, we have derived carbon abundances for stars ranging from [Fe/H]$=-1.3$ to [Fe/H]$=-3.8$. The formal errors are $\\sim 0.2$ dex in [C/Fe]. The strontium abundance in these stars was measured using spectral synthesis of the resonance line at 4215 {\\AA}. Using these two abundance measurments along with the barium abundances from our previous study of these stars, we show it is possible to identify neutron-capture-rich stars with our spectra. We find, as in other studies, a large scatter in [C/Fe] below [Fe/H]$ = -2$. Of the stars with [Fe/H]$<-2$, 9$\\pm$4% can be classified as carbon-rich metal-poor stars. The Sr and Ba abundances show that three of the carbon-rich stars are neutron-capture-rich, while two have normal Ba and Sr. This fraction of carbon enhanced stars is consistent with other studies that include this metallicity range.

David K. Lai; Jennifer A. Johnson; Michael Bolte; Sara Lucatello

2007-06-20T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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

Coordinate Data and Stars Identification in Astrophysical Catalogs  

E-Print Network (OSTI)

The aim of our paper is to make high-precision positional stellar catalogs by compiling large astrophysical data bulk and large astrometrical surveys. The data reliability and uniqueness is the primary request. The common precision of 1 arc sec in coordinates is insufficient now to guarantee the simple identification of stars. Therefore the technique of catalogs verification become relevant. The paper presents the outcome of stars identification in The Henry Draper Extension Charts catalog and Variable stars catalog using proper method. Examples of conflicts permission concerning doubles and multiples stars in astrophysical catalogs are discussed.

Ashimbaeva, Nuriya T

2008-01-01T23:59:59.000Z

422

Coordinate Data and Stars Identification in Astrophysical Catalogs  

E-Print Network (OSTI)

The aim of our paper is to make high-precision positional stellar catalogs by compiling large astrophysical data bulk and large astrometrical surveys. The data reliability and uniqueness is the primary request. The common precision of 1 arc sec in coordinates is insufficient now to guarantee the simple identification of stars. Therefore the technique of catalogs verification become relevant. The paper presents the outcome of stars identification in The Henry Draper Extension Charts catalog and Variable stars catalog using proper method. Examples of conflicts permission concerning doubles and multiples stars in astrophysical catalogs are discussed.

Nuriya T. Ashimbaeva

2008-10-01T23:59:59.000Z

423

Pre-Main Sequence Evolutions of Solar Abundance Lowmass Stars  

E-Print Network (OSTI)

We present the Pre-Main-Sequence (PMS) evolutionary tracks of stars with 0.0065~5.0Ms. The models were evolved from the PMS stellar birthline to the onset of hydrogen burning in the core. The convective turnover timescales which enables an observational test of theoretical model, particulary in the stellar dynamic activity, are also calculated. All models have Sun-like metal abundances, typically considered as the stars in the Galactic disk and the star formation region of Population I star. The convection phenomenon is treated by the usual mixing length approximation. All evolutionary tracks are available upon request.

Youn Kil Jung; Yong-Cheol Kim

2007-02-12T23:59:59.000Z

424

Chemical abundances of stars with brown-dwarf companions  

E-Print Network (OSTI)

It is well-known that stars with giant planets are on average more metal-rich than stars without giant planets, whereas stars with detected low-mass planets do not need to be metal-rich. With the aim of studying the weak boundary that separates giant planets and brown dwarfs (BDs) and their formation mechanism, we analyze the spectra of a sample of stars with already confirmed BD companions both by radial velocity and astrometry. We employ standard and automatic tools to perform an EW-based analysis and to derive chemical abundances from CORALIE spectra of stars with BD companions. We compare these abundances with those of stars without detected planets and with low-mass and giant-mass planets. We find that stars with BDs do not have metallicities and chemical abundances similar to those of giant-planet hosts but they resemble the composition of stars with low-mass planets. The distribution of mean abundances of $\\alpha$-elements and iron peak elements of stars with BDs exhibit a peak at about solar abundance...

Snchez, D Mata; Israelian, G; Santos, N C; Sahlmann, J; Udry, S

2014-01-01T23:59:59.000Z

425

EPA ENERGY STAR Webcast: Benchmarking Water/Wastewater Treatment...  

Energy Savers (EERE)

Benchmarking WaterWastewater Treatment Facilities in Portfolio Manager EPA ENERGY STAR Webcast: Benchmarking WaterWastewater Treatment Facilities in Portfolio Manager November...

426

ENERGY STAR Appliance Verification Testing - Pilot Program Summary...  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Appliance Verification Testing - Pilot Program Summary Report dated February 3, 2012 ENERGY STAR Appliance Verification Testing - Pilot Program Summary Report dated February 3,...

427

Calendar Year 2007 Program Benefits for ENERGY STAR Labeled Products  

E-Print Network (OSTI)

Administration, Office of Energy Markets and End Use.Administration, Office of Energy Markets and End Use.Protection Agency: ENERGY STAR Market Share of computers,

Sanchez, Marla Christine

2008-01-01T23:59:59.000Z

428

NEW YOUNG STAR CANDIDATES IN CG4 AND Sa101  

SciTech Connect

The CG4 and Sa101 regions together cover a region of {approx}0.5 deg{sup 2} in the vicinity of a 'cometary globule' that is part of the Gum Nebula. There are seven previously identified young stars in this region; we have searched for new young stars using mid- and far-infrared data (3.6-70 {mu}m) from the Spitzer Space Telescope, combined with ground-based optical data and near-infrared data from the Two Micron All Sky Survey. We find infrared excesses in all six of the previously identified young stars in our maps and identify 16 more candidate young stars based on apparent infrared excesses. Most (73%) of the new young stars are Class II objects. There is a tighter grouping of young stars and young star candidates in the Sa101 region, in contrast to the CG4 region, where there are fewer young stars and young star candidates, and they are more dispersed. Few likely young objects are found in the 'fingers' of the dust being disturbed by the ionization front from the heart of the Gum Nebula.

Rebull, L. M.; Laine, S.; Laher, R.; Legassie, M. [Spitzer Science Center/Caltech, M/S 220-6, 1200 E. California Blvd., Pasadena, CA 91125 (United States); Johnson, C. H. [Breck School Science Department, 123 Ottawa Ave., N., Golden Valley, MN 55422 (United States); Hoette, V. [The University of Chicago Department of Astronomy and Astrophysics, Yerkes Observatory Education and Outreach, 373 W. Geneva St., Williams Bay, WI 53191 (United States); Kim, J. S.; Foster, M. [Steward Observatory, University of Arizona, 933 N. Cherry Ave., Tucson, AZ 85721 (United States); Mallory, C. R. [Department of Astronomy, Pierce College, 6201 Winnetka Ave., Woodland Hills, CA 91371 (United States); McCarron, K. [Science Division, Oak Park and River Forest High School, 201 N. Scoville Ave., Oak Park, IL 60302 (United States); Sherry, W. H., E-mail: luisa.rebull@jpl.nasa.gov [NOAO/NSO, 950 N. Cherry Ave., Tucson, AZ 85719 (United States)

2011-07-15T23:59:59.000Z

429

The Federal Guiding Principles Checklist in ENERGY STAR Portfolio  

Energy.gov (U.S. Department of Energy (DOE))

This webcast will teach Federal energy and sustainability professionals how to use the ENERGY STAR measurement and tracking tool, Portfolio Manager, to help ensure compliance with the Guiding...

430

STAR Images: Image gallery from the Solenoidal Tracker at RHIC  

DOE Data Explorer (OSTI)

The primary physics task of STAR is to study the formation and characteristics of the quark-gluon plasma (QGP), a state of matter believed to exist at sufficiently high energy densities. STAR consists of several types of detectors, each specializing in detecting certain types of particles or characterizing their motion. These detectors allow final statements to be made about the collision. The gallery of STAR images makes available a small collection of event-generated images from Gold-Beam experiments, a simulation of TCP Drift, and a library of STAR instrument and construction photos. [See also DDE00093

431

Department of Energy Honors 50 ENERGY STAR Partners that Saved...  

Energy Savers (EERE)

security." ENERGY STAR began in 1992 as a voluntary, market-based partnership to reduce air pollution through increased energy efficiency. Today, DOE, in partnership with EPA,...

432

EPA ENERGY STAR Webcast - Successes in Sustainability: Tenants...  

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

Successes in Sustainability: Tenants and Landlords Team Up on Energy EPA ENERGY STAR Webcast - Successes in Sustainability: Tenants and Landlords Team Up on Energy November 12,...

433

Xcel Energy - Residential ENERGY STAR Rebate Program | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Residential ENERGY STAR Rebate Program Residential ENERGY STAR Rebate Program Xcel Energy - Residential ENERGY STAR Rebate Program < Back Eligibility Construction Residential Savings Category Home Weatherization Commercial Weatherization Sealing Your Home Appliances & Electronics Heating & Cooling Construction Commercial Heating & Cooling Design & Remodeling Ventilation Heating Commercial Lighting Lighting Water Heating Cooling Maximum Rebate Ground Source Heat Pump: $1500 Program Info Funding Source Home Performance with ENERGY STAR State Colorado Program Type Utility Rebate Program Rebate Amount Air Sealing and Weatherstripping: $160 Attic Insulation and Bypass Sealing: $350 High Efficiency Lighting: $40 Wall Insulation: $800 Set Back Thermostat: $25 Furnaces: $170 - $200 Boiler: $160 Electric Heat Pump: $550

434

Energy Star Building Upgrade Value Calculator | Open Energy Information  

Open Energy Info (EERE)

Energy Star Building Upgrade Value Calculator Energy Star Building Upgrade Value Calculator Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Energy Star Building Upgrade Value Calculator (for Office Properties) Agency/Company /Organization: ENERGY STAR Phase: "Evaluate Options and Determine Feasibility" is not in the list of possible values (Bring the Right People Together, Create a Vision, Determine Baseline, Evaluate Options, Develop Goals, Prepare a Plan, Get Feedback, Develop Finance and Implement Projects, Create Early Successes, Evaluate Effectiveness and Revise as Needed) for this property. User Interface: Spreadsheet Website: www.energystar.gov/index.cfm?c=comm_real_estate.building_upgrade_value The Building Upgrade Value Calculator allows practitioners to analyze the

435

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

436

FAQ's for: ENERGY STAR Verification Testing Pilot Program dated...  

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

faqfinaldecember-2010.pdf More Documents & Publications Comment submitted by the Alliance for Water Efficiency (AWE) regarding the Energy Star Verification Testing Program DOE...

437

Stars and gas in the Medusa merger  

E-Print Network (OSTI)

The Medusa (NGC 4194) is a well-studied nearby galaxy with the disturbed appearance of a merger and evidence for ongoing star formation. In order to test whether it could be the result of an interaction between a gas-rich disk-like galaxy and a larger elliptical, we have carried out optical and radio observations of the stars and the gas in the Medusa, and performed $N$-body numerical simulations of the evolution of such a system. We used the Nordic Optical Telescope to obtain a deep V-band image and the Westerbork Radio Synthesis Telescope to map the large-scale distribution and kinematics of atomic hydrogen. A single HI tail was found to the South of the Medusa with a projected length of 56 kpc (5') and a gas mass of 7* 10^8 M_sun, thus harbouring about one third of the total HI mass of the system. HI was also detected in absorption toward the continuum in the center. HI was detected in a small nearby galaxy to the North-West of the Medusa at a projected distance of 91 kpc. It is, however, unlikely that this galaxy has had a significant influence on the evolution of the Medusa. The simulations of the slightly prograde infall of a gas-rich disk galaxy on an larger, four time more massive elliptical (spherical) galaxy reproduce most of the observed features of the Medusa.Thus, the Medusa is an ideal object to study the merger-induced star formation contribution from the small galaxy of a minor merger.

E. Manthey; S. Huettemeister; S. Aalto; C. Horellou; P. Bjerkeli

2008-08-28T23:59:59.000Z

438

A Heavy Flavor Tracker for STAR  

SciTech Connect

The STAR Collaboration proposes to construct a state-of-the-art microvertex detector,the Heavy Flavor Tracker (HFT), utilizing active pixel sensors and silicon strip technology. The HFT will significantly extend the physics reach of the STAR experiment for precision measurement of the yields and spectra of particles containing heavy quarks. This will be accomplished through topological identification of D mesons by reconstruction of their displaced decay vertices with a precision of approximately 50 mu m in p+p, d+A, and A+A collisions. The HFT consists of 4 layers of silicon detectors grouped into two sub-systems with different technologies, guaranteeing increasing resolution when tracking from the TPC and the Silicon Strip Detector (SSD) towards the vertex of the collision. The Intermediate Silicon Tracker (IST), consisting of two layers of single-sided strips, is located inside the SSD. Two layers of Silicon Pixel Detector (PIXEL) are inside the IST. The PIXEL detectors have the resolution necessary for a precision measurement of the displaced vertex. The PIXEL detector will use CMOS Active Pixel Sensors (APS), an innovative technology never used before in a collider experiment. The APSsensors are only 50 mu m thick and at a distance of only 2.5 cm from the interaction point. This opens up a new realm of possibilities for physics measurements. In particular, a thin detector (0.28percent radiation length per layer) in STAR makes it possible to do the direct topological reconstruction of open charm hadrons down to very low pT by the identification of the charged daughters of the hadronic decay.

Chasman, C.; Beavis, D.; Debbe, R.; Lee, J.H.; Levine, M.J.; Videbaek, F.; Xu, Z.; Kleinfelder, S.; Li, S.; Cendejas, R.; Huang, H.; Sakai, S.; Whitten, C.; Joseph, J.; Keane, D.; Margetis, S.; Rykov, V.; Zhang, W.M.; Bystersky, M.; Kapitan, J.; Kushpil, V.; Sumbera, M.; Baudot, J.; Hu-Guo, C.; Shabetai, A.; Szelezniak, M.; Winter, M.; Kelsey, J.; Milner, R.; Plesko, M.; Redwine, R.; Simon, F.; Surrow, B.; Van Nieuwenhuizen, G.; Anderssen, E.; Dong, X.; Greiner, L.; Matis, H.S.; Morgan, S.; Ritter, H.G.; Rose, A.; Sichtermann, E.; Singh, R.P.; Stezelberger, T.; Sun, X.; Thomas, J.H.; Tram, V.; Vu, C.; Wieman, H.H.; Xu, N.; Hirsch, A.; Srivastava, B.; Wang, F.; Xie, W.; Bichsel, H.

2008-02-25T23:59:59.000Z

439

The Impact of College Students' Life Experiences on the Various Dimensions of Wellness: A Qualitative Study  

E-Print Network (OSTI)

, hereafter Lone Star Liberty University (LSLU). More specifically, this study aims at evaluating which particular dimension of wellness these health education majors perceive as most influenced or impacted, by their college life experience. 10..., hereafter Lone Star Liberty University (LSLU). More specifically, this study aims at evaluating which particular dimension of wellness these health education majors perceive as most influenced or impacted, by their college life experience. 10...

Garcia, Kristina Marie

2012-07-16T23:59:59.000Z

440

Energy Star Appliances 1 Texas A&M AgriLife Extension Service ENERGY STAR Appliances  

E-Print Network (OSTI)

Energy Star® Appliances 1 Texas A&M AgriLife Extension Service ENERGY STAR® Appliances ENERGY STAR®-labeled appliances save you money by using less electricity and water than other appliances. Better appliance energy efficiency comes from quality materials and technologically advanced materials. Although energy efficient

Note: This page contains sample records for the topic "waha lone star" 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

Helium enhancements in globular cluster stars from Asymptotic Giant Branch star pollution  

E-Print Network (OSTI)

Using a chemical evolution model we investigate the intriguing suggestion that there are populations of stars in some globular clusters (e.g. NGC 2808, omega Centauri) with enhanced levels of helium (Y from about 0.28 to 0.40) compared to the majority of the population that presumably have a primordial helium abundance. We assume that a previous generation of massive low-metallicity Asymptotic Giant Branch (AGB) stars has polluted the cluster gas via a slow stellar wind. We use two independent sets of AGB yields computed from detailed models to follow the evolution of helium, carbon, nitrogen and oxygen in the cluster gas using a Salpeter initial mass function (IMF) and a number of top-heavy IMFs. In no case were we able to fit the observational constraints, Y > 0.30 and C+N+O approximately constant. Depending on the shape of the IMF and the yields, we either obtained Y approximately greater than 0.30 and large increases in C+N+O or Y < 0.30 and C+N+O approximately constant. These results suggest that either AGB stars alone are not responsible for the large helium enrichment or that any dredge-up from this generation of stars was less than predicted by standard models.

Amanda Karakas; Yeshe Fenner; Alison Sills; Simon Campbell; John Lattanzio

2006-05-21T23:59:59.000Z

442

Portfolio Manager | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Tools and resources Tools and resources » Portfolio Manager 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 Success stories

443

Recognition | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Recognition Recognition 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 Success stories Target Finder Technical documentation

444

Training | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Training Training 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 Facility owners and managers Service providers Energy efficiency program administrators Tools and resources Training Training EPA offers training on a range of energy efficiency topics - from the ins and outs of Portfolio Manager to guidance on improving the energy performance of your buildings and plants. And that's all with no travel,

445

Financial resources | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Tools and resources Tools and resources » Financial resources 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 Success stories

446

Retail resources | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Retail resources Retail resources 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 Success stories Target Finder Technical documentation

447

Find financing | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Find financing Find financing 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 Learn the benefits Get started Use Portfolio Manager Save energy Find financing Calculate returns on energy efficiency investments Rebates, incentives, and financing services Public sector financing options Earn recognition Communicate your success Find financing Postponing the installation of energy-saving equipment can be an expensive

448

Technical documentation | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Technical documentation Technical documentation 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 Success stories Target Finder

449

Success stories | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Success stories Success stories 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 Success stories Target Finder Technical documentation

450

Communications resources | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Tools and resources Tools and resources » Communications resources 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 Success stories

451

Front end electronics for the STAR TPC  

SciTech Connect

The Solenoidal Tracker at RHIC (STAR) is a large acceptance detector now being built to study high energy heavy ion collisions. It detects charged particles with a large time projection chamber. The 136,600 TPC pads are instrumented with waveform digitizers, implemented in custom low noise preamplifier/shaper and switched capacitor array/ADCs ICs. The system is highly integrated with all analog functions mounted on small cards that plug into the TPC. Detector mounted readout boards multiplex data from 1,152 channels onto a 1.5 Gbit/sec fiber optic link to the data acquisition system.

Klein, S.R.; Barale, P.; Beuville, E. [and others

1995-10-01T23:59:59.000Z

452

Compact boson stars in K field theories  

E-Print Network (OSTI)

We study a scalar field theory with a non-standard kinetic term minimally coupled to gravity. We establish the existence of compact boson stars, that is, static solutions with compact support of the full system with self-gravitation taken into account. Concretely, there exist two types of solutions, namely compact balls on the one hand, and compact shells on the other hand. The compact balls have a naked singularity at the center. The inner boundary of the compact shells is singular, as well, but it is, at the same time, a Killing horizon. These singular, compact shells therefore resemble black holes.

C. Adam; N. Grandi; P. Klimas; J. Sanchez-Guillen; A. Wereszczynski

2009-09-16T23:59:59.000Z

453

Compact boson stars in K field theories  

E-Print Network (OSTI)

We study a scalar field theory with a non-standard kinetic term minimally coupled to gravity. We establish the existence of compact boson stars, that is, static solutions with compact support of the full system with self-gravitation taken into account. Concretely, there exist two types of solutions, namely compact balls on the one hand, and compact shells on the other hand. The compact balls have a naked singularity at the center. The inner boundary of the compact shells is singular, as well, but it is, at the same time, a Killing horizon. These singular, compact shells therefore resemble black holes.

Adam, C; Klimas, P; Snchez-Guilln, J; Wereszczynski, A

2009-01-01T23:59:59.000Z

454

Holographic cold nuclear matter and neutron star  

E-Print Network (OSTI)

We have previously found a new phase of cold nuclear matter based on a holographic gauge theory, where baryons are introduced as instanton gas in the probe D8/$\\overline{\\rm D8}$ branes. In our model, we could obtain the equation of state (EOS) of our nuclear matter by introducing fermi momentum. Then, here we apply this model to the neutron star and study its mass and radius by solving the Tolman-Oppenheimer-Volkoff (TOV) equations in terms of the EOS given here. We give some comments for our holographic model from a viewpoint of the other field theoretical approaches.

Kazuo Ghoroku; Kouki Kubo; Motoi Tachibana; Fumihiko Toyoda

2013-11-07T23:59:59.000Z

455

Photon emission from bare quark stars  

E-Print Network (OSTI)

We investigate the photon emission from the electrosphere of a quark star. It is shown that at temperatures T\\sim 0.1-1 MeV the dominating mechanism is the bremsstrahlung due to bending of electron trajectories in the mean Coulomb field of the electrosphere. The radiated energy for this mechanism is much larger than that for the Bethe-Heitler bremsstrahlung. The energy flux from the mean field bremsstrahlung exceeds the one from the tunnel e^{+}e^{-} pair creation as well. We demonstrate that the LPM suppression of the photon emission is negligible.

B. G. Zakharov

2010-08-16T23:59:59.000Z

456

Scalar Dark Matter and Cold Stars  

E-Print Network (OSTI)

In a medium composed of scalar particles with non-zero mass, the range of Van-der-Waals-type scalar mediated interactions among nucleons becomes infinite when the medium makes a transition to a Bose-Einstein condensed phase. We explore this phenomenon in an astrophysical context. Namely, we study the effect of a scalar dark matter background on the equilibrium of degenerate stars.In particular we focus on white dwarfs and the changes induced in their masses and in their radii.

J. A. Grifols

2005-05-30T23:59:59.000Z

457

Star Formation in the Local Universe  

E-Print Network (OSTI)

We present preliminary results of a long-term study aimed at answering a number of open questions on the evolution of starbursts in local galaxies. The project employes mainly HST data from the ultraviolet to the red of the stellar continuum and of the nebular emission from the galaxies. Here we concentrate on NGC5253 and NGC5236 (M83), that form a dwarf--massive galaxy pair at about 4 Mpc distance. The recent star formation history of the centers of the two galaxies is investigated in order to identify similarities and differences in the evolution of their central starbursts.

Daniela Calzetti; Jason Harris

2001-11-28T23:59:59.000Z

458

Sound velocity bound and neutron stars  

E-Print Network (OSTI)

It has been conjectured that the velocity of sound in any medium is smaller than the velocity of light in vacuum divided by $\\sqrt{3}$. Simple arguments support this bound in non-relativistic and/or weakly coupled theories. The bound has been demonstrated in several classes of strongly coupled theories with gravity duals and is saturated only in conformal theories. We point out that the existence of neutron stars with masses around two solar masses combined with the knowledge of the equation of state of hadronic matter at "low" densities is in strong tension with this bound.

Paulo F. Bedaque; Andrew W. Steiner

2015-01-25T23:59:59.000Z

459

Low Dimensional Dynamics in a Pulsating Star  

E-Print Network (OSTI)

We report the discovery of a low dimensional dynamical system in a 5.5 hr Hubble Space Telescope High Speed Photometer observation of a rapidly oscillating star. The topological description of the phase space orbits is given, as well as a dynamical model which describes the results. This model should motivate theorists of stellar pulsations to search for a three-dimensional system with the same topological structure to describe the mechanisms for pulsation. The equations are compatible with recently proposed nonlinear mode interaction models.

G. B. Mindlin; P. T. Boyd; J. L. Caaminos; J. A. Nunez

1995-10-31T23:59:59.000Z

460

Portfolio Manager | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Manager Manager 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 Success stories Target Finder Technical documentation

Note: This page contains sample records for the topic "waha lone star" 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

On the state of low luminous accreting neutron stars  

E-Print Network (OSTI)

Observational appearance of a neutron star in the subsonic propeller state which is a companion of a wind-fed mass-exchange close binary system is discussed. During the subsonic propeller state the neutron star magnetosphere is surrounded by a spherical quasi-static plasma envelope, which is extended from the magnetospheric boundary up to the star accretion radius. The energy input to the envelope due to the propeller action by the neutron star exceeds the radiative losses and the plasma temperature in the envelope is of the order of the free-fall temperature. Under this condition the magnetospheric boundary is interchange stable. Nevertheless, I find that the rate of plasma penetration from the envelope into the magnetic field of the neutron star due to diffusion and magnetic field line reconnection processes is large enough for the accretion power to dominate the spindown power. I show that the accretion luminosity of the neutron star in the subsonic propeller state is 5*10**{30} - 10**{33} (dM/dt)_{15} erg/s, where dM/dt is the strength of the normal companion stellar wind which is parametrized in terms of the maximum possible mass accretion rate onto the neutron star magnetosphere. On this basis I suggest that neutron stars in the subsonic propeller state are expected to be observed as low luminous accretion-powered pulsars. The magnetospheric radius of the neutron star in this state is determined by the strength of the stellar wind, (dM/dt)_c, while the accretion luminosity is determined by the rate of plasma penetration into the star magnetosphere, (dM/dt)_a, which is (dM/dt)_a << (dM/dt)_c. That is why the classification of the neutron star state in these objects using the steady accretion model (i.e. setting (dM/dt)_a = (dM/dt)_c) can lead to a mistaken conclusion.

Nazar Ikhsanov

2001-06-26T23:59:59.000Z

462

E-Print Network 3.0 - ancient star forming Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

star forming Search Powered by Explorit Topic List Advanced Search Sample search results for: ancient star forming Page: << < 1 2 3 4 5 > >> 1 OHIR STARS AS SIGNPOSTS FOR ANCIENT...

463

BETA STABLE NEUTRON STARS IN NON-LINEAR RELATIVISTIC MEAN FIELD MODELS  

E-Print Network (OSTI)

on the Beta Stability in Neutron Stars, LBL-11465 (to bealter the predicted neutron star properties. This work wasReferences For a review of neutron stars and a detailed list

Boguta, J.

2014-01-01T23:59:59.000Z

464

E-Print Network 3.0 - ae star hd Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

field measurements of the Herbig Ae stars HD 101412 (left panel) and HD 150193 (right panel) (FORS 2... cool stars and solar-like stars Instrumentation The most successful...

465

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

466

Shear viscosity in neutron star cores  

E-Print Network (OSTI)

We calculate the shear viscosity $\\eta = \\eta_{e\\mu}+\\eta_{n}$ in a neutron star core composed of nucleons, electrons and muons ($\\eta_{e\\mu}$ being the electron-muon viscosity, mediated by collisions of electrons and muons with charged particles, and $\\eta_{n}$ the neutron viscosity, mediated by neutron-neutron and neutron-proton collisions). Deriving $\\eta_{e\\mu}$, we take into account the Landau damping in collisions of electrons and muons with charged particles via the exchange of transverse plasmons. It lowers $\\eta_{e\\mu}$ and leads to the non-standard temperature behavior $\\eta_{e\\mu}\\propto T^{-5/3}$. The viscosity $\\eta_{n}$ is calculated taking into account that in-medium effects modify nucleon effective masses in dense matter. Both viscosities, $\\eta_{e\\mu}$ and $\\eta_{n}$, can be important, and both are calculated including the effects of proton superfluidity. They are presented in the form valid for any equation of state of nucleon dense matter. We analyze the density and temperature dependence of $\\eta$ for different equations of state in neutron star cores, and compare $\\eta$ with the bulk viscosity in the core and with the shear viscosity in the crust.

P. S. Shternin; D. G. Yakovlev

2008-08-14T23:59:59.000Z

467

Neutron star accretion and the neutrino fireball  

SciTech Connect

The mixing necessary to explain the Fe'' line widths and possibly the observed red shifts of 1987A is explained in terms of large scale, entropy conserving, up and down flows (calculated with a smooth particle 2-D code) taking place between the neutron star and the explosion shock wave due to the gravity and neutrino deposition. Depending upon conditions of entropy and mass flux further accretion takes place in single events, similar to relaxation oscillator, fed by the downward flows of low entropy matter. The shock, in turn, is driven by the upflow of the buoyant high entropy bubbles. Some accretion events will reach a temperature high enough to create a neutrino fireball,'' a region hot enough, 11 Mev, so as to be partially opaque to its own (neutrino) radiation. The continuing neutrino deposition drives the explosion shock until the entropy of matter flowing downwards onto the neutron star is high enough to prevent further accretion. This process should result in a robust supernova explosion.

Colgate, S.A. (Los Alamos National Lab., NM (United States)); Herant, M.E. (Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States)); Benz, W. (Steward Observatory, Tucson, AZ (United States))

1991-11-26T23:59:59.000Z

468

Neutron star accretion and the neutrino fireball  

SciTech Connect

The mixing necessary to explain the ``Fe`` line widths and possibly the observed red shifts of 1987A is explained in terms of large scale, entropy conserving, up and down flows (calculated with a smooth particle 2-D code) taking place between the neutron star and the explosion shock wave due to the gravity and neutrino deposition. Depending upon conditions of entropy and mass flux further accretion takes place in single events, similar to relaxation oscillator, fed by the downward flows of low entropy matter. The shock, in turn, is driven by the upflow of the buoyant high entropy bubbles. Some accretion events will reach a temperature high enough to create a neutrino ``fireball,`` a region hot enough, 11 Mev, so as to be partially opaque to its own (neutrino) radiation. The continuing neutrino deposition drives the explosion shock until the entropy of matter flowing downwards onto the neutron star is high enough to prevent further accretion. This process should result in a robust supernova explosion.

Colgate, S.A. [Los Alamos National Lab., NM (United States); Herant, M.E. [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (United States); Benz, W. [Steward Observatory, Tucson, AZ (United States)

1991-11-26T23:59:59.000Z

469

TOPICAL REVIEW: General relativistic boson stars  

E-Print Network (OSTI)

There is accumulating evidence that (fundamental) scalar fields may exist in Nature. The gravitational collapse of such a boson cloud would lead to a boson star (BS) as a new type of a compact object. Similarly as for white dwarfs and neutron stars, there exists a limiting mass, below which a BS is stable against complete gravitational collapse to a black hole. According to the form of the self-interaction of the basic constituents and the spacetime symmetry, we can distinguish mini-, axidilaton, soliton, charged, oscillating and rotating BSs. Their compactness prevents a Newtonian approximation, however, modifications of general relativity, as in the case of Jordan-Brans-Dicke theory as a low energy limit of strings, would provide them with gravitational memory. In general, a BS is a compact, completely regular configuration with structured layers due to the anisotropy of scalar matter, an exponentially decreasing 'halo', a critical mass inversely proportional to constituent mass, an effective radius, and a large particle number. Due to the Heisenberg principle, there exists a completely stable branch, and as a coherent state, it allows for rotating solutions with quantised angular momentum. In this review, we concentrate on the fascinating possibilities of detecting the various subtypes of (excited) BSs: Possible signals include gravitational redshift and (micro-)lensing, emission of gravitational waves, or, in the case of a giant BS, its dark matter contribution to the rotation curves of galactic halos.

Franz E. Schunck; Eckehard W. Mielke

2008-01-01T23:59:59.000Z

470

Mutual Friction in Superfluid Neutron Stars  

E-Print Network (OSTI)

We discuss vortex-mediated mutual friction in the two-fluid model for superfluid neutron star cores. Our discussion is based on the general formalism developed by Carter and collaborators, which makes due distinction between transport velocity and momentum for each fluid. This is essential for an implementation of the so-called entrainment effect, whereby the flow of one fluid imparts momentum in the other and vice versa. The mutual friction follows by balancing the Magnus force that acts on the quantised neutron vortices with a resistive force due to the scattering of electrons off of the magnetic field with which each vortex core is endowed. We derive the form of the macroscopic mutual friction force which is relevant for a model based on smooth-averaging over a collection of vortices. We discuss the coefficients that enter the expression for this force, and the timescale on which the two interpenetrating fluids in a neutron star core are coupled. This discussion confirms that our new formulation accords well with previous work in this area.

N. Andersson; T. Sidery; G. L. Comer

2005-10-03T23:59:59.000Z

471

HOT GAS LINES IN T TAURI STARS  

SciTech Connect

For Classical T Tauri Stars (CTTSs), the resonance doublets of N V, Si IV, and C IV, as well as the He II 1640 A line, trace hot gas flows and act as diagnostics of the accretion process. In this paper we assemble a large high-resolution, high-sensitivity data set of these lines in CTTSs and Weak T Tauri Stars (WTTSs). The sample comprises 35 stars: 1 Herbig Ae star, 28 CTTSs, and 6 WTTSs. We find that the C IV, Si IV, and N V lines in CTTSs all have similar shapes. We decompose the C IV and He II lines into broad and narrow Gaussian components (BC and NC). The most common (50%) C IV line morphology in CTTSs is that of a low-velocity NC together with a redshifted BC. For CTTSs, a strong BC is the result of the accretion process. The contribution fraction of the NC to the C IV line flux in CTTSs increases with accretion rate, from {approx}20% to up to {approx}80%. The velocity centroids of the BCs and NCs are such that V{sub BC} {approx}> 4 V{sub NC}, consistent with the predictions of the accretion shock model, in at most 12 out of 22 CTTSs. We do not find evidence of the post-shock becoming buried in the stellar photosphere due to the pressure of the accretion flow. The He II CTTSs lines are generally symmetric and narrow, with FWHM and redshifts comparable to those of WTTSs. They are less redshifted than the CTTSs C IV lines, by {approx}10 km s{sup -1}. The amount of flux in the BC of the He II line is small compared to that of the C IV line, and we show that this is consistent with models of the pre-shock column emission. Overall, the observations are consistent with the presence of multiple accretion columns with different densities or with accretion models that predict a slow-moving, low-density region in the periphery of the accretion column. For HN Tau A and RW Aur A, most of the C IV line is blueshifted suggesting that the C IV emission is produced by shocks within outflow jets. In our sample, the Herbig Ae star DX Cha is the only object for which we find a P-Cygni profile in the C IV line, which argues for the presence of a hot (10{sup 5} K) wind. For the overall sample, the Si IV and N V line luminosities are correlated with the C IV line luminosities, although the relationship between Si IV and C IV shows large scatter about a linear relationship and suggests that TW Hya, V4046 Sgr, AA Tau, DF Tau, GM Aur, and V1190 Sco are silicon-poor, while CV Cha, DX Cha, RU Lup, and RW Aur may be silicon-rich.

Ardila, David R. [NASA Herschel Science Center, California Institute of Technology, MC 100-22, Pasadena, CA 91125 (United States); Herczeg, Gregory J. [Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871 (China); Gregory, Scott G.; Hillenbrand, Lynne A. [Cahill Center for Astronomy and Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA 91125 (United States); Ingleby, Laura; Bergin, Edwin; Bethell, Thomas; Calvet, Nuria [Department of Astronomy, University of Michigan, 830 Dennison Building, 500 Church Street, Ann Arbor, MI 48109 (United States); France, Kevin; Brown, Alexander [Center for Astrophysics and Space Astronomy, University of Colorado, Boulder, CO 80309-0389 (United States); Edwards, Suzan [Department of Astronomy, Smith College, Northampton, MA 01063 (United States); Johns-Krull, Christopher [Department of Physics and Astronomy, Rice University, Houston, TX 77005 (United States); Linsky, Jeffrey L. [JILA, University of Colorado and NIST, 440 UCB Boulder, CO 80309-0440 (United States); Yang, Hao [Institute for Astrophysics, Central China Normal University, Wuhan 430079 (China); Valenti, Jeff A. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Abgrall, Herve [LUTH and UMR 8102 du CNRS, Observatoire de Paris, Section de Meudon, Place J. Janssen, F-92195 Meudon (France); Alexander, Richard D. [Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom); Brown, Joanna M.; Espaillat, Catherine [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 78, Cambridge, MA 02138 (United States); Hussain, Gaitee, E-mail: ardila@ipac.caltech.edu [ESO, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei Muenchen (Germany); and others

2013-07-01T23:59:59.000Z

472

2008 Status Report - Savings Estimates for the ENERGY STAR Voluntary  

NLE Websites -- All DOE Office Websites (Extended Search)

Status Report - Savings Estimates for the ENERGY STAR Voluntary Status Report - Savings Estimates for the ENERGY STAR Voluntary Labeling Program Title 2008 Status Report - Savings Estimates for the ENERGY STAR Voluntary Labeling Program Publication Type Journal Article LBNL Report Number LBNL-56380 Year of Publication 2007 Authors Sanchez, Marla C., Carrie A. Webber, Richard E. Brown, and Gregory K. Homan Date Published 11/2007 Publisher Lawrence Berkeley National Laboratory ISBN Number LBNL-56380(2008) Keywords Enduse, Energy End-Use Forecasting, EUF Abstract ENERGY STAR is a voluntary labeling program designed to identify and promote energy-efficient products, buildings and practices. Operated jointly by the Environmental Protection Agency (EPA) and the U.S. Department of Energy (DOE), ENERGY STAR includes more than thirty products, spanning office equipment, residential heating and cooling equipment, commercial and residential lighting, home electronics, and major appliances. This report presents savings estimates for ENERGY STAR labeled products. We present estimates of energy, dollar, and carbon savings achieved by the program in the year 2007, what we expect in 2008, and provide savings forecasts for the periods 2008 to 2015 and 2008 to 2025. The forecast represents our best estimate of future ENERGY STAR savings. It is based on realistic ENERGY STAR unit sales for each of the products.

473

NEWS & VIEWS nEutRon StaRS  

E-Print Network (OSTI)

NEWS & VIEWS nEutRon StaRS a magnetar by another name Fernando Camilo is at the Columbia core, held stable by neutron degeneracy pressure -- with more mass than the Sun within a 10 km radius -- has central densities comparable to those of nuclei. What does the neutron star sky look like, made

Loss, Daniel

474

Some Observational Aspects of R Coronae Borealis Stars  

E-Print Network (OSTI)

Some of the observational aspects related to the evolutionary status and dust production in R Cor Bor stars are discussed. Recent work regarding the surface abundances, stellar winds and evidence for dust production in these high luminosty hydrogen deficient stars are also reviewed. Possibility of the stellar winds being maintained by surface magnetic fields is also considered.

N. Kameswara Rao

2007-12-24T23:59:59.000Z

475

Star formation triggered by SNR impact into magnetized neutral clouds  

E-Print Network (OSTI)

Considering the physical conditions that are relevant for triggering star formation in interactions involving SN shocks and neutral clouds, we have built diagrams of the SNR radius versus the cloud density in which these conditions constrain a shaded zone where star formation is allowed. The diagrams are also tested with fully 3-D MHD radiative cooling simulations involving a SNR and a self-gravitating cloud and we find that the numerical analysis is consistent with the results predicted by the diagrams. While the inclusion of a homogeneous magnetic field approximately perpendicular to the impact velocity of the SNR with an intensity ~1 $mu$G results only a small shrinking of the star formation zone in the diagrams, a larger magnetic field (~10 $\\mu$G) causes a significant shrinking, as expected. Applications of our results to real star formation regions in our own galaxy have revealed that their formation could have been triggered by a SN shock wave. Finally, we have evaluated the effective global star formation efficiency of this sort of interactions and found that it is smaller than the observed values in our Galaxy (SFE ~0.01-0.3). This result is consistent with previous work in the literature and also suggests that the mechanism presently investigated, though very powerful to drive structure formation, supersonic turbulence and eventually, local star formation, does not seem to be sufficient to drive global star formation in normal star forming galaxies.

M. R. M. Leao; E. M. de Gouveia Dal Pino; D. Falceta-Goncalves; C. Melioli; F. G. Geraissate

2008-10-29T23:59:59.000Z

476

Hyperon stars at finite temperature in the Brueckner theory  

E-Print Network (OSTI)

We perform Brueckner-Hartree-Fock calculations of hypernuclear matter at finite temperature and provide convenient analytical parametrizations of the results. We study then the properties of (proto)neutron stars containing hyperons. We find important effects of trapping and finite temperature on the structure of hyperonic stars.

Burgio, G F; Li, A

2011-01-01T23:59:59.000Z

477

Hyperon stars at finite temperature in the Brueckner theory  

Science Journals Connector (OSTI)

We perform Brueckner-Hartree-Fock calculations of hypernuclear matter at finite temperature and provide convenient analytical parametrizations of the results. We then study the properties of (proto)neutron stars containing hyperons. We find important effects of trapping and finite temperature on the structure of hyperonic stars.

G. F. Burgio; H.-J. Schulze; A. Li (??)

2011-02-17T23:59:59.000Z

478

Heartbeat Stars and the Ringing of Tidal Pulsations Kelly Hambleton  

E-Print Network (OSTI)

Heartbeat Stars and the Ringing of Tidal Pulsations Kelly Hambleton Andrej Prsa, Don Kurtz, Jim Fuller, Susan Thompson University of Central Lancashire kmhambleton@uclan.ac.uk March 27, 2014 Kelly 3 Summary Conclusions Future Work Kelly Hambleton (UCLan) Heartbeat Stars March 27, 2014 2 / 33 #12

?umer, Slobodan

479

Modelling the hidden magnetic field of low-mass stars  

Science Journals Connector (OSTI)

......angular momentum in the wind remains unaffected...spin-down times and mass-loss rates calculated...coronae|stars: low-mass|stars: magnetic...planets by radial velocity searches. Despite...the powerful stellar winds (Vidotto et-al...order to reconstruct a map of the vector magnetic......

P. Lang; M. Jardine; J. Morin; J.-F. Donati; S. Jeffers; A. A. Vidotto; R. Fares

2014-01-01T23:59:59.000Z

480

The brightest stars of the sigma Orionis cluster  

E-Print Network (OSTI)

Context: The very young sigma Orionis cluster (about 3 Ma) is a cornerstone for the understanding of the formation of stars and substellar objects down to planetary masses. However, its stellar population is far to be completely known. Aims: This study has the purpose of identyfing and characterising the most massive stars of sigma Orionis to complement current and future deep searches for brown dwarfs and planetary-mass objects in the cluster. Methods: I have cross-correlated the sources in the Tycho and 2MASS catalogues in a region of 30 arcmin radius with centre in the O-type star sigma Ori A. In the area, I have studied the membership in the Ori OB 1b Association of the brightest stars in the optical using astrometric, X-ray and infrared and optical photometric data from public catalogues and spectroscopic data from the literature. Results: A list of 26 young stars, four candidate young stars and 16 probable foreground stars has arised from the study. Seven young stars probably harbour discs (four are new). There is no mass-dependence of the disc frequency in the cluster. I have derived for the first time the mass spectrum in sigma Orionis from 1.1 to 24 Msol (alpha = +2.0+0.2-0.1; roughly Salpeter-like). I have also provided additional proofs on the existence of several spatially superimposed stellar populations in the direction of sigma Orionis. Finally, the cluster may be closer and older than previously considered.

J. A. Caballero

2007-01-03T23:59:59.000Z

Note: This page contains sample records for the topic "waha lone star" 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.


481

Star-Forming Structures in Perseus Advisor: Prof. Alyssa Goodman  

E-Print Network (OSTI)

is a spectral energy dis- tribution (SED) shifted deep into the infrared, relative to a main sequence starStar-Forming Structures in Perseus Tom Laakso Advisor: Prof. Alyssa Goodman May 15th 2006 Abstract This year, both the Spitzer c2d legacy project and the COMPLETE survey have released new infrared

Harvard-Smithsonian Center for Astrophysics,

482

AN INFRARED CENSUS OF STAR FORMATION IN THE HORSEHEAD NEBULA  

SciTech Connect

At {approx} 400 pc, the Horsehead Nebula (B33) is the closest radiatively sculpted pillar to the Sun, but the state and extent of star formation in this structure is not well understood. We present deep near-infrared (IRSF/SIRIUS JHK {sub S}) and mid-infrared (Spitzer/IRAC) observations of the Horsehead Nebula to characterize the star-forming properties of this region and to assess the likelihood of triggered star formation. Infrared color-color and color-magnitude diagrams are used to identify young stars based on infrared excess emission and positions to the right of the zero-age main sequence, respectively. Of the 45 sources detected at both near- and mid-infrared wavelengths, three bona fide and five candidate young stars are identified in this 7' x 7' region. Two bona fide young stars have flat infrared spectral energy distributions and are located at the western irradiated tip of the pillar. The spatial coincidence of the protostars at the leading edge of this elephant trunk is consistent with the radiation-driven implosion model of triggered star formation. There is no evidence, however, for sequential star formation within the immediate {approx} 1.'5 (0.17 pc) region from the cloud/H II region interface.

Bowler, Brendan P. [Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States); Waller, William H. [Department of Physics and Astronomy, Tufts University, Medford, MA 02155 (United States); Megeath, S. Thomas [Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606 (United States); Patten, Brian M. [National Science Foundation, 4201 Wilson Blvd. Arlington, VA 22230 (United States); Tamura, Motohide [National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588 (Japan)], E-mail: bpbowler@ifa.hawaii.edu, E-mail: william.waller@tufts.edu, E-mail: megeath@physics.utoledo.edu, E-mail: bpatten@nsf.gov, E-mail: motohide.tamura@nao.ac.jp

2009-03-15T23:59:59.000Z

483

THE STAR FORMATION LAW AT LOW SURFACE DENSITY  

SciTech Connect

We investigate the nature of the star formation law at low gas surface densities using a sample of 19 low surface brightness (LSB) galaxies with existing H I maps in the literature, UV imaging from the Galaxy Evolution Explorer satellite, and optical images from the Sloan Digital Sky Survey. All of the LSB galaxies have (NUV - r) colors similar to those for higher surface brightness star-forming galaxies of similar luminosity indicating that their average star formation histories are not very different. Based upon four LSB galaxies with both UV and far-infrared (FIR) data, we find FIR/UV ratios significantly less than 1, implying low amounts of internal UV extinction in LSB galaxies. We use the UV images and H I maps to measure the star formation rate (SFR) and hydrogen gas surface density within the same region for all the galaxies. The LSB galaxy star formation rate surface densities lie below the extrapolation of the power law fit to the SFR surface density as a function of the total gas density for higher surface brightness galaxies. Although there is more scatter, the LSB galaxies also lie below a second version of the star formation law in which the SFR surface density is correlated with the gas density divided by the orbital time in the disk. The downturn seen in both star formation laws is consistent with theoretical models that predict lower star formation efficiencies in LSB galaxies due to the declining molecular fraction with decreasing density.

Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Foster, Karl; Friedman, Peter G.; Morrissey, Patrick; Neill, James D. [California Institute of Technology, MC 278-17, 1200 E. California Blvd., Pasadena, CA 91125 (United States); Neff, Susan G. [Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD, 20771 (United States); Schiminovich, David [Department of Astronomy, Columbia University, New York, NY 10027 (United States); Seibert, Mark; Madore, Barry F. [Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Bianchi, Luciana [Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 (United States); Donas, Jose; Milliard, Bruno [Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12 (France); Heckman, Timothy M.; Szalay, Alex S. [Department of Physics and Astronomy, Johns Hopkins University, Homewood Campus, Baltimore, MD 21218 (United States); Lee, Young-Wook; Yi, Sukyoung K. [Center for Space Astrophysics, Yonsei University, Seoul 120-749 (Korea, Republic of); Rich, R. Michael [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States)

2009-05-10T23:59:59.000Z

484

Making Sun-Earth Connections: Our Star Our Sun  

E-Print Network (OSTI)

1 Making Sun-Earth Connections: Our Star ­ Our Sun Presenter's Guide Grades: 3-5 #12;2 Making Sun-Earth Connections: Our Star ­ Our Sun Table of Contents: Slides and Captions: 1. Introduction and Space Exploration.........................................3 4. Structure of the Sun

Maxwell, Bruce D.

485

Utility Rebates for ENERGY STAR Appliances: Are They Effective?  

E-Print Network (OSTI)

Utility Rebates for ENERGY STAR Appliances: Are They Effective? Souvik Datta Sumeet Gulati CEPE;UTILITY REBATES FOR ENERGY STAR APPLIANCES: ARE THEY EFFECTIVE? SOUVIK DATTA ETH Z¨urich SUMEET GULATI by utility companies. To estimate the impact of these incentives we use the variation in timing and size

486

Theoretical Aspects of Star Formation Richard B. Larson  

E-Print Network (OSTI)

astrophysical processes: not only do the properties of stellar systems of all types depend on how their stars involved are just too numerous and too complex: star formation depends on many processes and many variables, all interrelated in complex ways that make the subject difficult to treat in a deterministic way

Larson, Richard B.

487

Texas LoanSTAR Program Savings Calculation Workbook  

E-Print Network (OSTI)

This is the report and manual for the Texas LoanSTAR Program Savings Calculation Workbook. The purpose of this report is to document the Texas LoanSTAR Program Savings Calculation Workbook to be used by the State Energy Conservation Office (SECO...

Liu, Z.; Baltazar-Cervantes, J. C.; Haberl, J. S.

2003-01-01T23:59:59.000Z

488

X-ray Emission from Massive Stars David Cohen  

E-Print Network (OSTI)

X-ray Emission from Massive Stars David Cohen Department of Physics and Astronomy Swarthmore University, Oct. 13, 2005 astro.swarthmore.edu/~cohen/ #12;Outline 1. What you need to know: a. X-rays from the Sun - magnetic activity, x-ray spectra b. Hot stars c. Radiation-driven winds and the Doppler shift d

Cohen, David

489

Calendar Year 2007 Program Benefits for U.S. EPA Energy Star Labeled Products: Expanded Methodology  

E-Print Network (OSTI)

Administration, Office of Energy Markets and End Use.Administration, Office of Energy Markets and End Use.Total Shipments Star Energy Market Star Share Shipments

Sanchez, Marla

2010-01-01T23:59:59.000Z

490

E-Print Network 3.0 - ankle replacement star Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

star Search Powered by Explorit Topic List Advanced Search Sample search results for: ankle replacement star Page: << < 1 2 3 4 5 > >> 1 BOSTON UNIVERSITY COLLEGE OF ENGINEERING...

491

BLAST: studying cosmic and Galactic star formation from a stratospheric balloon.  

E-Print Network (OSTI)

??Understanding the history of the formation of stars and evolution of galaxies is one of the foremost goals of astrophysics. While stars emit most of (more)

Moncelsi, Lorenzo

2011-01-01T23:59:59.000Z

492

E-Print Network 3.0 - accretion stars Sample Search Results  

NLE Websites -- All DOE Office Websites (Extended Search)

accretion... transfer. Mass transfer manifests itself by accretion onto the star and windjet outflows while angular... rotation rate of young stars. ... Source: Ecole...

493

North Star Refrigerator: Proposed Penalty (2013-CE-5355) | Department of  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

North Star Refrigerator: Proposed Penalty (2013-CE-5355) North Star Refrigerator: Proposed Penalty (2013-CE-5355) North Star Refrigerator: Proposed Penalty (2013-CE-5355) March 26, 2013 DOE alleged in a Notice of Proposed Civil Penalty that North Star Refrigerator Co., Inc. failed to certify a variety of walk-in cooler or freezer components as compliant with the applicable energy conservation standards. DOE regulations require a manufacturer (which includes importers) to submit reports certifying that its products have been tested and meet the applicable energy conservation standards. This civil penalty notice advises the company of the potential penalties and DOE's administrative process, including the company's right to a hearing. North Star Refrigerator: Proposed Penalty (2013-CE-5355) More Documents & Publications

494

Learn about benchmarking | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Learn about benchmarking Learn about benchmarking 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use Learn about benchmarking Use ENERGY STAR benchmarking tools ENERGY STAR in action Communicate and educate Find out who's partnered with ENERGY STAR

495

Service and product provider's marketing toolkit | ENERGY STAR Buildings  

NLE Websites -- All DOE Office Websites (Extended Search)

Service and product provider's marketing toolkit Service and product provider's marketing toolkit 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 How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner ENERGY STAR service & product provider training series Service and product provider's marketing toolkit Industry initiatives ENERGY STAR sales tools for service and product providers

496

MHK Technologies/CurrentStar | Open Energy Information  

Open Energy Info (EERE)

CurrentStar CurrentStar < MHK Technologies Jump to: navigation, search << Return to the MHK database homepage CurrentStar.jpg Technology Profile Primary Organization Bourne Energy Technology Resource Click here Current Technology Type Click here Axial Flow Turbine Technology Description The CurrentStar series is designed to harness the enormous potential source of clean energy in ocean currents Ocean currents flow at all depths in the ocean but the strongest usually occur in the upper layer Technology Dimensions Length (m) 30.5 Width (m) 30.5 Freeboard (m) 3.65 Technology Nameplate Capacity (MW) 1 Device Testing Date Submitted 42:27.8 << Return to the MHK database homepage Retrieved from "http://en.openei.org/w/index.php?title=MHK_Technologies/CurrentStar&oldid=6815

497

Denver Watts to Water | ENERGY STAR Buildings & Plants  

NLE Websites -- All DOE Office Websites (Extended Search)

Denver Watts to Water Denver Watts to Water 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 How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use ENERGY STAR in action Communicate and educate ENERGY STAR communications toolkit Bring Your Green to Work with ENERGY STAR

498

City of Tallahassee Utilities - Energy Star Certified New Homes Rebate  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Tallahassee Utilities - Energy Star Certified New Homes Tallahassee Utilities - Energy Star Certified New Homes Rebate Program City of Tallahassee Utilities - Energy Star Certified New Homes Rebate Program < Back Eligibility Multi-Family Residential Residential Savings Category Heating & Cooling Home Weatherization Construction Commercial Weatherization Commercial Heating & Cooling Design & Remodeling Maximum Rebate $2,000 Program Info State Florida Program Type Utility Rebate Program Rebate Amount $1 per square foot Provider City of Tallahassee Utilities The City of Tallahassee Utilities offers a rebate of $1 per square foot (up to $2,000) for ENERGY STAR qualified new homes. Qualifying housing types include single-family detached, single-family attached, low-rise multifamily, and existing-home renovations. To earn the ENERGY STAR, a home

499

Streamlining ENERGY STAR Appliance Testing | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

Streamlining ENERGY STAR Appliance Testing Streamlining ENERGY STAR Appliance Testing Streamlining ENERGY STAR Appliance Testing September 26, 2013 - 11:46am Addthis To save taxpayer dollars and help lower the costs of innovative energy-efficient technologies, the Energy Department is streamlining ENERGY STAR testing for appliances such as clothes washers. | Photo courtesy of Bethany Sparn, National Renewable Energy Laboratory. To save taxpayer dollars and help lower the costs of innovative energy-efficient technologies, the Energy Department is streamlining ENERGY STAR testing for appliances such as clothes washers. | Photo courtesy of Bethany Sparn, National Renewable Energy Laboratory. John Cymbalsky Program Manager, Appliance and Equipment Standards & Building Codes What does this mean for me?

500

STAR Teaching Program Application Period | Department of Energy  

Energy.gov (U.S. Department of Energy (DOE)) Indexed Site

STAR Teaching Program Application Period STAR Teaching Program Application Period STAR Teaching Program Application Period December 28, 2012 2:30PM EST to January 31, 2013 5:30PM EST Cal Poly The Science Teacher and Researcher (STAR) Researcher program, a collaborative project of California State University, provides pre-service and early career science teachers with eight week long paid mentor and research opportunities at a national research center. Applicants must have the following: A demonstrated interest in becoming a science or mathematics teacher at the secondary level (grades 6-12) Either a California State University (CSU) student OR NSF Noyce Scholar in the United States OR a STAR Alum with two or fewer years of participation AND two or fewer years of teaching experience (first time participants must be pre-service teachers, i.e., not yet teaching full-time