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Note: This page contains sample records for the topic "ames ia 630-252-3721" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of 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

CONTACT LIST Records Management Field Officers (RMFOs) PRGM  

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

PRGM PRGM NAME PRGM OFC EMPLOY LOCATION PHONE EMAIL Ames Lab Tehan, Amy Ames Laboratory Federal Ames, IA 630-252-3721 ajotehan@ameslab.gov ANL Martin, Mary L. Argonne National Laboratory Contractor Germantown, MD 630-252-3721 mmartin@anl.gov BHSO Nekulak, Kim Brookhaven Site Office Federal Upton, NY 631-344-7439 knekulak@bnl.gov BNL Flood, Patricia E. Brookhaven National Laboratory Contractor Upton, NY 631-344-7886 flood@bnl.gov BPA Frost, Christopher Bonneville Power Administration Federal Portland, OR 503-230-5602 cmfrost@bpa.gov CB Chism, Lea Carlsbad Field Office Federal Carlsbad, NM 575-234-7442 lea.chism@wipp.ws CH Lane, Georgette M. Chicago Operations Office Federal Argonne, IL 630-252-8906 georgette.lane@ch.doe.gov EMCBC Reid, Kathy Portsmouth Paducah Project Office (PPPO, EM Small Sites: GE Vallecitos, Inhalation Toxicology Lab,

2

CP Tech Center I Iowa State University I 2711 S. Loop Dr. Suite 4700,Ames, IA 50010-8664 I 515-294-5798 FOR MORE INFORMATION  

E-Print Network [OSTI]

CP Tech Center I Iowa State University I 2711 S. Loop Dr. Suite 4700,Ames, IA 50010-8664 I 515 calcium sulfate in the form of hemihydrate (plaster) in the cement (false set) or the uncontrolled early

3

DOE - Office of Legacy Management -- Ames Laboratory Research...  

Office of Legacy Management (LM)

Ames Laboratory Research Reactor Facility - IA 03 FUSRAP Considered Sites Site: Ames Laboratory Research Reactor Facility (IA.03) Designated Name: Alternate Name: Location:...

4

Phenotypic Data Collection and Sample Preparation for Genomics of Wood Formation and Cellulosic Biomass Traits in Sunflower: Ames, IA location.  

SciTech Connect (OSTI)

Three fields were planted in Ames in 2010, two association mapping fields, N3 and A, and a recombinant inbred line field, N13. Phenotype data and images were transferred to UGA to support genetic and genomic analyses of woody biomass-related traits.

Marek, Laura F.

2011-06-17T23:59:59.000Z

5

DOE - Office of Legacy Management -- Iowa State University Ames Laboratory  

Office of Legacy Management (LM)

Iowa State University Ames Iowa State University Ames Laboratory - IA 01 FUSRAP Considered Sites Site: Iowa State University Ames Laboratory (IA.01 ) Eliminated from further consideration under FUSRAP Designated Name: Not Designated Alternate Name: None Location: Wallace Road , Ames , Iowa IA.01-1 IA.01-2 Evaluation Year: Circa 1985 IA.01-3 Site Operations: Produced uranium and thorium metal, recovered uranium scrap, and conducted studies and experimental investigations in connection with chemistry and metallurgy of natural uranium and its allied forms. IA.01-1 IA.01-4 IA.01-5 IA.01-6 IA.01-7 Site Disposition: Eliminated - Referred to Chicago Operations Office for appropriate action IA.01-6 Radioactive Materials Handled: Yes Primary Radioactive Materials Handled: Uranium, Thorium IA.01-1

6

Ames Laboratory Logos | The Ames Laboratory  

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

Ames Laboratory Logos The Ames Laboratory Logo comes in several formats. EPS files are vector graphics created in Adobe Illustrator and saved with a tiff preview so they will...

7

jevans | The Ames Laboratory  

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

jevans Ames Laboratory Profile James Evans Associate 315 Wilhelm Phone Number: 515-294-1638 Email Address: evans@ameslab.gov Ames Laboratory Associate and Professor, Iowa State...

8

SULI at Ames Laboratory  

SciTech Connect (OSTI)

A video snapshot of the Science Undergraduate Laboratory Internship (SULI) program at Ames Laboratory.

None

2011-01-01T23:59:59.000Z

9

Ames Laboratory Site Sustainability Plan | The Ames Laboratory  

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

Ames Laboratory Site Sustainability Plan Document Number: NA Effective Date: 122012 File (public): Ames FY2013 SSP FINAL.pdf...

10

aerospace & mechanical (AME) AME overview programs available  

E-Print Network [OSTI]

22 aerospace & mechanical (AME) AME overview · programs available courses of instruction-thruster (the Free Molecule Micro-Resistojet) and the aerodynamics of ground vehicles. Mechanical Engineering Mechanical Engineers apply scientific methodology to find solutions to mechanical problems and to create

Rohs, Remo

11

Ames Laboratory Research Reactor Facility Ames, Iowa  

Office of Legacy Management (LM)

,, *' ; . Final Radiological Condition of the Ames Laboratory Research Reactor Facility Ames, Iowa _, . AGENCY: Office of Operational Safety, Department of Energy ' ACTION: Notice of Availability of Archival Information Package SUMMARY: The'Office of Operational Safety of the Department O i Energy (DOE) has reviewed documentation relating to the decontamination and decommissioning operations conducted at the Ames Laboratory Research Reactor Facility, Ames, Iowa and has prepared an archival informati0.n package to permanently document the results of the action and the site conditions and use restriction placed on the . site at the tim e of release. This review is based on post-decontamination survey data and other pertinent documentation referenced in and included in the archival package. The material and

12

budko | The Ames Laboratory  

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

budko Ames Laboratory Profile Serguei Budko Scientist I Division of Materials Science & Engineering A111 Zaffarano Phone Number: 515-294-3986 Email Address: budko@ameslab.gov...

13

Disclaimers | The Ames Laboratory  

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

of the United States Government or Iowa State University, and shall not be used for advertising or product endorsements purposes. COPYRIGHT STATUS: Ames Laboratory authored...

14

marit | The Ames Laboratory  

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

marit Ames Laboratory Profile Marit Nilsen-Hamilton Associate 3206 Molecular Biology Bldg Phone Number: 515-294-9996 Email Address: marit@iastate.edu Education: Postdoctoral Cell...

15

Factsheets | The Ames Laboratory  

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

disruptions. Image Rare Earths Info Card This handy pocket card highlights the rare earth elements on the front and provides information on the back concerning Ames...

16

Sustainability | The Ames Laboratory  

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

Sustainability Ames Laboratory is committed to environmental sustainability in all of its operations as outlined in the Laboratory's Site Sustainability Plan. Executive orders set...

17

Ames Lab 101: Technology Transfer  

SciTech Connect (OSTI)

Ames Laboratory Associate Laboratory Director, Sponsored Research Administration, Debra Covey discusses technology transfer. Covey also discusses Ames Laboratory's most successful transfer, lead-free solder.

Covey, Debra

2010-01-01T23:59:59.000Z

18

Home | Ames Laboratory  

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

ABOUT | NEED A MATERIAL | NEWS CENTER | RESEARCH | TECH ABOUT | NEED A MATERIAL | NEWS CENTER | RESEARCH | TECH TRANSFER | CONTACT search LOG IN | RARE EARTH METALS | CRITICAL MATERIALS INSTITUTE | STAFF/ASSOCIATES | VISITORS | BE A PART OF AMES LAB | STUDENTS | EDUCATORS | FUNDING AGENCIES | INDUSTRY | RESEARCHERS | COMMUNITY RARE EARTH METALS Current Market Prices About Rare Earth Metals Materials Preparation STAFF/ASSOCIATES Operations Forms & Documents Find People VISITORS How To Get Here Tours of Ames Laboratory Local Events Calendar BE A PART OF AMES LAB Job News Human Resources Ames Lab At A Glance STUDENTS K-12 Resources Undergraduates Graduates and Others EDUCATORS Science Bowl SULI Program VFP Program FUNDING AGENCIES DOE/Contractor Research Highlights Contract INDUSTRY Technology Transfer Unique Capabilities

19

Initiatives | The Ames Laboratory  

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

and Development PRIMROSE- Primary Research Into Magnetic Resonance Of the Solid-state for Energy GReen Advances for Catalysis and Energy (GRACE) AMES will be a world leader in...

20

AMEE | Open Energy Information  

Open Energy Info (EERE)

AMEE AMEE Jump to: navigation, search Name AMEE Place London, United Kingdom Sector Carbon Product AMEE aims to build the largest engine to calculate carbon footprints for organisations, companies and individuals. Clients include Morgan Stanley, Google, UK Department of Energy and Climate Change Coordinates 51.506325°, -0.127144° 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":51.506325,"lon":-0.127144,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Ames Lab 101: Danny Shechtman Returns to the Ames Laboratory  

ScienceCinema (OSTI)

Danny Shechtman, Ames Laboratory Scientist and winner of the Nobel Prize in Chemistry 2011, returned to the Ames Lab on February 14, 2012. During this time, the Nobel Laureate met with the press as well as ISU students.

Shechtman, Danny

2013-03-01T23:59:59.000Z

22

Routine environmental audit of Ames Laboratory, Ames, Iowa  

SciTech Connect (OSTI)

This document contains the findings identified during the routine environmental audit of Ames Laboratory, Ames, Iowa, conducted September 12--23, 1994. The audit included a review of all Ames Laboratory operations and facilities supporting DOE-sponsored activities. The audit`s objective is to advise the Secretary of Energy, through the Assistant Secretary for Environment, Safety and Health, as to the adequacy of the environmental protection programs established at Ames Laboratory to ensure the protection of the environment, and compliance with Federal, state, and DOE requirements.

NONE

1994-09-01T23:59:59.000Z

23

johnson2 | The Ames Laboratory  

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

johnson2 Ames Laboratory Profile Stacie Johnson Lab Assistant-X Environmental & Protective Sciences 5 Spedding Phone Number: 515-294-2069 Email Address: johnson2...

24

Records Management | The Ames Laboratory  

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

Training, Documents, & Records Records Management The Records Management Program at the Ames Laboratory provides guidance and assistance for administrative departments and...

25

2012 Professional Development Meeting; Ames, IA Research update: Bee health  

E-Print Network [OSTI]

, pumpkins · Cantaloupes, watermelons · Carrots, canola, alfalfa · Almonds, macadamia and other nut crops #12+ million ac), most wheat (24 million ac), canola, cotton, etc. · Rates range from 0.25-1.25 mg

Jurenka, Russell A.

26

Ames Lab 101: Rare Earths  

ScienceCinema (OSTI)

"Mr. Rare Earth," Ames Laboratory scientist Karl Gschneidner Jr., explains the importance of rare-earth materials in many of the technologies we use today -- ranging from computers to hybrid cars to wind turbines. Gschneidner is a world renowned rare-earths expert at the U.S. Department of Energy's Ames Laboratory.

Gschneidner, Karl

2012-08-29T23:59:59.000Z

27

Latest Feature Video | The Ames Laboratory  

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

the Science Undergraduate Laboratory Internship (SULI) program at the Ames Laboratory. Printing 3D Catalytic Devices Ames Laboratory scientist Igor Slowing discusses using 3D...

28

Who We Are - Ames Laboratory's Brand | The Ames Laboratory  

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

State University. But really, who are we and what do we do? In other words, what's our brand? Through the efforts of a branding committee, Ames Laboratory's strengths were...

29

Ames Laboratory | Open Energy Information  

Open Energy Info (EERE)

Ames Laboratory Ames Laboratory Jump to: navigation, search Name Ames Laboratory Place Ames, Iowa Zip 50011-3020 Product Research facility focused on solutions to energy-related problems. Coordinates 30.053389°, -94.742269° 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":30.053389,"lon":-94.742269,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

30

Licensing Oppurtunities | The Ames Laboratory  

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

with the US Treasury. Ames Laboratory has been the only Laboratory to have returned royalty income to the US Treasury and has done so for the last 5 years. For additional...

31

Welcome to the Ames Laboratory  

ScienceCinema (OSTI)

Alex King, director of The Ames Laboratory, discusses the state of the Lab for 2011, the goals of the Lab and the importance of the research taking place here.

King, Alex

2013-03-01T23:59:59.000Z

32

IA Blog Archive  

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

71 IA Blog Archive en IA News Archive http:energy.goviaia-news-archive IA News Archive

33

Environmental Survey preliminary report, Ames Laboratory, Ames, Iowa  

SciTech Connect (OSTI)

This report presents the preliminary findings of the first phase of the environmental Survey of the United States Department of Energy's (DOE) Ames Laboratory, conducted April 18 through 22, 1988. The Survey is being conducted by an interdisciplinary team of environmental specialists, led and managed by the Office of Environment, Safety and Health's Office of Environmental Audit. Individual team members are being supplied by private contractors. The objective of the Survey is to identify environmental problems and areas of environmental risk associated with the Ames Laboratory. The Survey covers all environmental media and all areas of environmental regulation. It is being performed in accordance with the DOE Environmental Survey Manual. This phase of the Survey involves the review of existing site environmental data, observations of the operations carried on at the Ames Laboratory, and interviews with site personnel. The Survey team developed a Sampling and Analysis (S A) Plan to assist in further assessing certain of the environmental problems identified during its on-site activities. The S A plan is being developed by the Idaho National Engineering Laboratory. When S A is completed, the results will be incorporated into the Ames Laboratory Environmental Survey findings for inclusion in the Environmental Survey Summary Report. 60 refs., 13 figs., 20 tabs.

Not Available

1989-03-01T23:59:59.000Z

34

Ames Lab 101: Science Bowl 2011  

ScienceCinema (OSTI)

High school students from across Iowa converged on Ames Jan. 30, 2011 to compete in the 21st annual Ames Laboratory/Iowa State University Regional High School Science Bowl.

None

2013-03-01T23:59:59.000Z

35

The Ames Project (1942-1946)  

ScienceCinema (OSTI)

The Ames Laboratory was officially founded on May 17, 1947, following development of a process to purify uranium metal for the historic Manhattan Project. From 1942 to 1946, Ames Lab scientists produced over two-million pounds of uranium metal. A U.S. Department of Energy national research laboratory, the Ames Laboratory creates materials and energy solutions. Iowa State University operates Ames Laboratory under contract with the DOE.

None

2013-06-05T23:59:59.000Z

36

Hybrid Model Structures Aaron David Ames  

E-Print Network [OSTI]

Hybrid Model Structures by Aaron David Ames B.A. (University of St. Thomas) 2001 B.S. (University of California, Berkeley Fall 2006 #12;Hybrid Model Structures Copyright 2006 by Aaron David Ames #12;Abstract Hybrid Model Structures by Aaron David Ames Masters of Arts in Mathematics University of California

Ames, Aaron

37

Ames Site Ofice 9800 South Cass Avenue  

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

of Energy of Energy Ames Site Ofice 9800 South Cass Avenue Argonne, Illinois 60439 January 15, 2013 MEMORANDUM FOR GREGORY H. WOODS, GENERAL COUNSEL OFFICE OF THE GENERAL COUNSEL FROM: SUBJECT: CYNTHIA BAEBLER, MANAGER iLJ�= AMES SITE OFFICE AMES SITE OFFICE (AMSO) 2013 ANNUAL NATIONAL ENVIRONMENTAL POLICY ACT (NEPA) PLANNING SUMMARY Section 5(a)(7) of DOE Order 451.1B Change 3, NEPA Compliance Program, requires

38

Materials Discovery Design, Synthesis & Processing | The Ames...  

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

Materials Discovery Design, Synthesis & Processing Vision: AMES will be the premier U.S. laboratory lusing an "atoms to applications" approach to discover and design new materials....

39

Ames Lab 101: Improving Solar Cell Efficiency  

ScienceCinema (OSTI)

Rana Biswas, a scientist with the Ames Laboratory, discusses his team's research in creating more efficient solar cells and working with Iowa Thin Film to produce these cells.

Biswas, Rana

2012-08-29T23:59:59.000Z

40

Materials and Transportation Services | The Ames Laboratory  

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

Materials and Transportation Services General Information: Materials and Transportation Services provides Ames Laboratory employees with a wide array of services and support...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Facilties & Engineering Services | The Ames Laboratory  

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

Facilties & Engineering Services The Facilities Services Group (FSG) is responsible for the facilities and infrastructure of the Ames Laboratory. The group includes custodial...

42

Environmental Management System Steering Committee | The Ames...  

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

Environmental Management System Steering Committee The Environmental Management System Steering Committee (EMSSC) is a standing Ames Laboratory committee that advises the members...

43

Ames Lab 101: Improving Solar Cell Efficiency  

SciTech Connect (OSTI)

Rana Biswas, a scientist with the Ames Laboratory, discusses his team's research in creating more efficient solar cells and working with Iowa Thin Film to produce these cells.

Biswas, Rana

2011-01-01T23:59:59.000Z

44

Foreign Visits & Assignments Guidelines | The Ames Laboratory  

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

Visits and Assignments Request Form, as well as the Ames Laboratory Specific Security Plan Form. Form 473 Foreign Visits and Assignments Request Form Specific Security Plan...

45

Latest News Releases | The Ames Laboratory  

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

within the nanoparticles to maximize catalytic output. Read More Ames Laboratory 3D printing technology research taking shape 09232014 Scientists at the U.S. Department of...

46

Expedited Site Characterization | The Ames Laboratory  

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

money in the characterization of DOE sites, Ames Lab scientists are advancing adoption of innovative technologies along with a more efficient characterization method. What we are...

47

Ames Lab 101: VE-Suite  

ScienceCinema (OSTI)

Ames Laboratory scientist Mark Bryden talks about virtual engineering and the advantages it gives engineers when they can "walk through" designs visually.

Bryden, Mark

2012-08-29T23:59:59.000Z

48

Materials Preparation Center | Ames Laboratory  

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

Materials Preparation Center Materials Preparation Center Materials Preparation Center The Materials Preparation Center (MPC) is a U.S. Department of Energy, Office of Science, Office of Basic Energy Sciences, Division of Materials Sciences & Engineering specialized research center located at the Ames Laboratory. MPC operations are primarily funded by the Materials Discovery, Design, & Synthesis team's Synthesis & Processing Science core research activity. MPC is recognized throughout the worldwide research community for its unique capabilities in purification, preparation, and characterization of: Rare earth metals [learn about rare earths] Single crystal growth Metal Powders/Atomization Alkaline-earth metals [learn more, wikipedia] External Link Icon Refractory metal [learn more, wikipedia] External Link Icon

49

UESC Project Overview: NASA Ames Research Center  

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

NASA Ames Research Center NASA Ames Research Center Utility Energy Services Contract Project Overview Federal Utilities Partnership Working Group Philadelphia, PA October 2011 NASA Ames Research Center Utility Energy Services Contract 2 Today's Discussion * NASA Ames Research Center (ARC) Energy Challenges * UESC Project Goals * Energy and Water Conservation Projects * Project Benefits and Results * Q&A NASA Ames Research Center Utility Energy Services Contract 3 NASA's Energy Challenges * Compliance with federal mandates - EISA, EPAct, Executive Orders (prior to UESC ARC was behind all of its goals) * Very low electric cost (<$0.05/kWh) * Not eligible for electric incentives through local utility (ARC purchases power from WAPA) * Aging mechanical and electrical infrastructure requiring significant

50

Tom Lograsso, Ames Laboratory (Iowa State University), Future...  

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

Tom Lograsso, Ames Laboratory (Iowa State University), Future Directions in Rare Earth Research: Critical Materials for 21st Century Industry Tom Lograsso, Ames Laboratory (Iowa...

51

Ames Lab 101: Reinventing the Power Cable  

ScienceCinema (OSTI)

Ames Laboratory researchers are working to develop new electrical power cables that are stronger and lighter than the cables currently used in the nation's power grid. Nano Tube animation by Iain Goodyear

Russell, Alan

2014-06-04T23:59:59.000Z

52

Ames Lab 101: Rare-Earth Magnets  

ScienceCinema (OSTI)

Senior Scientist, Bill McCallum, briefly discusses rare-earth magnets and their uses and how Ames Lab is research new ways to save money and energy using magnets.

McCallum, Bill

2012-08-29T23:59:59.000Z

53

Ames Lab 101: Reinventing the Power Cable  

SciTech Connect (OSTI)

Ames Laboratory researchers are working to develop new electrical power cables that are stronger and lighter than the cables currently used in the nation's power grid. Nano Tube animation by Iain Goodyear

Russell, Alan

2013-09-27T23:59:59.000Z

54

Ames Lab 101: Next Generation Power Lines  

SciTech Connect (OSTI)

Ames Laboratory scientist Alan Russell discusses the need to develop new power lines that are stronger and more conductive as a way to address the problem of the nation's aging and inadequate power grid.

Russell, Alan

2010-01-01T23:59:59.000Z

55

Middle School Science Bowl | The Ames Laboratory  

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

of Energy's National competition The academic competition The Ames LabISU Middle School Science Bowl is one of 50 regional competitions held across the nation. It is a...

56

Ames Site Office 9800 South Cass Avenue  

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

Ames Site Office Ames Site Office 9800 South Cass Avenue Argonne, Illinois 60439 January 9, 2012 MEMORANDUM FOR TIMOTHY G. LYNCH FROM : DEPUTY GENERAL COUSNEL FOR LITIGATION CYNTHIA K. BAEBLER MANAGER SUBJECT: AMES SITE OFFICE (AMSO) 2012 ANNUAL NATIONAL ENVIRONMENTAL POLICY ACT (NEPA) PLANNING SUMMARY Section 5(a)(7) of DOE Order 451.1B Change 2, NEPA Compliance Program, requires each Secretarial Officer and Head of Field Organization to submit an annual NEPA Annual Planning Summary to the Office of General Counsel. We have reviewed your associated December 5, 2011, memorandum and in consultation with Ames Laboratory staff determined that we have no Environmental Impacts Statements or Environmental Assessments either ongoing or forecast for the next 12 to 24 months.

57

Ames Lab 101: osgBullet  

ScienceCinema (OSTI)

Ames Laboratory scientist Doug McCorkle explains osgBullet, a 3-D virtual simulation software, and how it helps engineers design complex products and systems in a realistic, real-time virtual environment.

McCorkle, Doug

2012-08-29T23:59:59.000Z

58

Ames Lab Named an Industry Safety Leader  

ScienceCinema (OSTI)

The U.S. Department of Energy's Ames Laboratory has been named a 2010 Industry Leader Award winner by the National Safety Council. The Ames Laboratory was one of only 81 companies/organizations to receive the award for their safety performance and the only DOE national laboratory on the list. The award represents the top 5 percent of members that have qualified for the National Safety Council 2010 Occupational Excellence Achievement Award, based on 2009 calendar year data.

Wessels, Tom

2013-03-01T23:59:59.000Z

59

Chemical studies of the Ames oxydesulfurization process  

SciTech Connect (OSTI)

The validity of the Ames claim of up to 40% removal of organic sulfur from coal was assessed by subjecting model compounds to the Ames Process which utilizes 0.2 M aqueous Na/sub 2/CO/sub 3/ at 150/sup 0/C under pressure of 300 psi O/sub 2/ for one hour. This type of oxydesulfurization has been described as a two step process involving initial oxidation at sulfur to produce sulfoxides and sulfones. This step is then thought to be followed by the thermal and, in the Ames Process, base assisted extrusion of SO/sub x/. In this concept, the initial oxidation at sulfur facilitates desulfurization by polarizing and weakening the carbon to sulfur bond. The conclusions concerning the oxydesulfurization process are: (1) thiophenols and disulfides are the only groups oxidized at sulfur; (2) sulfides, including thiophenes, are not oxidized at sulfur; (3) reactive sulfides are oxidized at reactive carbon-hydrogen bonds; (4) reactive carbon-hydrogen bonds in functions not containing sulfur also react; (5) the Ames Process is directly analogous to hydrocarbon autoxidation; and (6) more efficient sulfur removal without severe degradation of the coal is not possible under the present process conditions. The success which these model compound studies have had in defining the limits of the efficacy of the Ames oxydesulfurization process encourage one to believe that this approach will be quite valuable in the evaluation of other proposed chemical coal cleaning techniques.

Squires, T.G.; Venier, C.G.; Chang, L.W.; Schmidt, T.E.

1981-03-29T23:59:59.000Z

60

Transforming BIM to BEM: Generation of Building Geometry for the NASA Ames Sustainability Base BIM  

E-Print Network [OSTI]

Building Geometry for the NASA Ames Sustainability Base BIMBuilding Geometry for the NASA Ames Sustainability Base BIMusing the recently constructed NASA Ames Sustainability Base

O'Donnell, James T.

2014-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

The State of the Ames Laboratory Address 2011  

ScienceCinema (OSTI)

Alex King, director of The Ames Laboratory, discusses the budget situation, improvements at Ames Lab and infrastructure improvements during the State of the Lab address on Tuesday, May 24, 2011.

King, Alex

2013-03-01T23:59:59.000Z

62

2013 Annual Planning Summary for the Ames Site Office  

Broader source: Energy.gov [DOE]

The ongoing and projected Environmental Assessments and Environmental Impact Statements for 2013 and 2014 within theAmes Site Office.

63

Ames Lab 101: Rare-Earth Recycling  

SciTech Connect (OSTI)

Recycling keeps paper, plastics, and even jeans out of landfills. Could recycling rare-earth magnets do the same? Perhaps, if the recycling process can be improved. Scientists at the U.S. Department of Energy's Ames Laboratory are working to more effectively remove the neodymium, a rare earth, from the mix of other materials in a magnet.

Ryan Ott

2012-09-05T23:59:59.000Z

64

Ames Lab 101: Single Crystal Growth  

SciTech Connect (OSTI)

Ames Laboratory scientist Deborah Schlagel talks about the Lab's research in growing single crystals of various metals and alloys. The single crystal samples are vital to researchers' understanding of the characteristics of a materials and what gives these materials their particular properties.

Schlagel, Deborah

2013-09-27T23:59:59.000Z

65

Ames Lab 101: Ultrafast Magnetic Switching  

SciTech Connect (OSTI)

Ames Laboratory physicists have found a new way to switch magnetism that is at least 1000 times faster than currently used in magnetic memory technologies. Magnetic switching is used to encode information in hard drives, magnetic random access memory and other computing devices. The discovery potentially opens the door to terahertz and faster memory speeds.

Jigang Wang

2013-04-08T23:59:59.000Z

66

Ames Lab 101: Ultrafast Magnetic Switching  

ScienceCinema (OSTI)

Ames Laboratory physicists have found a new way to switch magnetism that is at least 1000 times faster than currently used in magnetic memory technologies. Magnetic switching is used to encode information in hard drives, magnetic random access memory and other computing devices. The discovery potentially opens the door to terahertz and faster memory speeds.

Jigang Wang

2013-06-05T23:59:59.000Z

67

Ames, Iowa: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

Ames, Iowa: Energy Resources Ames, Iowa: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 42.02335°, -93.625622° 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":42.02335,"lon":-93.625622,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

68

Research Summary Namrata Vaswani, ECE Dept, Iowa State University, Ames, IA  

E-Print Network [OSTI]

solution with very high complexity. The alternative 5 10 15 20 0 0.01 0.02 0.03 Time |Nt\\Nt-1| |Nt to the 99% energy support of the 2D discrete wavelet transform of the cardiac sequence of Fig. 1(b (modified-CS). Fig. 1(b) is for a sparsified car

Vaswani, Namrata

69

Category:Mason, IA | Open Energy Information  

Open Energy Info (EERE)

IA IA Jump to: navigation, search Go Back to PV Economics By Location Media in category "Mason, IA" The following 16 files are in this category, out of 16 total. SVQuickServiceRestaurant Mason IA MidAmerican Energy Co (Iowa).png SVQuickServiceRestaura... 64 KB SVFullServiceRestaurant Mason IA MidAmerican Energy Co (Iowa).png SVFullServiceRestauran... 64 KB SVHospital Mason IA MidAmerican Energy Co (Iowa).png SVHospital Mason IA Mi... 73 KB SVLargeHotel Mason IA MidAmerican Energy Co (Iowa).png SVLargeHotel Mason IA ... 72 KB SVLargeOffice Mason IA MidAmerican Energy Co (Iowa).png SVLargeOffice Mason IA... 73 KB SVMediumOffice Mason IA MidAmerican Energy Co (Iowa).png SVMediumOffice Mason I... 69 KB SVMidriseApartment Mason IA MidAmerican Energy Co (Iowa).png

70

DC Optimal Power Flow Formulation in AMES Leigh Tesfatsion  

E-Print Network [OSTI]

@iastate.edu, http://www.econ.iastate.edu/tesfatsi/ Fig. 1. AMES day-ahead energy market activities during each day D wholesale power market testbed. I. AMES TESTBED The latest version of AMES (Agent-based Modeling.econ.iastate.edu/tesfatsi/AMESLMPDetermination.LT.pdf this objective, the ISO operates a day-ahead energy market settled by means of LMP. The welfare of each LSE j

Tesfatsion, Leigh

71

Sandia National Laboratories: NASA Ames Research Center in northern...  

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

NASA Ames Research Center in northern California Sierra Unmanned Aerial Vehicle to Begin Flights Over Arctic Sea Ice On July 25, 2013, in Climate, Customers & Partners, Global,...

72

Ames Lab 101: Improving Materials with Advanced Computing  

ScienceCinema (OSTI)

Ames Laboratory's Chief Research Officer Duane Johnson talks about using advanced computing to develop new materials and predict what types of properties those materials will have.

Johnson, Duane

2014-06-04T23:59:59.000Z

73

Printing 3D Catalytic Devices | The Ames Laboratory  

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

Printing 3D Catalytic Devices Ames Laboratory scientist Igor Slowing discusses using 3D printers to create new materials, including catalysts...

74

SULI student wins Goldwater Scholarship | The Ames Laboratory  

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

SULI student wins Goldwater Scholarship SULI student Robin Lindemann talks about winning the Goldwater Scholarship and how his internship experience at Ames Laboratory helped him...

75

Rapporteurs Report: Tom Lograsso, Ames Laboratory and Nick Morley...  

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

LSRapporteursReport.doc More Documents & Publications Trans-Atlantic Workshop on Rare Earth Elements and Other Critical Materials for a Clean Energy Future Tom Lograsso, Ames...

76

Nanomaterials Safety Implementation Plan, Ames Laboratory | Department of  

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

Nanomaterials Safety Implementation Plan, Ames Laboratory Nanomaterials Safety Implementation Plan, Ames Laboratory Nanomaterials Safety Implementation Plan, Ames Laboratory Ames Laboratory has limited activities involving nanomaterials. Potential hazards associated with nanomaterials work are addressed through the Laboratory's Integrated Safety Management System (ISMS) and specifically the Readiness Review process. Readiness Review provides the identification and evaluation of potential hazards and establishes effective control mechanisms to ensure protection of the employee and the environment. To date, hazards associated with projects involving nanomaterials have been determined to be amenable to conventional controls such as ventilation and use of personal protective equipment. The Laboratory recognizes that nanotechnology is an emerging field and that

77

Bloodstain Pattern Analysis Video Collection | The Ames Laboratory  

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

through a National Institute of Justice (NIJ) grant administered by the Midwest Forensic Resource Centre (MFRC) in Ames, Iowa. The principal investigators were Terry Laber,...

78

New approaches for modeling type Ia supernovae  

E-Print Network [OSTI]

ich and J. Stein. On the thermonuclear runaway in Type IaSmall-Scale Stability of Thermonuclear Flames o in Type IaS. E. Woosley. The thermonuclear explosion of chandrasekhar

Zingale, Michael; Almgren, Ann S.; Bell, John B.; Day, Marcus S.; Rendleman, Charles A.; Woosley, Stan

2007-01-01T23:59:59.000Z

79

E-Print Network 3.0 - ames laboratory calendar Sample Search...  

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

309. 341abL Mechoptronics Laboratory I and II (3-3, Fa... for Design AME 309 Dynamics of Fluids AME 310 Engineering Thermodynamics I AME 341aL Mechoptronics Laboratory... I ......

80

Rare Earth Metals and Alloys | Ames Laboratory  

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

Mpc » Rare Earth Metals and Alloys Mpc » Rare Earth Metals and Alloys Rare Earth Metals and Alloys Terbium (Tb) and Cerium (Ce) phosphors in your computer screen allow you to see GREEN. Europium (Eu) is the source of the RED light and BLUE emitted by our display. The Ames Laboratory has been actively involved in the preparation of very pure rare earth metals since the early 1940's when Dr. Frank H. Spedding and his group of pioneers developed the ion-exchange process, a technique that separates the "fraternal fifteen" plus yttrium and scandium. As a result of this and subsequent work, high-purity oxides are available from which high-purity rare earth metals can be prepared. In most cases, the rare earth oxides are first converted to their respective fluorides and are then reduced metallothermicaly on a kilogram

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Abstract IA37: Clinical genomics  

Science Journals Connector (OSTI)

...Research. 15 October 2014 meeting-abstract Clinical Genomics Clinical Genomics: Oral Presentations - Invited Abstracts Abstracts...2013; San Diego, CA Abstract IA37: Clinical genomics Katherine A. Janeway Dana-Farber Cancer Institute...

Katherine A. Janeway

2014-10-15T23:59:59.000Z

82

Ames Electric Department - Residential Energy Efficiency Rebate Programs |  

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

Ames Electric Department - Residential Energy Efficiency Rebate Ames Electric Department - Residential Energy Efficiency Rebate Programs Ames Electric Department - Residential Energy Efficiency Rebate Programs < Back Eligibility Multi-Family Residential Residential Savings Category Heating & Cooling Commercial Heating & Cooling Cooling Appliances & Electronics Home Weatherization Construction Commercial Weatherization Design & Remodeling Heat Pumps Commercial Lighting Lighting Maximum Rebate Appliances: 50% of the equipment cost Programmable Thermostats: 3 per household Room AC: 2 per household Program Info State Iowa Program Type Utility Rebate Program Rebate Amount Energy Star New Home: $500 Energy Audit: FREE Lighting: $2 - $16 per fixture Lighting Sensors: $10 per unit Refrigerators: $25 - $100 Freezers: $50 Dishwashers: $50

83

Ames Laboratory Scientist Receives Award for Advancing Diversity...  

Energy Savers [EERE]

the Ames Laboratory SULI program. I also partnered with colleagues Steve Karsjen, Emily Smith and Malika Jeffries-EL to be the first mentors in the a Visiting Faculty Program (VFP)...

84

Ames Laboratory 3D printing technology research taking shape...  

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

3D printing technology research taking shape Insider Scientists at the U.S. Department of Energy's Ames Laboratory see amazing potential in 3D printing and additive manufacturing,...

85

Learning the language of cell life: Ames Laboratory scientists...  

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

to know how plants and microbes in the soil talk to each other," said Marit Nilsen-Hamilton, an Ames Laboratory scientist and professor in the Roy J Carver Department of...

86

Ames Lab 101: Real-Time 3D Imaging  

ScienceCinema (OSTI)

Ames Laboratory scientist Song Zhang explains his real-time 3-D imaging technology. The technique can be used to create high-resolution, real-time, precise, 3-D images for use in healthcare, security, and entertainment applications.

Zhang, Song

2012-08-29T23:59:59.000Z

87

Labs at-a-Glance: Ames Laboratory | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames Laboratory Ames Laboratory Laboratories Ames Laboratory Argonne National Laboratory Brookhaven National Laboratory Fermi National Accelerator Laboratory Lawrence Berkeley National Laboratory Oak Ridge National Laboratory Pacific Northwest National Laboratory Princeton Plasma Physics Laboratory SLAC National Accelerator Laboratory Thomas Jefferson National Accelerator Facility Laboratory Policy and Evaluation Safety, Security and Infrastructure Laboratory Science Highlights Contact Information Office of Science U.S. Department of Energy 1000 Independence Ave., SW Washington, DC 20585 P: (202) 586-5430 Labs at-a-Glance: Ames Laboratory Print Text Size: A A A RSS Feeds FeedbackShare Page Ames Laboratory Logo Visit the Ames Laboratory website External link Ames Laboratory Quick Facts

88

String Landscape and Supernovae Ia  

E-Print Network [OSTI]

We present a model for the triggering of Supernovae Ia (SN Ia) by a phase transition to exact supersymmetry (susy) in the core of a white dwarf star. The model, which accomodates the data on SN Ia and avoids the problems of the standard astrophysical accretion based picture, is based on string landscape ideas and assumes that the decay of the false broken susy vacuum is enhanced at high density. In a slowly expanding susy bubble, the conversion of pairs of fermions to pairs of degenerate scalars releases a significant amount of energy which induces fusion in the surrounding normal matter shell. After cooling, the absence of degeneracy pressure causes the susy bubble to collapse to a black hole of about 0.1 solar mass or to some other stable susy object.

L. Clavelli

2011-10-09T23:59:59.000Z

89

Ames Site Office Homepage | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Home Home Ames Site Office (AMSO) AMSO Home About Current Projects Contract Management Environment, Safety and Health (ES&H) Resources Contact Information Ames Site Office U.S. Department of Energy 9800 S. Cass Avenue Argonne, IL 60439 P: (630) 252-6167 F: (630) 252-2855 Ames Site Office Pictured Right: Ames Laboratory Ames Laboratory 1 of 2 Print Text Size: A A A RSS Feeds FeedbackShare Page The Ames Site Office (AMSO) is an organization within the U.S. Department of Energy's Office of Science with responsibility to oversee and manage the Management and Operating (M&O) contract for the Ames Laboratory in Ames, Iowa. Ames Laboratory is one of ten Office of Science Laboratories and is a single program laboratory with a primary mission on delivering breakthrough science and technology in the area of Basic Energy Sciences. The AMSO is

90

Ames Electric Department - Commercial Energy Efficiency Rebate Programs |  

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

Ames Electric Department - Commercial Energy Efficiency Rebate Ames Electric Department - Commercial Energy Efficiency Rebate Programs Ames Electric Department - Commercial Energy Efficiency Rebate Programs < Back Eligibility Commercial Industrial Savings Category Heating & Cooling Commercial Heating & Cooling Cooling Appliances & Electronics Other Heat Pumps Commercial Lighting Lighting Maximum Rebate Appliances: 50% of equipment cost per unit Lighting: Will not exceed equipment cost per unit, (contact AED about incentives expected to exceed $10,000) Power Factor Correction Equipment: Incentives over $15,000 will be examined on case by case basis Custom Rebate: Incentives over $15,000 willexamined on case by case basis Program Info State Iowa Program Type Utility Rebate Program Rebate Amount Refrigerators: $25 - $100

91

Ames Laboratory site environmental report, calendar year 1995  

SciTech Connect (OSTI)

This report summarizes the environmental status of Ames Laboratory for calendar year 1995. It includes descriptions of the Laboratory site, its mission, the status of its compliance with applicable environmental regulations, its planning and activities to maintain compliance, and a comprehensive review of its environmental protection, surveillance and monitoring programs.

NONE

1997-01-01T23:59:59.000Z

92

AME CURRICULUM GUIDE FALL 2014 AUDIO AND MUSIC ENGINEERING  

E-Print Network [OSTI]

, and software engineering. Through a series of design and project courses integrated with their other courseAME CURRICULUM GUIDE FALL 2014 AUDIO AND MUSIC ENGINEERING THE HAJIM SCHOOL OF ENGINEERING students a technically rigorous, design-based education in the field of audio, music and sonic engineering

93

Ethylene ame synthesis of well-aligned multi-walled carbon nanotubes  

E-Print Network [OSTI]

Ethylene ¯ame synthesis of well-aligned multi-walled carbon nanotubes Liming Yuan a , Kozo Saito a and curved shape multi-walled carbon nanotubes (MWNTs) were harvested from an ethylene±air diusion ¯ame applied to the nitrogen-diluted ethylene diusion ¯ame; well-aligned and well-graphitized carbon nanotubes

Chen, Zhi

94

Rapidly-Exploring Random Trees: Progress and Prospects Steven M. LaValle, Iowa State University, Ames, IA, USA  

E-Print Network [OSTI]

Rapidly-Exploring Random Trees: Progress and Prospects Steven M. LaValle, Iowa State University current progress on the design and analysis of path planning algorithms based on Rapidly- exploring Random to rapidly and uniformly explore the state space, o#11;ering bene#12;ts that are similar to those ob- tained

LaValle, Steven M.

95

Critical Materials and Rare Futures: Ames Laboratory Signs a New Agreement  

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

Critical Materials and Rare Futures: Ames Laboratory Signs a New Critical Materials and Rare Futures: Ames Laboratory Signs a New Agreement on Rare-Earth Research Critical Materials and Rare Futures: Ames Laboratory Signs a New Agreement on Rare-Earth Research June 15, 2011 - 7:07pm Addthis The plasma torch in the Retech plasma furnace is one tool used in Materials Preparation Center to create ultra-high purity metal alloy samples, particularly rare-earth metals, located at the Ames Lab. | Photo Courtesy of the Ames Lab Flickr The plasma torch in the Retech plasma furnace is one tool used in Materials Preparation Center to create ultra-high purity metal alloy samples, particularly rare-earth metals, located at the Ames Lab. | Photo Courtesy of the Ames Lab Flickr Charles Rousseaux Charles Rousseaux Senior Writer, Office of Science

96

Steamboat IA Geothermal Facility | Open Energy Information  

Open Energy Info (EERE)

IA Geothermal Facility IA Geothermal Facility Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Steamboat IA Geothermal Facility General Information Name Steamboat IA Geothermal Facility Facility Steamboat IA Sector Geothermal energy Location Information Location Washoe, Nevada Coordinates 40.5608387°, -119.6035495° 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":40.5608387,"lon":-119.6035495,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

97

Ames Laboratory scientists discover new family of quasicrystals | Argonne  

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

Science Science Computing, Environment & Life Sciences Energy Engineering & Systems Analysis Photon Sciences Physical Sciences & Engineering Energy Frontier Research Centers Science Highlights Postdoctoral Researchers Ames Laboratory scientists discover new family of quasicrystals July 16, 2013 Tweet EmailPrint Scientists at the U.S. Department of Energy's (DOE) Ames Laboratory have discovered a new family of rare-earth quasicrystals using an algorithm they developed to help pinpoint them. Quasicrystalline materials may be found close to crystalline phases that contain similar atomic motifs, called crystalline approximants. And just like fishing experts know that casting a line in the right habitat hooks the big catch, the scientists used their knowledge to hone in on just the right spot for new quasicrystal materials

98

Ames Laboratory Site Environmental Report, Calendar year 1991  

SciTech Connect (OSTI)

The summarized data and conclusions from the Ames Laboratory environmental monitoring program are presented in this Annual Site Environmental Report. This program is a working requirement of Department of Energy (DOE) Order 5484.1, ``Environmental Protection, Safety, and Health Protection Information Reporting Requirements`` and Order 5400.1, ``General Environmental Protection Program.`` Ames Laboratory is located on the campus of Iowa State University (ISU) and occupies several buildings owned by the DOE. The Laboratory also leases space in ISU-owned buildings. Laboratory research activities involve less than ten percent of the total chemical use and one percent of the radioisotope use on the ISU campus. Ames Laboratory is responsible for a small chemical burial site, located on ISU property. The site was used for the disposal of chemical and metal slags from thorium and uranium production. Samples of water from existing test wells and upstream and downstream sites on the nearby Squaw Creek show no detectable migration of the contents of the burial site. A Site Assessment plan submitted to the State of Iowa Department of Natural Resources (DNR) was approved. A Remedial Investigation/Feasibility Study work plan has been completed for additional studies at the site. This has been reviewed and approved by the DOE Chicago Field Office and the DNR. A National Environmental Policy Act (NEPA) review of the site resulted in a categorical exclusion finding which has been approved by the DOE. Ames Laboratory has an area contaminated by diesel fuel at the location of a storage tank which was removed in 1970. Soil corings and groundwater have been analyzed for contamination and an assessment written. Pollution awareness and waste minimization programs and plans were implemented in 1990. Included in this effort was the implementation of a waste white paper and green computer paper recycling program.

Mathison, L.

1991-12-31T23:59:59.000Z

99

Ames Laboratory annual site environmental report, calendar year 1996  

SciTech Connect (OSTI)

This report summarizes the environmental status of Ames Laboratory for calendar year 1996. It includes descriptions of the Laboratory site, its mission, the status of its compliance with applicable environmental regulations, its planning and activities to maintain compliance, and a comprehensive review of its environmental protection, surveillance and monitoring programs. Ames Laboratory is located on the campus of Iowa State University (ISU) and occupies twelve buildings owned by the Department of Energy (DOE). The Laboratory also leases space in ISU owned buildings. Laboratory activities involve less than ten percent of the total chemical use and approximately one percent of the radioisotope use on the ISU campus. In 1996, the Office of Assurance and Assessment merged with the Environment, Safety and Health Group forming the Environment, Safety, Health and Assurance (ESH and A) office. In 1996, the Laboratory accumulated and disposed of wastes under US Environmental Protection Agency (EPA) issued generator numbers. Ames Laboratory submitted a Proposed Site Treatment Plan to EPA in December 1995. This plan complied with the Federal Facilities Compliance Act (FFCA). It was approved by EPA in January 1996. The consent agreement/consent order was issued in February 1996. Pollution awareness, waste minimization and recycling programs, implemented in 1990 and updated in 1994, continued through 1996. Included in these efforts were a waste white paper and green computer paper recycling program. Ames Laboratory also continued to recycle salvageable metal and used oil, and it recovered freon for recycling. All of the chemical and nearly all of the radiological legacy wastes were properly disposed by the end of 1996. Additional radiological legacy waste will be properly disposed during 1997.

NONE

1998-04-01T23:59:59.000Z

100

THE LOCAL HOSTS OF TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1 Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of approx10{sup 10} M{sub sun}, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population. A low host extinction subsample hints at a residual trend in peak luminosity with host age, after correcting for light-curve shape, giving the appearance that older hosts produce less-extincted SNe Ia on average. This has implications for cosmological fitting of SNe Ia, and suggests that host age could be useful as a parameter in the fitting. Converting host mass to metallicity and computing {sup 56}Ni mass from the supernova light curves, we find that our local sample is consistent with a model that predicts a shallow trend between stellar metallicity and the {sup 56}Ni mass that powers the explosion, but we cannot rule out the absence of a trend. We measure a correlation between {sup 56}Ni mass and host age in the local universe that is shallower and not as significant as that seen at higher redshifts. The details of the age-{sup 56}Ni mass correlations at low and higher redshift imply a luminosity-weighted age threshold of approx3 Gyr for SN Ia hosts, above which they are less likely to produce SNe Ia with {sup 56}Ni masses above approx0.5 M{sub sun}.

Neill, James D.; Martin, D. Christopher; Barlow, Tom A.; Foster, Karl; Friedman, Peter G.; Morrissey, Patrick; Wyder, Ted K. [California Institute of Technology, 1200 E. California Blvd., Pasadena, CA 91125 (United States); Sullivan, Mark [University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH (United Kingdom); Howell, D. Andrew [Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117 (United States); Conley, Alex [Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ONM5S3H8 (Canada); Seibert, Mark; Madore, Barry F. [The Observatories of the Carnegie Institute of Washington, 813 Santa Barbara Street, Pasadena, CA, 91101 (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); Bianchi, Luciana [Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles St., 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. [Department of Physics and Astronomy, Johns Hopkins University, Homewood Campus, Baltimore, MD 21218 (United States); Lee, Young-Wook [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)

2009-12-20T23:59:59.000Z

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

NASA/Ames Global Emissions Data Set (GLEMIS) | Open Energy Information  

Open Energy Info (EERE)

NASA/Ames Global Emissions Data Set (GLEMIS) NASA/Ames Global Emissions Data Set (GLEMIS) Jump to: navigation, search Tool Summary LAUNCH TOOL Name: NASA/Ames Global Emissions Data Set (GLEMIS) Agency/Company /Organization: National Aeronautics and Space Administration Sector: Land Focus Area: Forestry, Agriculture Topics: GHG inventory Resource Type: Dataset, Maps Website: gcmd.nasa.gov/records/GCMD_NASA_AMES_GLEMIS.html NASA/Ames Global Emissions Data Set (GLEMIS) Screenshot References: NASA/Ames Global Emissions Data Set (GLEMIS)[1] "NASA-CASA data sets include global maps for predicted fluxes of soil nitrogen gases (N2O and NO), methane (CH4), and carbon monoxide (CO), plus predictions of net primary production (NPP) and carbon storage in leaf, wood, root, litter, and surface soil pools. Others data sets will follow.

102

Supersoft Sources as SN Ia Progenitors  

E-Print Network [OSTI]

of the existence of supersoft X­ray sources. It is argued that SNe Ia are thermonuclear explosions of accreting C is that they represent thermonuclear disruptions of mass accreting white dwarfs (WDs). Thus, the basic ingredient

Greiner, Jochen

103

ETODOS NUM ERICOS EN INGENIER IA  

E-Print Network [OSTI]

CONSERVATIVOS ENERG #19; IA-MOMENTO Jos#19;e M. Goicolea Ruig#19;omez y Juan Carlos Garc#19;#16;a Orden EscuelaM #19; ETODOS NUM #19; ERICOS EN INGENIER #19; IA R. Abascal, J. Dom#19;#16;nguez y G. Bugeda (Eds.upm.es Palabras clave: Din#19;amica no lineal, mecanismos, sistemas multicuerpo exibles, energ#19;#16;a- momento

Romero, Ignacio

104

E-Print Network 3.0 - ames test progress Sample Search Results  

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

Search Powered by Explorit Topic List Advanced Search Sample search results for: ames test progress Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and...

105

E-Print Network 3.0 - ames salmonella test Sample Search Results  

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

test Search Powered by Explorit Topic List Advanced Search Sample search results for: ames salmonella test Page: << < 1 2 3 4 5 > >> 1 Information for Veterinarians and Veterinary...

106

E-Print Network 3.0 - ames test communication Sample Search Results  

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

Search Powered by Explorit Topic List Advanced Search Sample search results for: ames test communication Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and...

107

Ames Site Office CX Determinations | U.S. DOE Office of Science...  

Office of Science (SC) Website

Ames Site Office CX Determinations Safety and Security Policy (SSP) SSP Home About Frequently Used Resources Categorical Exclusion Determinations Continuity of Operations (COOP)...

108

E-Print Network 3.0 - ames human resources Sample Search Results  

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

Agents Gregory Dorais... NASA Ames Research Center David Kortenkamp NASA Johnson Space Center ... Source: Kortenkamp, David - Texas Robotics and Automation Center...

109

Photo 3D-Printer, Image Credit, Ames Lab | OSTI, US Dept of Energy...  

Office of Scientific and Technical Information (OSTI)

Photo 3D-Printer, Image Credit, Ames Lab Critical Materials Institute speed metals research with 3D printer. Default Caption and Credits Read More: Critical Materials Institute...

110

E-Print Network 3.0 - ames laboratory research Sample Search...  

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

results for: ames laboratory research Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique, complex mechanical-optical- Summary: synthesizing...

111

E-Print Network 3.0 - ames research center Sample Search Results  

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

search results for: ames research center Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique, complex mechanical, optical, Summary: boundaries,...

112

E-Print Network 3.0 - ames collaborative study Sample Search...  

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

results for: ames collaborative study Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique, complex mechanical, optical, Summary: studies. No...

113

E-Print Network 3.0 - ames research library Sample Search Results  

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

search results for: ames research library Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique, complex mechanical-optical- Summary: synthesizing...

114

E-Print Network 3.0 - ames laboratory researchers Sample Search...  

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

results for: ames laboratory researchers Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique, complex mechanical-optical- Summary: synthesizing...

115

SBOT IOWA AMES LAB POC Lisa Rodgers Telephone  

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

IOWA IOWA AMES LAB POC Lisa Rodgers Telephone (515) 294-4191 Email rodgers@ameslab.gov GOODS Photographic Equipment and Supplies Merchant Wholesalers 423410 Computer and Computer Peripheral Equipment and Software Merchant Wholesalers 423430 Other Commercial Equipment Merchant Wholesalers 423440 Other Professional Equipment and Supplies Merchant Wholesalers 423490 Electrical Apparatus and Equipment, Wiring Supplies, and Related Equipment Merchant Wholesalers 423610 Electrical and Electronic Appliance, Television, and Radio Set Merchant Wholesalers 423620 Other Electronic Parts and Equipment Merchant Wholesalers 423690 Industrial Machinery and Equipment Merchant Wholesalers 423830 Industrial Supplies Merchant Wholesalers 423840 Other Miscellaneous Durable Goods Merchant Wholesalers

116

AME:NDMENT OF SOLICITATION/MODIFICATION OF CONTRACT  

National Nuclear Security Administration (NNSA)

AME:NDMENT OF SOLICITATION/MODIFICATION OF CONTRACT AME:NDMENT OF SOLICITATION/MODIFICATION OF CONTRACT 1. CONTRACT 10 CODE PAGE 1 OF 224 PAGES 2. AMENDMENT/MODIFICATION NO. M202 3. EFFECTIVE DATE October 1, 2003 4. REQUISITION/PURCHASE REQ. NO. 5. PROJECT NO. (If applicable) 6. ISSUED BY CODE 7. ADMINISTERED BY (If other than Item 6) CODE U.s. Department of Energy N.itional Nuclear Security Administration Sandia Site Office Mail Stop 0184 P.O. Box 5400 AlbuauerQue, NM 87185-5400 8. NAME AND ADDRESS OF CONTRACTOR (No., street, county, state, ZIP Code) 9A. AMENDMENT OF SOLICITATION NO. Sandia Corporation P. O. Box 5800 Albuquerque, NM 87185 98. DATED (SEE ITEM 11) 10A. MODIFICATION OF CONTRACT/ORDER NO. DE-ACO4-94AL85000 108. DATED (SEE ITEM 13) October 1, 1993 CODE II-ACIL~ CODE 11. THIS ITEM ONLY APPLIES TO AMENDMENTS OF SOLICITATIONS

117

Rolling Hills (IA) | Open Energy Information  

Open Energy Info (EERE)

Rolling Hills (IA) Rolling Hills (IA) Jump to: navigation, search Name Rolling Hills (IA) Facility Rolling Hills (IA) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner MidAmerican Energy Company Developer MidAmerican Energy Company Energy Purchaser MidAmerican Energy Company Location Massena IA Coordinates 41.230443°, -94.75459° 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":41.230443,"lon":-94.75459,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

118

Iowa Start-up Taps Ames Laboratory Technology in Challenge | Department of  

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

Taps Ames Laboratory Technology in Challenge Taps Ames Laboratory Technology in Challenge Iowa Start-up Taps Ames Laboratory Technology in Challenge August 10, 2011 - 2:21pm Addthis Using gas atomization technology developed at the Ames Lab (click through the photo to see a video), IPAT will be able to make titanium powder 10 times more efficiently than traditional powder-making methods. Above right, 1.8 grams of gas atomized titanium powder makes a finished 1.8 gram titanium bolt. | Image Courtesy of IPAT Using gas atomization technology developed at the Ames Lab (click through the photo to see a video), IPAT will be able to make titanium powder 10 times more efficiently than traditional powder-making methods. Above right, 1.8 grams of gas atomized titanium powder makes a finished 1.8 gram titanium bolt. | Image Courtesy of IPAT

119

A Statement from U.S. Secretary of Energy Ernest Moniz on New Leadership at Ames National Laboratory  

Broader source: Energy.gov [DOE]

This week, the Energy Department welcomes Dr. Adam Schwartz as the new director of Ames National Laboratory.

120

City of Ames, Iowa (Utility Company) | Open Energy Information  

Open Energy Info (EERE)

Iowa (Utility Company) Iowa (Utility Company) Jump to: navigation, search Name Ames City of Place Iowa Utility Id 554 Utility Location Yes Ownership M NERC Location MRO NERC MRO Yes ISO MISO Yes Operates Generating Plant Yes Activity Generation Yes Activity Transmission Yes Activity Buying Transmission Yes Activity Distribution Yes Activity Wholesale Marketing Yes Alt Fuel Vehicle Yes Alt Fuel Vehicle2 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 Industrial Rates Industrial Large Commercial Rates Commercial Residential Residential Small Commercial Rates Commercial Average Rates

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

A threat-based definition of IA and IA-enabled products.  

SciTech Connect (OSTI)

This paper proposes a definition of 'IA and IA-enabled products' based on threat, as opposed to 'security services' (i.e., 'confidentiality, authentication, integrity, access control or non-repudiation of data'), as provided by Department of Defense (DoD) Instruction 8500.2, 'Information Assurance (IA) Implementation.' The DoDI 8500.2 definition is too broad, making it difficult to distinguish products that need higher protection from those that do not. As a consequence the products that need higher protection do not receive it, increasing risk. The threat-based definition proposed in this paper solves those problems by focusing attention on threats, thereby moving beyond compliance to risk management. (DoDI 8500.2 provides the definitions and controls that form the basis for IA across the DoD.) Familiarity with 8500.2 is assumed.

Shakamuri, Mayuri; Schaefer, Mark A.; Campbell, Philip LaRoche

2010-09-01T23:59:59.000Z

122

A threat-based definition of IA- and IA-enabled products.  

SciTech Connect (OSTI)

This paper proposes a definition of 'IA and IA-enabled products' based on threat, as opposed to 'security services' (i.e., 'confidentiality, authentication, integrity, access control or non-repudiation of data'), as provided by Department of Defense (DoD) Instruction 8500.2, 'Information Assurance (IA) Implementation.' The DoDI 8500.2 definition is too broad, making it difficult to distinguish products that need higher protection from those that do not. As a consequence the products that need higher protection do not receive it, increasing risk. The threat-based definition proposed in this paper solves those problems by focusing attention on threats, thereby moving beyond compliance to risk management. (DoDI 8500.2 provides the definitions and controls that form the basis for IA across the DoD.) Familiarity with 8500.2 is assumed.

Shakamuri, Mayuri; Schaefer, Mark A.; Campbell, Philip LaRoche

2010-07-01T23:59:59.000Z

123

Comparison of Recent SnIa datasets  

E-Print Network [OSTI]

We rank the six latest Type Ia supernova (SnIa) datasets (Constitution (C), Union (U), ESSENCE (Davis) (E), Gold06 (G), SNLS 1yr (S) and SDSS-II (D)) in the context of the Chevalier-Polarski-Linder (CPL) parametrization $w(a)=w_0+w_1 (1-a)$, according to their Figure of Merit (FoM), their consistency with the cosmological constant ($\\Lambda$CDM), their consistency with standard rulers (Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillations (BAO)) and their mutual consistency. We find a significant improvement of the FoM (defined as the inverse area of the 95.4% parameter contour) with the number of SnIa of these datasets ((C) highest FoM, (U), (G), (D), (E), (S) lowest FoM). Standard rulers (CMB+BAO) have a better FoM by about a factor of 3, compared to the highest FoM SnIa dataset (C). We also find that the ranking sequence based on consistency with $\\Lambda$CDM is identical with the corresponding ranking based on consistency with standard rulers ((S) most consistent, (D), (C), (E), (U), (G) least consistent). The ranking sequence of the datasets however changes when we consider the consistency with an expansion history corresponding to evolving dark energy $(w_0,w_1)=(-1.4,2)$ crossing the phantom divide line $w=-1$ (it is practically reversed to (G), (U), (E), (S), (D), (C)). The SALT2 and MLCS2k2 fitters are also compared and some peculiar features of the SDSS-II dataset when standardized with the MLCS2k2 fitter are pointed out. Finally, we construct a statistic to estimate the internal consistency of a collection of SnIa datasets. We find that even though there is good consistency among most samples taken from the above datasets, this consistency decreases significantly when the Gold06 (G) dataset is included in the sample.

J. C. Bueno Sanchez; S. Nesseris; L. Perivolaropoulos

2009-10-01T23:59:59.000Z

124

After 15 Years, A New Top Earning Patent At Ames Lab | Department of Energy  

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

After 15 Years, A New Top Earning Patent At Ames Lab After 15 Years, A New Top Earning Patent At Ames Lab After 15 Years, A New Top Earning Patent At Ames Lab January 20, 2012 - 11:32am Addthis Ames Laboratory senior metallurgist Iver Anderson explains the importance of lead-free solder in taking hazardous lead out of the environment by eliminating it from discarded computers and electronics that wind up in landfills. Anderson led a team that developed a tin-silver-copper replacement for traditional lead solder that has been adopted by more than 50 companies worldwide and has generated more than $39 million in licensing income. Michael Hess Michael Hess Former Digital Communications Specialist, Office of Public Affairs What are the key facts? As of the end of June 2011, lead-free solder generated $38.9 million

125

Analysis of Hexanitrostilbene (HNS) and Dipicryethane (DPE) for Mutagenicity by the Ames/Salmonella Assay  

SciTech Connect (OSTI)

The Ames/Salmonella assay, developed by Professor Bruce Ames at the University of California, Berkeley, is a rapid and sensitive assay for detecting mutagenicity of various chemical compounds (Maron and Ames, 1983). It is a widely accepted short-term assay for detecting chemicals that induce mutations in the histidine (his) gene of Salmonella typhimurium. This is a reverse mutation assay that detects the mutational reversion of his-dependent Salmonella to the his-independent counterpart. Thereby, mutagenic compounds will increase the frequency of occurrence of his-independent bacterial colonies. The assay utilizes the specific genetically constructed strains of bacteria either with or without mammalian metabolic activation enzymes (S9), Aroclor induced rat liver homogenate to assess the mutagenicity of different compounds. In this study, we will use the Ames/Salmonella assay to investigate the mutagenicity of Hexanitrostilbene (HNS) from both Bofors and Pantex, and Dipicryethane (DPE).

Wu, R; Felton, J

2007-10-12T23:59:59.000Z

126

Instrument Development F.P.J. Valero P. Pilewskie NASA Ames Research...  

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

F.P.J. Valero P. Pilewskie NASA Ames Research Center Moffett Field, CA 94035-1000 Radiative proces,ses in the atmosphere are at the heart of anthropogenically induced climatic...

127

E-Print Network 3.0 - ames quantum laboratory Sample Search Results  

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

presentee devant Summary: at relativistic energies (100 AMeV Elab 2 AGeV) are the unique tool to study in the laboratory nucleonic systems... A moving source in the laboratory . ....

128

E-Print Network 3.0 - ames test mutagenicity Sample Search Results  

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

Search Powered by Explorit Topic List Advanced Search Sample search results for: ames test mutagenicity Page: << < 1 2 3 4 5 > >> 1 Mutation Research, 286 (1993) 75-100 75 1993...

129

E-Print Network 3.0 - ames test Sample Search Results  

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

Search Powered by Explorit Topic List Advanced Search Sample search results for: ames test Page: << < 1 2 3 4 5 > >> 1 Aerospace and Mechanical Engineers design and build unique,...

130

Making Stuff Outreach at the Ames Laboratory and Iowa State University  

SciTech Connect (OSTI)

The U. S. Department of Energy's Ames Laboratory in Ames, Iowa was a coalition partner for outreach activities connected with NOVA's Making Stuff television series on PBS. Volunteers affiliated with the Ames Laboratory and Iowa State University, with backgrounds in materials science, took part in activities including a science-themed Family Night at a local mall, Science Cafes at the Science Center of Iowa, teacher workshops, demonstrations at science nights in elementary and middle schools, and various other events. We describe a selection of the activities and present a summary of their outcomes and extent of their impact on Ames, Des Moines and the surrounding communities in Iowa. In Part 2, results of a volunteer attitude survey are presented, which shed some light on the volunteer experience and show how the volunteers participation in outreach activities has affected their views of materials education.

Ament, Katherine; Karsjen, Steven; Leshem-Ackerman, Adah; King, Alexander

2011-04-01T23:59:59.000Z

131

Category:Des Moines, IA | Open Energy Information  

Open Energy Info (EERE)

IA IA Jump to: navigation, search Go Back to PV Economics By Location Media in category "Des Moines, IA" The following 16 files are in this category, out of 16 total. SVFullServiceRestaurant Des Moines IA MidAmerican Energy Co (Iowa).png SVFullServiceRestauran... 64 KB SVQuickServiceRestaurant Des Moines IA MidAmerican Energy Co (Iowa).png SVQuickServiceRestaura... 64 KB SVHospital Des Moines IA MidAmerican Energy Co (Iowa).png SVHospital Des Moines ... 73 KB SVLargeHotel Des Moines IA MidAmerican Energy Co (Iowa).png SVLargeHotel Des Moine... 72 KB SVLargeOffice Des Moines IA MidAmerican Energy Co (Iowa).png SVLargeOffice Des Moin... 73 KB SVMediumOffice Des Moines IA MidAmerican Energy Co (Iowa).png SVMediumOffice Des Moi... 69 KB SVMidriseApartment Des Moines IA MidAmerican Energy Co (Iowa).png

132

DOE - Office of Legacy Management -- Bendix Aviation Corp Pioneer Div - IA  

Office of Legacy Management (LM)

Bendix Aviation Corp Pioneer Div - Bendix Aviation Corp Pioneer Div - IA 05 FUSRAP Considered Sites Site: BENDIX AVIATION CORP., PIONEER DIV. (IA.05 ) Eliminated from consideration under FUSRAP Designated Name: Not Designated Alternate Name: Pioneer Division, Bendix Aviation Corporation Bendix Aviation Corporation Bendix Pioneer Division IA.05-1 IA.05-2 IA.05-3 Location: Davenport , Iowa IA.05-1 Evaluation Year: 1990 IA.05-2 IA.05-4 Site Operations: Conducted studies to investigate the feasibility of using sonic cleaning equipment to decontaminate uranium contaminated drums. IA.05-1 Site Disposition: Eliminated - Potential for contamination considered remote based on limited operations at the site IA.05-2 IA.05-4 IA.05-5 Radioactive Materials Handled: Yes Primary Radioactive Materials Handled: Uranium IA.05-1

133

DOE - Office of Legacy Management -- Titus Metals - IA 04  

Office of Legacy Management (LM)

from consideration under FUSRAP Also see Documents Related to TITUS METALS IA.04-1 - Argonne National Laboratory Memorandum; Lonergan to Novak; Subject: Extrusion of Billets,...

134

Conformal cosmological model and SNe Ia data  

SciTech Connect (OSTI)

Now there is a huge scientific activity in astrophysical studies and cosmological ones in particular. Cosmology transforms from a pure theoretical branch of science into an observational one. All the cosmological models have to pass observational tests. The supernovae type Ia (SNe Ia) test is among the most important ones. If one applies the test to determine parameters of the standard Friedmann-Robertson-Walker cosmological model one can conclude that observations lead to the discovery of the dominance of the {Lambda} term and as a result to an acceleration of the Universe. However, there are big mysteries connected with an origin and an essence of dark matter (DM) and the {Lambda} term or dark energy (DE). Alternative theories of gravitation are treated as a possible solution of DM and DE puzzles. The conformal cosmological approach is one of possible alternatives to the standard {Lambda}CDM model. As it was noted several years ago, in the framework of the conformal cosmological approach an introduction of a rigid matter can explain observational data without {Lambda} term (or dark energy). We confirm the claim with much larger set of observational data.

Zakharov, A. F., E-mail: zakharov@itep.ru [National Astronomical Observatories of Chinese Academy of Sciences (China); Pervushin, V. N. [Joint Institute for Nuclear Research, Bogoliubov Laboratory for Theoretical Physics (Russian Federation)

2012-11-15T23:59:59.000Z

135

Type Ia Supernova Explosion: Gravitationally Confined Detonation  

Science Journals Connector (OSTI)

We present a new mechanism for Type Ia supernova explosions in massive white dwarfs. The scenario follows from relaxing assumptions of symmetry and involves a detonation born near the stellar surface. The explosion begins with an essentially central ignition of a deflagration that results in the formation of a buoyancy-driven bubble of hot material that reaches the stellar surface at supersonic speeds. The bubble breakout laterally accelerates fuel-rich outer stellar layers. This material, confined by gravity to the white dwarf, races along the stellar surface and is focused at the location opposite to the point of the bubble breakout. These streams of nuclear fuel carry enough mass and energy to trigger a detonation just above the stellar surface that will incinerate the white dwarf and result in an energetic explosion. The stellar expansion following the deflagration redistributes mass in a way that ensures production of intermediate-mass and iron group elements with ejecta having a strongly layered structure and a mild amount of asymmetry following from the early deflagration phase. This asymmetry, combined with the amount of stellar expansion determined by details of the evolution (principally the energetics of deflagration, timing of detonation, and structure of the progenitor), can be expected to create a family of mildly diverse Type Ia supernova explosions.

T. Plewa; A. C. Calder; D. Q. Lamb

2004-01-01T23:59:59.000Z

136

The distant type Ia supernova rate  

SciTech Connect (OSTI)

We present a measurement of the rate of distant Type Ia supernovae derived using 4 large subsets of data from the Supernova Cosmology Project. Within this fiducial sample,which surveyed about 12 square degrees, thirty-eight supernovae were detected at redshifts 0.25--0.85. In a spatially flat cosmological model consistent with the results obtained by the Supernova Cosmology Project, we derive a rest-frame Type Ia supernova rate at a mean red shift z {approx_equal} 0.55 of 1.53 {sub -0.25}{sub -0.31}{sup 0.28}{sup 0.32} x 10{sup -4} h{sup 3} Mpc{sup -3} yr{sup -1} or 0.58{sub -0.09}{sub -0.09}{sup +0.10}{sup +0.10} h{sup 2} SNu(1 SNu = 1 supernova per century per 10{sup 10} L{sub B}sun), where the first uncertainty is statistical and the second includes systematic effects. The dependence of the rate on the assumed cosmological parameters is studied and the redshift dependence of the rate per unit comoving volume is contrasted with local estimates in the context of possible cosmic star formation histories and progenitor models.

Pain, R.; Fabbro, S.; Sullivan, M.; Ellis, R.S.; Aldering, G.; Astier, P.; Deustua, S.E.; Fruchter, A.S.; Goldhaber, G.; Goobar, A.; Groom, D.E.; Hardin, D.; Hook, I.M.; Howell, D.A.; Irwin, M.J.; Kim, A.G.; Kim, M.Y.; Knop, R.A.; Lee, J.C.; Perlmutter, S.; Ruiz-Lapuente, P.; Schahmaneche, K.; Schaefer, B.; Walton, N.A.

2002-05-20T23:59:59.000Z

137

The Distant Type Ia Supernova Rate  

DOE R&D Accomplishments [OSTI]

We present a measurement of the rate of distant Type Ia supernovae derived using 4 large subsets of data from the Supernova Cosmology Project. Within this fiducial sample, which surveyed about 12 square degrees, thirty-eight supernovae were detected at redshifts 0.25--0.85. In a spatially flat cosmological model consistent with the results obtained by the Supernova Cosmology Project, we derive a rest-frame Type Ia supernova rate at a mean red shift z {approx_equal} 0.55 of 1.53 {sub -0.25}{sub -0.31}{sup 0.28}{sup 0.32} x 10{sup -4} h{sup 3} Mpc{sup -3} yr{sup -1} or 0.58{sub -0.09}{sub -0.09}{sup +0.10}{sup +0.10} h{sup 2} SNu(1 SNu = 1 supernova per century per 10{sup 10} L{sub B}sun), where the first uncertainty is statistical and the second includes systematic effects. The dependence of the rate on the assumed cosmological parameters is studied and the redshift dependence of the rate per unit comoving volume is contrasted with local estimates in the context of possible cosmic star formation histories and progenitor models.

Pain, R.; Fabbro, S.; Sullivan, M.; Ellis, R. S.; Aldering, G.; Astier, P.; Deustua, S. E.; Fruchter, A. S.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hardin, D.; Hook, I. M.; Howell, D. A.; Irwin, M. J.; Kim, A. G.; Kim, M. Y.; Knop, R. A.; Lee, J. C.; Perlmutter, S.; Ruiz-Lapuente, P.; Schahmaneche, K.; Schaefer, B.; Walton, N. A.

2002-05-28T23:59:59.000Z

138

Ames: Oct 1, 2010 - Sept 30, 2011 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2010 - Sept 30, 2011 Ames: Oct 1, 2010 - Sept 30, 2011 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards Ames: Oct 1, 2010 - Sept 30, 2011 Argonne: Oct 1, 2010 - Sept 30, 2011 BNL: Oct 1, 2010 - Sept 30, 2011 Fermilab: Oct 1, 2010 - Sept 30, 2011 LBNL: Oct 1, 2010 - Sept 30, 2011 ORNL: Oct 1, 2010 - Sept 30, 2011 PNNL: Oct 1, 2010 - Sept 30, 2011 PPPL: October 1, 2010 - September 30, 2011 SLAC: Oct 1, 2010 - Sept 30, 2011 JLab: Oct 1, 2010 - Sept 30, 2011 FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards

139

Ames: Oct 1, 2012 - Sept 30, 2013| U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2012 - Sept 30, 2013 Ames: Oct 1, 2012 - Sept 30, 2013 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards Ames: Oct 1, 2012 - Sept 30, 2013 Argonne: Oct 1, 2012 - Sept 30, 2013 BNL: Oct 1, 2012 - Sept 30, 2013 Fermilab: Oct 1, 2012 - Sept 30, 2013 LBNL: Oct 1, 2012 - Sept 30, 2013 ORNL: Oct 1, 2012 - Sept 30, 2013 PNNL: Oct 1, 2012 - Sept 30, 2013 PPPL: Oct 1, 2012 - Sept 30, 2013 SLAC: Oct 1, 2012 - Sept 30, 2013 JLab: Oct 1, 2012 - Sept 30, 2013 FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards FY 2007 SC Laboratory Performance Report Cards

140

Ames Site Office CX Determinations | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames Site Office CX Determinations Ames Site Office CX Determinations Integrated Support Center (ISC) ISC Home About Services Freedom of Information Act (FOIA) Privacy Act Categorical Exclusion Determinations Contact Information Integrated Support Center Roxanne Purucker U.S. Department of Energy 9800 S. Cass Avenue Argonne, IL 60439 P: (630) 252-2110 Larry Kelly U.S. Department of Energy 200 Administration Road Oak Ridge, TN 37830 P: (865) 576-0885 Categorical Exclusion (CX) Determinations Ames Site Office CX Determinations Print Text Size: A A A RSS Feeds FeedbackShare Page Categorical Exclusion Determination Documents (CX Determinations): * Determination Date Name of Action: Description Categorical Exclusion Number External link 07/10/2013 Sensitive Instrument Facility .pdf file (792KB) B3.6

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Ames: Jan 1, 2007 - Sept 30, 2007 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Jan 1, 2007 - Sept 30, 2007 Ames: Jan 1, 2007 - Sept 30, 2007 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards FY 2007 SC Laboratory Performance Report Cards Ames: Jan 1, 2007 - Sept 30, 2007 Argonne: Oct 1, 2006 - Sept 30, 2007 BNL: Oct 1, 2006 - Sept 30, 2007 Fermilab: Jan 1, 2007 - Sept 30, 2007 LBNL: Oct 1, 2006 - Sept 30, 2007 ORNL: Oct 1, 2006 - Sept 30, 2007 PNNL: Oct 1, 2006 - Sept 30, 2007 PPPL: Oct 1, 2006 - Sept 30, 2007 SLAC: Oct 1, 2006 - Sept 30, 2007

142

Ames: Oct 1, 2005 - Sept 30, 2006 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2005 - Sept 30, 2006 Ames: Oct 1, 2005 - Sept 30, 2006 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards FY 2007 SC Laboratory Performance Report Cards FY 2006 SC Laboratory Performance Report Cards Ames: Oct 1, 2005 - Sept 30, 2006 Argonne: Oct 1, 2005 - Sept 30, 2006 BNL: Oct 1, 2005 - Sept 30, 2006 Fermilab: Oct 1, 2005 - Sept 30, 2006 LBNL: Oct 1, 2005 - Sept 30, 2006 ORNL: Oct 1, 2005 - Sept 30, 2006 PNNL: Oct 1, 2005 - Sept 30, 2006 PPPL: Oct 1, 2005 - Sept 30, 2006

143

Ames: Oct 1, 2009 - Sept 30, 2010 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2009 - Sept 30, 2010 Ames: Oct 1, 2009 - Sept 30, 2010 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards Ames: Oct 1, 2009 - Sept 30, 2010 Argonne: Oct 1, 2009 - Sept 30, 2010 BNL: Oct 1, 2009 - Sept 30, 2010 Fermilab: Oct 1, 2009 - Sept 30, 2010 LBNL: Oct 1, 2009 - Sept 30, 2010 ORNL: Oct 1, 2009 - Sept 30, 2010 PNNL: Oct 1, 2009 - Sept 30, 2010 PPPL: October 1, 2009 - September 30, 2010 SLAC: Oct 1, 2009 - Sept 30, 2010 JLab: Oct 1, 2009 - Sept 30, 2010 FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards

144

Ames: Oct 1, 2007 - Sept 30, 2008 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2007 - Sept 30, 2008 Ames: Oct 1, 2007 - Sept 30, 2008 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards Ames: Oct 1, 2007 - Sept 30, 2008 Argonne: Oct 1, 2007 - Sept 30, 2008 BNL: Oct 1, 2007 - Sept 30, 2008 Fermilab: Oct 1, 2007 - Sept 30, 2008 JLab: Oct 1, 2007 - Sept 30, 2008 LBNL: Oct 1, 2007 - Sept 30, 2008 ORNL: Oct 1, 2007 - Sept 30, 2008 PNNL: Oct 1, 2007 - Sept 30, 2008 PPPL: Oct 1, 2007 - Sept 30, 2008 SLAC: Oct 1, 2007 - Sept 30, 2008 FY 2007 SC Laboratory Performance Report Cards

145

Ames: Oct 1, 2008 - Sept 30, 2009 | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2008 - Sept 30, 2009 Ames: Oct 1, 2008 - Sept 30, 2009 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards Ames: Oct 1, 2008 - Sept 30, 2009 Argonne: Oct 1, 2008 - Sept 30, 2009 BNL: Oct 1, 2008 - Sept 30, 2009 Fermilab: Oct 1, 2008 - Sept 30, 2009 LBNL: Oct 1, 2008 - Sept 30, 2009 ORNL: Oct 1, 2008 - Sept 30, 2009 PNNL: Oct 1, 2008 - Sept 30, 2009 PPPL: Apr 1, 2009 - Sept 30, 2009 SLAC: Oct 1, 2008 - Sept 30, 2009 JLab: Oct 1, 2008 - Sept 30, 2009 FY 2008 SC Laboratory Performance Report Cards FY 2007 SC Laboratory Performance Report Cards

146

Ames Site Office CX Determinations | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames Site Office CX Determinations Ames Site Office CX Determinations Safety, Security and Infrastructure (SSI) SSI Home Facilities and Infrastructure Safeguards & Security Environment, Safety and Health (ES&H) Organization Chart .pdf file (82KB) Phone Listing .pdf file (129KB) SC HQ Continuity of Operations (COOP) Implementation Plan .pdf file (307KB) Categorical Exclusion Determinations SLI & SS Budget Contact Information Safety, Security and Infrastructure U.S. Department of Energy SC-31/Germantown Building 1000 Independence Ave., SW Washington, DC 20585 P: (301) 903-4097 F: (301) 903-7047 Categorical Exclusion (CX) Determinations Ames Site Office CX Determinations Print Text Size: A A A RSS Feeds FeedbackShare Page Categorical Exclusion Determination Documents (CX Determinations): *

147

Ames: Oct 1, 2011 - Sept 30, 2012| U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Ames: Oct 1, 2011 - Sept 30, 2012 Ames: Oct 1, 2011 - Sept 30, 2012 Laboratory Policy and Evaluation (LPE) LPE Home Staff M&O Contracts SC Laboratory Appraisal Process FY 2013 SC Laboratory Performance Report Cards FY 2012 SC Laboratory Performance Report Cards Ames: Oct 1, 2011 - Sept 30, 2012 Argonne: Oct 1, 2011 - Sept 30, 2012 BNL: Oct 1, 2011 - Sept 30, 2012 Fermilab: Oct 1, 2011 - Sept 30, 2012 LBNL: Oct 1, 2011 - Sept 30, 2012 ORNL: Oct 1, 2011 - Sept 30, 2012 PNNL: Oct 1, 2011 - Sept 30, 2012 PPPL: Oct 1, 2011 - Sept 30, 2012 SLAC: Oct 1, 2011 - Sept 30, 2012 JLab: Oct 1, 2011 - Sept 30, 2012 FY 2011 SC Laboratory Performance Report Cards FY 2010 SC Laboratory Performance Report Cards FY 2009 SC Laboratory Performance Report Cards FY 2008 SC Laboratory Performance Report Cards FY 2007 SC Laboratory Performance Report Cards

148

Ames Laboratory to Lead New Research Effort to Address Shortages in Rare  

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

Laboratory to Lead New Research Effort to Address Shortages in Laboratory to Lead New Research Effort to Address Shortages in Rare Earth and Other Critical Materials Ames Laboratory to Lead New Research Effort to Address Shortages in Rare Earth and Other Critical Materials January 9, 2013 - 12:13pm Addthis NEWS MEDIA CONTACT (202) 586-4940 WASHINGTON - The U.S. Department of Energy announced today that a team led by Ames Laboratory in Ames, Iowa, has been selected for an award of up to $120 million over five years to establish an Energy Innovation Hub that will develop solutions to the domestic shortages of rare earth metals and other materials critical for U.S. energy security. The new research center, which will be named the Critical Materials Institute (CMI), will bring together leading researchers from academia, four Department of Energy

149

NASA Ames Saves Energy and Reduces Project Costs with Non-Invasive Retrofit Technologies  

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

NASA Ames Saves Energy and Reduces Project Costs NASA Ames Saves Energy and Reduces Project Costs with Non-Invasive Retrofit Technologies The Wireless Pneumatic Thermostat Enables Energy Efficiency Strategies, Ongoing Commissioning and Improved Operational Control Harry Sim CEO Cypress Envirosystems harry.sim@cypressenvirosystems.com www.cypressenvirosystems.com NASA Ames Reduced Project Cost by Over 80% with Non-Invasive Retrofit Technologies * Legacy Pneumatic Thermostats  Waste energy  High maintenance costs  Uncomfortable occupants  No visibility * Project Scope  14 buildings  1,370 pneumatic thermostats  Integration with campus BAS  Diagnostics for ongoing commissioning * Traditional DDC Retrofit  Cost over $4.1 million  Asbestos exposure/abatement  Occupants significantly disrupted

150

Intermediate-band Photometry of Type Ia Supernovae  

E-Print Network [OSTI]

We present optical light curves of five Type Ia supernovae (2002er, 2002fk, 2003cg, 2003du, 2003fk). The photometric observations were performed in a set of intermediate-band filters. SNe 2002er, 2003du appear to be normal SN Ia events with similar light curve shapes, while SN 2003kf shows the behavior of a brighter SN Ia with slower decline rate after maximum. The light curves of SN 2003cg is unusual; they show a fast rise and dramatic decline near maximum and do not display secondary peak at longer wavelengths during 15-30 days after maximum light. This suggests that SN 2003cg is likely to be an intrinsically subluminous, 91bg-like SN Ia. Exploration of SN Ia feature lines through intermediate-band photometry is briefly discussed.

Wang, X; Zhang, T; Li, Z; Wang, Xiaofeng; Zhou, Xu; Zhang, Tianmeng; Li, Zongwei

2004-01-01T23:59:59.000Z

151

9Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Human-Centered  

E-Print Network [OSTI]

9Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center-based Reasoning Related WorkRelated Work #12;10Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Autonomous Control SystemsAutonomous Control Systems l Brings to table

Kortenkamp, David

152

National Aeronautics and Space Administration,Ames Research Center,Moffett Field,CA www.nasa.gov  

E-Print Network [OSTI]

National Aeronautics and Space Administration,Ames Research Center,Moffett Field,CA July 2008 www Conference held in July at the center. developed at Ames and satellite data from Goddard Space Flight Center to heighten awareness of center management's concern for security at the center. Computer programs

153

Visualizing Type Ia Supernova Explosions at NERSC  

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

Supernova Explosions Supernova Explosions Visualizing Type Ia Supernova Explosions Childs1a-Supernovasm.png Deep inside a dying star in a galaxy far, far away, a carbon fusion flame ignites. Ignition may happen in the middle or displaced slightly to one side, but this simulation explores the consequences of central ignition. In a localized hot spot, represented here by a deformed sphere with an average radius of 100 km, carbon is assumed to have already fused to iron, producing hot ash (~10 billion K) with a density about 20% less than its surroundings. As the burning progresses, this hot buoyant ash rises up and interacts with cold fuel. Rayleigh-Taylor fingers give rise to shear and turbulence, which interacts with the flame, causing it to move faster. In about 2 seconds, the energy released blows the entire white dwarf star up,

154

Published in 2009 by John Wiley & Sons, Ltd Correspondence to: David A. Laird, USDA, ARS, National Soil Tilth Laboratory, 2110 University Blvd., Ames IA 50011-3120, USA.  

E-Print Network [OSTI]

quantities of renewable bioenergy while simultaneously reducing emissions of greenhouse gases. At the present time, the pyrolysis platform is economically marginal because markets for bio-oil and biochar bioenergy industry has been promoted as a means of simultaneously improving energy secu- rity, improving

Lehmann, Johannes

155

Hybrid Geometric Reduction of Hybrid Systems Aaron D. Ames and Shankar Sastry  

E-Print Network [OSTI]

Hybrid Geometric Reduction of Hybrid Systems Aaron D. Ames and Shankar Sastry Abstract-- This paper presents a unifying framework in which to carry out the hybrid geometric reduction of hybrid systems, generalizing classical reduction to a hybrid setting. I. INTRODUCTION The reduction of mechanical systems

Sastry, S. Shankar

156

SCHOOLING AND PARENTAL DEATH Paul Gertler, David I. Levine, and Minnie Ames*  

E-Print Network [OSTI]

nations have always lost parents to accidents, childbirth, and illness. Unfortunately, the scourge of HIV African children under the age of 15 has lost one or both parents (Hunter & Williamson, 2000SCHOOLING AND PARENTAL DEATH Paul Gertler, David I. Levine, and Minnie Ames* Abstract

Sadoulet, Elisabeth

157

Combined Simple Biosphere/Carnegie-Ames-Stanford Approach terrestrial carbon cycle model  

E-Print Network [OSTI]

Combined Simple Biosphere/Carnegie-Ames-Stanford Approach terrestrial carbon cycle model Kevin and physical processes to test our understanding of the terrestrial carbon cycle and to predict ecosystem biomass and carbon fluxes. We combine the photosynthesis and biophysical calculations in the Simple

Collett Jr., Jeffrey L.

158

High-resolution fracture aperture mapping using optical profilometry Pasha Ameli,1  

E-Print Network [OSTI]

High-resolution fracture aperture mapping using optical profilometry Pasha Ameli,1 Jean E. Elkhoury] Fractures play an important role in the Earth's crust, often controlling both mechanical and transport of fracture surfaces and the contacts and void spaces between fracture surfaces at high spatial resolution (10

Elkhoury, Jean

159

DOE - Office of Legacy Management -- Iowa Army Ammunition Plant - IA 02  

Office of Legacy Management (LM)

Army Ammunition Plant - IA 02 Army Ammunition Plant - IA 02 FUSRAP Considered Sites Iowa Army Ammunition Plant, IA Alternate Name(s): Burlington Ordnance Plant Iowa Ordnance Plant Silas Mason Company IA.02-3 Location: Located in Township 70 North, Range 3 West, Section 32, 5th Principal Meridian, Des Moines County, Burlington, Iowa IA.02-1 IA.02-5 Historical Operations: Assembled nuclear weapons, primarily high explosive components and conducted explosives testing using the high explosive components and depleted uranium. AEC and ERDA operations conducted under permit from the Department of the Army. IA.02-3 IA.02-4 Eligibility Determination: Eligible IA.02-5 Radiological Survey(s): Assessment Survey IA.02-2 Site Status: Cleanup pending by U.S. Army Corps of Engineers. IA.02-6

160

21Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Design of AA systemsDesign of AA systems  

E-Print Network [OSTI]

21Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center in autonomy #12;22Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Generic control system

Kortenkamp, David

Note: This page contains sample records for the topic "ames ia 630-252-3721" from the National Library of EnergyBeta (NLEBeta).
While these samples are representative of the content of NLEBeta,
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We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


161

Tracked Flame Simulation for Type Ia Yongmin Zhang1  

E-Print Network [OSTI]

tracking of the ame front which is critically important to the accurate modeling of turbulent thermonuclear, and the strength and brightness of the burning are all determined by the speed of thermonuclear burning 12, 13 needs to model the propagation of thermonuclear burning inside the exploding star. The mech- anism

New York at Stoney Brook, State University of

162

UMore Ph IA CR Report 7-8-10.pdf  

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

PHASE IA ARCHAEOLOGICAL AND PHASE IA ARCHAEOLOGICAL AND ARCHITECTURAL HISTORY SURVEY FOR THE UMORE PARK RESEARCH WIND TURBINE PROJECT, DAKOTA COUNTY, MINNESOTA SHPO File No. Pending Client No. Pending The 106 Group Project No. 10-18 Submitted to: Barr Engineering Company 4700 West 77th Street Minneapolis, MN 55435-4803 Submitted by: The 106 Group Ltd. The Dacotah Building 370 Selby Avenue St. Paul, MN 55102 Principal Investigators: AnneKetz, M.A., RPA Greg Mathis, M.C.R.P. Report Authors: Mark Doperalski, B.S. Miranda Van Vleet, M.H.P July 2010 UMore Park Wind Turbine Project Phase IA Archaeological and Architectural History Survey Page i MANAGEMENT SUMMARY During May of 2010, The 106 Group Ltd. (106 Group) conducted a Phase IA archaeological and architectural history survey for the University of Minnesota Outreach, Research, and

163

CIRCUMSTELLAR ABSORPTION IN DOUBLE DETONATION TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

Upon formation, degenerate He core white dwarfs are surrounded by a radiative H-rich layer primarily supported by ideal gas pressure. In this Letter, we examine the effect of this H-rich layer on mass transfer in He+C/O double white dwarf binaries that will eventually merge and possibly yield a Type Ia supernova (SN Ia) in the double detonation scenario. Because its thermal profile and equation of state differ from the underlying He core, the H-rich layer is transferred stably onto the C/O white dwarf prior to the He core's tidal disruption. We find that this material is ejected from the binary system and sweeps up the surrounding interstellar medium hundreds to thousands of years before the SN Ia. The close match between the resulting circumstellar medium profiles and values inferred from recent observations of circumstellar absorption in SNe Ia gives further credence to the resurgent double detonation scenario.

Shen, Ken J. [Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720 (United States); Guillochon, James [Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States); Foley, Ryan J., E-mail: kenshen@astro.berkeley.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States)

2013-06-20T23:59:59.000Z

164

Abstract IA14: Functional genomics and cancer vulnerabilities  

Science Journals Connector (OSTI)

...Cancer Research. November 2014 meeting-abstract Genomics Genomics: Oral Presentations - Invited Abstracts Abstracts...2013; San Diego, CA Abstract IA14: Functional genomics and cancer vulnerabilities William C. Hahn Dana-Farber...

William C. Hahn

2014-11-01T23:59:59.000Z

165

EARLY EMISSION FROM TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

A unique feature of deflagration-to-detonation (DDT) white dwarf explosion models of supernovae of type Ia is the presence of a strong shock wave propagating through the outer envelope. We consider the early emission expected in such models, which is produced by the expanding shock-heated outer part of the ejecta and precedes the emission driven by radioactive decay. We expand on earlier analyses by considering the modification of the pre-detonation density profile by the weak shocks generated during the deflagration phase, the time evolution of the opacity, and the deviation of the post-shock equation of state from that obtained for radiation pressure domination. A simple analytic model is presented and shown to provide an acceptable approximation to the results of one-dimensional numerical DDT simulations. Our analysis predicts a {approx}10{sup 3} s long UV/optical flash with a luminosity of {approx}1 to {approx}3 Multiplication-Sign 10{sup 39} erg s{sup -1}. Lower luminosity corresponds to faster (turbulent) deflagration velocity. The luminosity of the UV flash is predicted to be strongly suppressed at t > t{sub drop} {approx} 1 hr due to the deviation from pure radiation domination.

Rabinak, Itay; Waxman, Eli [Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 76100 (Israel); Livne, Eli, E-mail: itay.rabinak@weizmann.ac.il [Racah Institute of Physics, Hebrew University, Jerusalem (Israel)

2012-09-20T23:59:59.000Z

166

The 1.05-?m feature in the spectrum of the Type Ia supernova 1994D: He in SNe Ia?  

Science Journals Connector (OSTI)

......SNe Ia). Although the agreed basic scenario is thermonuclear fusion within a white dwarf (WD), the process leading...a pressure wave into the WD which then triggers thermonuclear fusion in the core. In this scenario, explosion can......

P. A. Mazzali; L. B. Lucy

1998-04-01T23:59:59.000Z

167

Simulations of Turbulent Thermonuclear Burning in Type Ia Supernovae  

E-Print Network [OSTI]

Type Ia supernovae have recently received considerable attention because it appears that they can be used as "standard candles" to measure cosmic distances out to billions of light years away from us. Observations of type Ia supernovae seem to indicate that we are living in a universe that started to accelerate its expansion when it was about half its present age. These conclusions rest primarily on phenomenological models which, however, lack proper theoretical understanding, mainly because the explosion process, initiated by thermonuclear fusion of carbon and oxygen into heavier elements, is difficult to simulate even on supercomputers. Here, we investigate a new way of modeling turbulent thermonuclear deflagration fronts in white dwarfs undergoing a type Ia supernova explosion. Our approach is based on a level set method which treats the front as a mathematical discontinuity and allows for full coupling between the front geometry and the flow field. New results of the method applied to the problem of type Ia supernovae are obtained. It is shown that in 2-D with high spatial resolution and a physically motivated subgrid scale model for the nuclear flames numerically "converged" results can be obtained, but for most initial conditions the stars do not explode. In contrast, simulations in 3-D, do give the desired explosions and many of their properties, such as the explosion energies, lightcurves and nucleosynthesis products, are in very good agreement with observed type Ia supernovae.

W. Hillebrandt; M. Reinecke; W. Schmidt; F. K. Roepke; C. Travaglio; J. C. Niemeyer

2004-05-11T23:59:59.000Z

168

Type Ia Supernovae Yielding Distances with 3-4% Precision  

E-Print Network [OSTI]

The luminosities of Type Ia supernovae (SN), the thermonuclear explosions of white dwarf stars, vary systematically with their intrinsic color and light-curve decline rate. These relationships have been used to calibrate their luminosities to within ~0.14-0.20 mag from broadband optical light curves, yielding individual distances accurate to ~7-10%. Here we identify a subset of SN Ia that erupt in environments having high ultraviolet surface brightness and star-formation surface density. When we apply a steep model extinction law, these SN can be calibrated to within ~0.065-0.075 mag, corresponding to ~3-4% in distance -- the best yet with SN Ia by a substantial margin. The small scatter suggests that variations in only one or two progenitor properties account for their light-curve-width/color/luminosity relation.

Kelly, Patrick L; Burke, David L; Hicken, Malcolm; Ganeshalingam, Mohan; Zheng, Weikang

2014-01-01T23:59:59.000Z

169

Signatures of A Companion Star in Type Ia Supernovae  

E-Print Network [OSTI]

While type Ia Supernovae (SNe Ia) have been used as precise cosmological distance indicators, their progenitor systems remain unresolved. One of the key questions is if there is a non-degenerate companion star at the time of a thermonuclear explosion of a white dwarf (WD). In this paper, we investigate if an interaction between the SN ejecta and the companion star may result in observable footprints around the maximum brightness and thereafter, by performing multi-dimensional radiation transfer simulations based on hydrodynamic simulations of the interaction. We find that such systems result in variations in various observational characteristics due to different viewing directions, while the predicted behaviors (redder and fainter for the companion direction) are opposite to what were suggested by the previous study. The variations are generally modest and within observed scatters. However, the model predicts trends between some observables different from observationally derived, thus a large sample of SNe Ia...

Maeda, Keiichi; Shigeyama, Toshikazu

2014-01-01T23:59:59.000Z

170

Double degenerates and progenitors of supernovae type Ia  

E-Print Network [OSTI]

We report on systematic radial velocity surveys for white dwarf - white dwarf binaries (double degenerates - DDs) including SPY (ESO Supernovae Ia progenitor survey) recently carried out at the VLT. A large sample of DD will allow us to put strong constrains on the phases of close binary evolution of the progenitor systems and to perform an observational test of the DD scenario for supernovae of type Ia. We explain how parameters of the binaries can be derived from various methods. Results for a sample of DDs are presented and discussed.

R. Napiwotzki; L. Yungelson; G. Nelemans; T. R. Marsh; B. Leibundgut; A. Renzini; D. Homaier; D. Koester; S. Moehler; N. Christlieb; D. Reimers; H. Drechsel; U. Heber; C. Karl; E. -M. Pauli

2004-03-25T23:59:59.000Z

171

Audit of Acquisition of Scientific Research at Ames Laboratory, ER-B-95-05  

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

S. DEPARTMENT OF ENERGY S. DEPARTMENT OF ENERGY OFFICE OF INSPECTOR GENERAL REPORT ON AUDIT OF ACQUISITION OF SCIENTIFIC RESEARCH AT AMES LABORATORY The Office of Inspector General wants to make the distribution of its reports as customer friendly and cost effective as possible. Therefore, this report will be available electronically through the Internet five to seven days after publication at the following alternative addresses: Department of Energy Headquarters Gopher gopher.hr.doe.gov Department of Energy Headquarters Anonymous FTP vm1.hqadmin.doe.gov U.S. Department of Energy Human Resources and Administration

172

Search for double degenerate progenitors of supernovae type Ia with SPY  

E-Print Network [OSTI]

We report on a large survey for double degenerate (DD) binaries as potential progenitors of type Ia supernovae with the UVES spectrograph at the ESO VLT (ESO SN Ia Progenitor surveY - SPY).

R. Napiwotzki; H. Drechsel; U. Heber; C. Karl; E. -M. Pauli; N. Christlieb; H. -J. Hagen; D. Reimers; D. Koester; S. Moehler; D. Homeier; B. Leibundgut; A. Renzini; T. R. Marsh; G. Nelemans; L. Yungelson

2002-10-07T23:59:59.000Z

173

Spectral Observations and Analyses of Low-Redshift Type Ia Supernovae  

E-Print Network [OSTI]

1.3.2 Thermonuclear Supernovae . . . . . . . . 1.4 Why WriteIa are the result of thermonuclear explosions of C/O whiteIa are the result of thermonuclear explosions of C/O white

Silverman, Jeffrey Michael

2011-01-01T23:59:59.000Z

174

INDECOMPOSABLE RACKS OF ORDER p 2 MAT IAS GRA  

E-Print Network [OSTI]

INDECOMPOSABLE RACKS OF ORDER p 2 MAT ?? IAS GRA ? NA Abstract. We classify indecomposable racks order is trivial. 1. Introduction Racks and quandles have been considered by G. Wraith and J. Conway categories, one is immediately led to the notion of a rack. On the other hand, in [ESS, EGS, S] and [LYZ1

Graña, Matías

175

INCOMPLETE CARBON-OXYGEN DETONATION IN TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

Incomplete carbon-oxygen detonation with reactions terminating after burning of C{sup 12} in the leading C{sup 12} + C{sup 12} reaction (C-detonation) may occur in the low-density outer layers of white dwarfs exploding as Type Ia supernovae (SNe Ia). Previous studies of carbon-oxygen detonation structure and stability at low densities were performed under the assumption that the velocity of a detonation wave is derived from complete burning of carbon and oxygen to iron. In fact, at densities {rho} {<=} 10{sup 6} g cm{sup -3} the detonation in SNe Ia may release less than a half of the available nuclear energy. In this paper, we study basic properties of such detonations. We find that the length of an unsupported steady-state C-detonation is {approx_equal}30-100 times greater than previously estimated and that the decreased energy has a drastic effect on the detonation stability. In contrast to complete detonations which are one-dimensionally stable, C-detonations may be one-dimensionally unstable and propagate by periodically re-igniting themselves via spontaneous burning. The re-ignition period at {rho} {<=} 10{sup 6} g cm{sup -3} is estimated to be greater than the timescale of an SN Ia explosion. This suggests that propagation and quenching of C-detonations at these densities could be affected by the instability. Potential observational implications of this effect are discussed.

Dominguez, Inma [Departamento de Fisica Teorica y del Cosmos, University of Granada, 18071 Granada (Spain); Khokhlov, Alexei [Department of Astronomy and Astrophysics and the Enrico Fermi Institute, University of Chicago, Chicago, IL 60637 (United States)

2011-04-01T23:59:59.000Z

176

The EqIA Publishing Template Impact Assessment Summary  

E-Print Network [OSTI]

The EqIA Publishing Template Impact Assessment Summary 1. Name of policy, function or service. Bedgebury 5 year strategy and development plan. This is a partial assessment. 2. Purpose and aims with ETWF: Sustainable Resource, Climate Change, Natural Environment, Quality of Life, Business and Markets

177

HOSPITALITY AND TOURISM MANAGEMENT MAJOR Virgu1iaTech  

E-Print Network [OSTI]

Hospitality Facilities Planning and Methods I (3) Management (3) #HTM 3484 Socio-Cultural Impacts of Tourism 4414 Food and Beverage Management (Pre: HTM 3414) * #HTM 4464 Human Resources Management in HospHOSPITALITY AND TOURISM MANAGEMENT MAJOR Virgu1iaTech Panplil College of BusIness Department

Virginia Tech

178

Circumstellar interaction of the type Ia supernova 2002ic  

Science Journals Connector (OSTI)

......with arguments in favour of a high-energy SN Ia event in this case, raises...WD explosion with a high kinetic energy of ejecta. The SN 1.5 origin of...2002ic-like events requires an accurate energy audit, for which the direct detection......

N. N. Chugai; R. A. Chevalier; P. Lundqvist

2004-12-01T23:59:59.000Z

179

Thermonuclear supernova models, and observations of Type Ia supernovae  

E-Print Network [OSTI]

In this paper, we review the present state of theoretical models of thermonuclear supernovae, and compare their predicitions with the constraints derived from observations of Type Ia supernovae. The diversity of explosion mechanisms usually found in one-dimensional simulations is a direct consequence of the impossibility to resolve the flame structure under the assumption of spherical symmetry. Spherically symmetric models have been successful in explaining many of the observational features of Type Ia supernovae, but they rely on two kinds of empirical models: one that describes the behaviour of the flame on the scales unresolved by the code, and another that takes account of the evolution of the flame shape. In contrast, three-dimensional simulations are able to compute the flame shape in a self-consistent way, but they still need a model for the propagation of the flame in the scales unresolved by the code. Furthermore, in three dimensions the number of degrees of freedom of the initial configuration of the white dwarf at runaway is much larger than in one dimension. Recent simulations have shown that the sensitivity of the explosion output to the initial conditions can be extremely large. New paradigms of thermonuclear supernovae have emerged from this situation, as the Pulsating Reverse Detonation. The resolution of all these issues must rely on the predictions of observational properties of the models, and their comparison with current Type Ia supernova data, including X-ray spectra of Type Ia supernova remnants.

E. Bravo; C. Badenes; D. Garcia-Senz

2004-12-07T23:59:59.000Z

180

39Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Requirements OutlineRequirements Outline  

E-Print Network [OSTI]

39Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center responsibility: both accept and request #12;40Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center MotivationsMotivations l Adjustable autonomy places severe requirements

Kortenkamp, David

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

60Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center NASA HCA Applications OutlineNASA HCA Applications Outline  

E-Print Network [OSTI]

60Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center NASA HCA Applications OutlineNASA HCA Applications Outline l 3T Control Architecture ­ architecture Satellite Assistant (under development) #12;61Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David

Kortenkamp, David

182

81Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Deep Space One Remote AgentDeep Space One Remote Agent  

E-Print Network [OSTI]

81Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center of the NASA 1999 Software of the Year Award #12;82Dr. Gregory A. Dorais, NASA Ames Research Center Dr. David Kortenkamp, NASA Johnson Space Center Deep Space One (DS1)Deep Space One (DS1) l Launched 10/98 l Remote

Kortenkamp, David

183

An Analysis of Department of Defense Instruction 8500.2 'Information Assurance (IA) Implementation.'  

SciTech Connect (OSTI)

The Department of Defense (DoD) provides its standard for information assurance in its Instruction 8500.2, dated February 6, 2003. This Instruction lists 157 'IA Controls' for nine 'baseline IA levels.' Aside from distinguishing IA Controls that call for elevated levels of 'robustness' and grouping the IA Controls into eight 'subject areas' 8500.2 does not examine the nature of this set of controls, determining, for example, which controls do not vary in robustness, how this set of controls compares with other such sets, or even which controls are required for all nine baseline IA levels. This report analyzes (1) the IA Controls, (2) the subject areas, and (3) the Baseline IA levels. For example, this report notes that there are only 109 core IA Controls (which this report refers to as 'ICGs'), that 43 of these core IA Controls apply without variation to all nine baseline IA levels and that an additional 31 apply with variations. This report maps the IA Controls of 8500.2 to the controls in NIST 800-53 and ITGI's CoBIT. The result of this analysis and mapping, as shown in this report, serves as a companion to 8500.2. (An electronic spreadsheet accompanies this report.)

Campbell, Philip LaRoche

2012-01-01T23:59:59.000Z

184

Learning from the scatter in type Ia supernovae  

SciTech Connect (OSTI)

Type Ia Supernovae are standard candles so their mean apparent magnitude has been exploited to learn about the redshift-distance relationship. Besides intrinsic scatter in this standard candle, additional scatter is caused by gravitational magnification by large scale structure. Here we probe the dependence of this dispersion on cosmological parameters and show that information about the amplitude of clustering, {sigma}{sub 8}, is contained in the scatter. In principle, it will be possible to constrain {sigma}{sub 8} to within 5% with observations of 2000 Type Ia Supernovae. We identify three sources of systematic error - evolution of intrinsic scatter, baryon contributions to lensing, and non-Gaussianity of lensing - which will make this measurement difficult.

Dodelson, Scott [Particle Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500 (United States); Department of Astronomy and Astrophysics, University of Chicago, Chicago, Illinois 60637-1433 (United States); Vallinotto, Alberto [Particle Astrophysics Center, Fermi National Accelerator Laboratory, Batavia, Illinois 60510-0500 (United States); Department of Physics, The University of Chicago, Chicago, Illinois 60637-1433 (United States)

2006-09-15T23:59:59.000Z

185

RADIOACTIVELY POWERED RISING LIGHT CURVES OF TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

The rising luminosity of the recent, nearby supernova 2011fe shows a quadratic dependence with time during the first Almost-Equal-To 0.5-4 days. In addition, studies of the composite light curves formed from stacking together many Type Ia supernovae (SNe Ia) have found similar power-law indices for the rise, but may also show some dispersion that may indicate diversity. I explore what range of power-law rises are possible due to the presence of radioactive material near the surface of the exploding white dwarf (WD). I summarize what constraints such a model places on the structure of the progenitor and the distribution and velocity of ejecta. My main conclusion is that for the inferred explosion time for SN 2011fe, its rise requires an increasing mass fraction X {sub 56} Almost-Equal-To (4-6) Multiplication-Sign 10{sup -2} of {sup 56}Ni distributed between a depth of Almost-Equal-To 10{sup -2} and 0.3 M {sub Sun} below the WD's surface. Radioactive elements this shallow are not found in simulations of a single C/O detonation. Scenarios that may produce this material include helium-shell burning during a double-detonation ignition, a gravitationally confined detonation, and a subset of deflagration to detonation transition models. In general, the power-law rise can differ from quadratic depending on the details of the velocity, density, and radioactive deposition gradients in a given event. Therefore, comparisons of this work with observed bolometric rises of SNe Ia would place strong constraints on the properties of the shallow outer layers, providing important clues for identifying the elusive progenitors of SNe Ia.

Piro, Anthony L., E-mail: piro@caltech.edu [Theoretical Astrophysics, California Institute of Technology, 1200 East California Boulevard, M/C 350-17, Pasadena, CA 91125 (United States)

2012-11-10T23:59:59.000Z

186

Ames Lab Plays Elemental Role in New PBS Special | Department of Energy  

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

Lab Plays Elemental Role in New PBS Special Lab Plays Elemental Role in New PBS Special Ames Lab Plays Elemental Role in New PBS Special April 4, 2012 - 2:34pm Addthis New York Times technology correspondent David Pogue -- host of NOVA’s popular “Making Stuff” series -- takes viewers on a quest to understand chemistry and all of the materials of life: the 118 unique elements that make up the amazing periodic table, including the 90 naturally-occurring elements and those created by scientists. | Photo courtesy of PBS. New York Times technology correspondent David Pogue -- host of NOVA's popular "Making Stuff" series -- takes viewers on a quest to understand chemistry and all of the materials of life: the 118 unique elements that make up the amazing periodic table, including the 90 naturally-occurring

187

THE NASA AMES POLYCYCLIC AROMATIC HYDROCARBON INFRARED SPECTROSCOPIC DATABASE: THE COMPUTED SPECTRA  

SciTech Connect (OSTI)

The astronomical emission features, formerly known as the unidentified infrared bands, are now commonly ascribed to polycyclic aromatic hydrocarbons (PAHs). The laboratory experiments and computational modeling done at the NASA Ames Research Center to create a collection of PAH IR spectra relevant to test and refine the PAH hypothesis have been assembled into a spectroscopic database. This database now contains over 800 PAH spectra spanning 2-2000 {mu}m (5000-5 cm{sup -1}). These data are now available on the World Wide Web at www.astrochem.org/pahdb. This paper presents an overview of the computational spectra in the database and the tools developed to analyze and interpret astronomical spectra using the database. A description of the online and offline user tools available on the Web site is also presented.

Bauschlicher, C. W.; Ricca, A. [NASA Ames Research Center, MS 230-3, Moffett Field, CA 94035 (United States); Boersma, C.; Mattioda, A. L.; Cami, J.; Peeters, E.; Allamandola, L. J. [NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035 (United States); Sanchez de Armas, F.; Puerta Saborido, G. [SETI Institute, 515 N. Whisman Road, Mountain View, CA 94043 (United States); Hudgins, D. M., E-mail: Charles.W.Bauschlicher@nasa.go [NASA Headquarters, MS 3Y28, 300 E St. SW, Washington, DC 20546 (United States)

2010-08-15T23:59:59.000Z

188

The Diversity of Variations in the Spectra of Type Ia Supernovae  

E-Print Network [OSTI]

for the degree of DOCTOR OF PHILOSOPHY Approved by: Chair of Committee, Lifan Wang Committee Members, Nicholas Suntze George Kattawar Sean McDeavitt Head of Department, George R. Welch August 2012 Major Subject: Physics iii ABSTRACT The Diversity... of Variations in the Spectra of Type Ia Supernovae. (August 2012) Andrew James Wagers, B.A., Berea College; M.S., Stephen F. Austin State University Chair of Advisory Committee: Dr. Lifan Wang Type Ia supernovae (SNe Ia) are currently the best probe...

Wagers, Andrew James

2012-10-19T23:59:59.000Z

189

Experto Universitario Java Enterprise 2012-2013 Depto. Ciencia de la Computacin e IA  

E-Print Network [OSTI]

Experto Universitario Java Enterprise © 2012-2013 Depto. Ciencia de la Computación e IA Lenguaje Lenguaje Java Avanzado © 2012-2013 Depto. Ciencia de la Computación e IA Lenguaje Java 2 Índice. Ciencia de la Computación e IA Lenguaje Java 3 Java · Java es un lenguaje OO creado por Sun Microsystems

Escolano, Francisco

190

Experto Universitario Java Enterprise 2012-2013 Depto. Ciencia de la Computacin e IA  

E-Print Network [OSTI]

Experto Universitario Java Enterprise © 2012-2013 Depto. Ciencia de la Computación e IA Lenguaje Avanzado © 2012-2013 Depto. Ciencia de la Computación e IA Depuración y logs - 2 · El depurador de Eclipse Enterprise Lenguaje Java Avanzado © 2012-2013 Depto. Ciencia de la Computación e IA Depuración y logs - 3 El

Escolano, Francisco

191

Teor'ia de Grupos y Mec'anica Qu'antica Luis A. Seco  

E-Print Network [OSTI]

determinado por el Hamiltoniano de la energ'ia, un operador que, actuando sobre una funci'on /(x 1 ; : : : ; xTeor'ia de Grupos y Mec'anica Qu'antica Luis A. Seco Universidad de Toronto. Notas del curso; Teor'ia de Grupos y Mec'anica Cu'antica, L. Seco. U.I.M.P. La Coru~na, 27 Junio -- 1 Julio, 1994

Seco, Luis A.

192

Turbulence-Flame Interactions in Type Ia Supernovae  

E-Print Network [OSTI]

The large range of time and length scales involved in type Ia supernovae (SN Ia) requires the use of flame models. As a prelude to exploring various options for flame models, we consider, in this paper, high-resolution three-dimensional simulations of the small-scale dynamics of nuclear flames in the supernova environment in which the details of the flame structure are fully resolved. The range of densities examined, 1 to $8 \\times 10^7$ g cm$^{-3}$, spans the transition from the laminar flamelet regime to the distributed burning regime where small scale turbulence disrupts the flame. The use of a low Mach number algorithm facilitates the accurate resolution of the thermal structure of the flame and the inviscid turbulent kinetic energy cascade, while implicitly incorporating kinetic energy dissipation at the grid-scale cutoff. For an assumed background of isotropic Kolmogorov turbulence with an energy characteristic of SN Ia, we find a transition density between 1 and $3 \\times 10^7$ g cm$^{-3}$ where the nature of the burning changes qualitatively. By $1 \\times 10^7$ g cm$^{-3}$, energy diffusion by conduction and radiation is exceeded, on the flame scale, by turbulent advection. As a result, the effective Lewis Number approaches unity. That is, the flame resembles a laminar flame, but is turbulently broadened with an effective diffusion coefficient, $D_T \\sim u' l$, where $u'$ is the turbulent intensity and $l$ is the integral scale. For the larger integral scales characteristic of a real supernova, the flame structure is predicted to become complex and unsteady. Implications for a possible transition to detonation are discussed.

A. J. Aspden; J. B. Bell; M. S. Day; S. E. Woosley; M. Zingale

2008-11-17T23:59:59.000Z

193

The Recurrent Nova U Scorpii - A Type Ia Supernova Progenitor  

E-Print Network [OSTI]

We derive the mass of the white dwarf in the eclipsing recurrent nova U Sco from the radial velocity semi-amplitudes of the primary and secondary stars. Our results give a high white dwarf mass of M_1 = 1.55 \\pm 0.24M_\\odot, consistent with the thermonuclear runaway model of recurrent nova outbursts. We confirm that U Sco is the best Type Ia supernova progenitor known, and predict that the time to explosion is within ~700,000 years.

T. D. Thoroughgood; V. S. Dhillon; S. P. Littlefair; T. R. Marsh; D. A. Smith

2001-09-28T23:59:59.000Z

194

Tension in the Recent Type Ia Supernovae Datasets  

E-Print Network [OSTI]

In the present work, we investigate the tension in the recent Type Ia supernovae (SNIa) datasets Constitution and Union. We show that they are in tension not only with the observations of the cosmic microwave background (CMB) anisotropy and the baryon acoustic oscillations (BAO), but also with other SNIa datasets such as Davis and SNLS. Then, we find the main sources responsible for the tension. Further, we make this more robust by employing the method of random truncation. Based on the results of this work, we suggest two truncated versions of the Union and Constitution datasets, namely the UnionT and ConstitutionT SNIa samples, whose behaviors are more regular.

Hao Wei

2010-04-07T23:59:59.000Z

195

KPD1930+2752 - a candidate Type Ia supernova progenitor  

E-Print Network [OSTI]

We present spectra of the pulsating sdB star KPD1930+2752 which confirm that this star is a binary. The radial velocities measured from the H-alpha and HeI6678 spectral lines vary sinusoidally with the same period (2h 17m) as the ellipsoidal variability seen by Billeres et al. (2000). The amplitude of the orbital motion (349.3+-2.7 km/s) combined with the canonical mass for sdB stars (0.5 solar masses) implies a total mass for the binary of 1.47+-0.01 solar masses The unseen companion star is almost certainly a white dwarf star. The binary will merge within about 200 million years due to gravitational wave radiation. The accretion of helium and other elements heavier than hydrogen onto the white dwarf which then exceeds the Chandrasekhar mass (1.4 solar masses) is a viable model for the cause of Type Ia supernovae. KPD1930+2752 is the first star to be discovered which is a good candidate for the progenitor of a Type Ia supernova of this type which will merge on an astrophysically interesting timescale.

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

2000-07-18T23:59:59.000Z

196

Search for progenitors of supnernovae type Ia with SPY  

E-Print Network [OSTI]

We have started a large survey for double degenerate (DD) binaries as potential progenitors of type Ia supernovae with the UVES spectrograph at the ESO VLT (ESO SN Ia Progenitor surveY - SPY). About 400 white dwarfs were checked for radial velocity variations during the first 15 months of this project, twice the number of white dwarfs investigated during the last 20 years. We give an overview of the SPY project and present first results Fifty four new DDs have been discovered, seven of them double lined (only 18 and 6 objects of these groups were known before, respectively). The final sample is expected to contain 150 to 200 DDs. Eight new pre-cataclysmic binaries were also detected. SPY is the first DD survey which encompasses also non-DA white dwarfs. SPY produces an immense, unique sample of very high resolution white dwarf spectra, which provides a lot of spin-off opportunities. We describe our projects to exploit the SPY sample for the determination of basic parameters, kinematics, and rotational velocities of white dwarfs. A catalogue with a first subset of our white dwarf data has already been published by Koester et al. 2001.

R. Napiwotzki; N. Christlieb; H. Drechsel; H. -J. Hagen; U. Heber; D. Homeier; C. Karl; D. Koester; B. Leibundgut; T. R. Marsh; S. Moehler; G. Nelemans; E. -M. Pauli; D. Reimers; A. Renzini; L. Yungelson

2002-03-09T23:59:59.000Z

197

NJ WY AK AL CA AR CO CT DE FL GA HI ID KS IL IN IA IA KY LA  

Gasoline and Diesel Fuel Update (EIA)

0.00-1.99 0.00-1.99 2.00-2.99 3.00-3.99 4.00-4.99 5.00-5.99 6.00-6.99 7.00+ NJ WY AK AL CA AR CO CT DE FL GA HI ID KS IL IN IA IA KY LA ME MI MA MD MN MS MT MO NE ND OH NV NM NY NH NC OK OR PA RI SC SD TN TX UT VT WA WV WI AZ VA DC 0.00-1.99 2.00-2.99 3.00-3.99 4.00-4.99 5.00-5.99 6.00-6.99 7.00+ 18. Average Price of Natural Gas Delivered to U.S. Onsystem Industrial Consumers, 1996 (Dollars per Thousand Cubic Feet) Figure 19. Average Price of Natural Gas Delivered to U.S. Electric Utilities, 1996 (Dollars per Thousand Cubic Feet) Figure Sources: Federal Energy Regulatory Commission (FERC), Form FERC-423, "Monthly Report of Cost and Quality of Fuels for Electric Plants," and Energy Information Administration (EIA), Form EIA-176, "Annual Report of Natural and Supplemental Gas Supply and Disposition." Note: In 1996, consumption of natural gas for agricultural use

198

Search for double degenerate progenitors of supernovae type Ia with SPY  

E-Print Network [OSTI]

We report on a large survey for double degenerate (DD) binaries as potential progenitors of type Ia supernovae with the UVES spectrograph at the ESO VLT (SN Ia Progenitor surveY - SPY). About 560 white dwarfs were checked for radial velocity variations until now. Ninety new DDs have been discovered, including short period systems with masses close to the Chandrasekhar mass.

R. Napiwotzki; N. Christlieb; H. Drechsel; H. -J. Hagen; U. Heber; D. Homeier; C. Karl; D. Koester; B. Leibundgut; T. R. Marsh; S. Moehler; G. Nelemans; E. -M. Pauli; D. Reimers; A. Renzini; L. Yungelson

2002-10-29T23:59:59.000Z

199

Analytical Expressions For Light-Curves Of Ordinary And Superluminous Supernovae Type Ia  

E-Print Network [OSTI]

Ordinary supernovae of type Ia (SNeIa) may be produced by the thermonuclear explosion of white dwarfs (WDs), which after their nascence in proto-planetary nebulae accrete fall-back matter and approach the Chandrasekhar mass limit. If the detonation continues into the fall-back layer and/or if the SNIa debris collide with it, they may produce a super Chandrasekhar SNIa. A few underlying physical assumptions of such model yield a very simple master formula that reproduces quite well the bolometric light-curves of both ordinary and supeluminous SNeIa. Other main properties of SNeIa, including the empirical 'brighter-slower' Philipps' relation that was used to standardize ordinary SNeIa as distance indicators and led to the discovery of the accelerating expansion of the universe are also reproduced.

Shlomo Dado; Arnon Dar

2014-02-06T23:59:59.000Z

200

Type Ia supernova rate studies from the SDSS-II Supernova Study  

SciTech Connect (OSTI)

The author presents new measurements of the type Ia SN rate from the SDSS-II Supernova Survey. The SDSS-II Supernova Survey was carried out during the Fall months (Sept.-Nov.) of 2005-2007 and discovered {approx} 500 spectroscopically confirmed SNe Ia with densely sampled (once every {approx} 4 days), multi-color light curves. Additionally, the SDSS-II Supernova Survey has discovered several hundred SNe Ia candidates with well-measured light curves, but without spectroscopic confirmation of type. This total, achieved in 9 months of observing, represents {approx} 15-20% of the total SNe Ia discovered worldwide since 1885. The author describes some technical details of the SN Survey observations and SN search algorithms that contributed to the extremely high-yield of discovered SNe and that are important as context for the SDSS-II Supernova Survey SN Ia rate measurements.

Dilday, Benjamin; /Chicago U.

2008-08-01T23:59:59.000Z

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Type Ia supernovae selection and forecast of cosmology constraints for the Dark Energy Survey  

Science Journals Connector (OSTI)

We present the results of a study of selection criteria to identify Type Ia supernovae photometrically in a simulated mixed sample of Type Ia supernovae and core collapse supernovae. The simulated sample is a mockup of the expected results of the Dark Energy Survey. Fits to the \\{MLCS2k2\\} and SALT2 Type Ia supernova models are compared and used to help separate the Type Ia supernovae from the core collapse sample. The Dark Energy Task Force Figure of Merit (modified to include core collapse supernovae systematics) is used to discriminate among the various selection criteria. This study of varying selection cuts for Type Ia supernova candidates is the first to evaluate core collapse contamination using the Figure of Merit. Different factors that contribute to the Figure of Merit are detailed. With our analysis methods, both SALT2 and \\{MLCS2k2\\} Figures of Merit improve with tighter selection cuts and higher purities, peaking at 98% purity.

Eda Gjergo; Jefferson Duggan; John D. Cunningham; Steve Kuhlmann; Rahul Biswas; Eve Kovacs; Joseph P. Bernstein; Harold Spinka

2013-01-01T23:59:59.000Z

202

Microsoft PowerPoint - IEEE IAS PES 102313.pptx  

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

DOE's ARRA DOE's ARRA Smart Grid Program Steve Bossart, Senior Energy Analyst IEEE IAS/PES Pittsburgh Section October 23, 2013 ‹#› Topics * OE ARRA Smart Grid Program * OE ARRA Smart Grid Progress * Results and Case Studies * Life After ARRA Smart Grid ‹#› DOE OE ARRA Smart Grid Program ‹#› American Recovery and Reinvestment Act ($4.5B) * Smart Grid Investment Grants (99 projects) - $3.4 billion Federal; $4.7 billion private sector - > 800 PMUs covering almost 100% of transmission - ~ 8000 distribution automation circuits - > 15 million smart meters * Smart Grid Demonstration Projects (32 projects) - $685 million Federal; $1 billion private sector - 16 storage projects - 16 regional demonstrations Smart Grid ARRA Activities ‹#› Smart Grid investment from ARRA field projects

203

Type Ia Supernova: Burning and Detonation in the Distributed Regime  

E-Print Network [OSTI]

A simple, semi-analytic representation is developed for nuclear burning in Type Ia supernovae in the special case where turbulent eddies completely disrupt the flame. The speed and width of the ``distributed'' flame front are derived. For the conditions considered, the burning front can be considered as a turbulent flame brush composed of corrugated sheets of well-mixed flames. These flames are assumed to have a quasi-steady-state structure similar to the laminar flame structure, but controlled by turbulent diffusion. Detonations cannot appear in the system as long as distributed flames are still quasi-steady-state, but this condition is violated when the distributed flame width becomes comparable to the size of largest turbulent eddies. When this happens, a transition to detonation may occur. For current best estimates of the turbulent energy, the most likely density for the transition to detonation is in the range 0.5 - 1.5 x 10^7 g cm^{-3}.

S. E. Woosley

2007-09-26T23:59:59.000Z

204

Type Ia Supernova Hubble Residuals and Host-Galaxy Properties  

SciTech Connect (OSTI)

Kim et al. (2013) [K13] introduced a new methodology for determining peak- brightness absolute magnitudes of type Ia supernovae from multi-band light curves. We examine the relation between their parameterization of light curves and Hubble residuals, based on photometry synthesized from the Nearby Supernova Factory spec- trophotometric time series, with global host-galaxy properties. The K13 Hubble residual step with host mass is 0.013 ? 0.031 mag for a supernova subsample with data coverage corresponding to the K13 training; at ? 1?, the step is not significant and lower than previous measurements. Relaxing the data coverage requirement the Hubble residual step with host mass is 0.045 ? 0.026 mag for the larger sample; a calculation using the modes of the distributions, less sensitive to outliers, yields a step of 0.019 mag. The analysis of this article uses K13 inferred luminosities, as distinguished from previous works that use magnitude corrections as a function of SALT2 color and stretch param- eters: Steps at> 2? significance are found in SALT2 Hubble residuals in samples split by the values of their K13 x(1) and x(2) light-curve parameters. x(1) affects the light- curve width and color around peak (similar to the?m15 and stretch parameters), and x(2) affects colors, the near-UV light-curve width, and the light-curve decline 20 to 30 days after peak brightness. The novel light-curve analysis, increased parameter set, and magnitude corrections of K13 may be capturing features of SN Ia diversity arising from progenitor stellar evolution.

Nearby Supernova Factory; Kim, A. G.; Aldering, G.; Antilogus, P.; Aragon, C.; Bailey, S.; Baltay, C.; Bongard, S.; Buton, C.; Canto, A.; Cellier-Holzem, F.; Childress, M.; Chotard, N.; Copin, Y.; Fakhouri, H. K.; Feindt, U.; Fleury, M.; Gangler, E.; Greskovic, P.; Guy, J.; Kowalski, M.; Lombardo, S.; Nordin, J.; Nugent, P.; Pain, R.; Pecontal, E.; Pereira, R.; Perlmutter, S.; Rabinowitz, D.; Rigault, M.; Runge, K.; Saunders, C.; Scalzo, R.; Smadja, G.; Tao, C.; Thomas, R. C.; Weaver, B. A.

2014-01-17T23:59:59.000Z

205

A mutant of Escherichia coli defective in penicillin-binding protein 5 and lacking D-alanine carboxypeptidase IA.  

Science Journals Connector (OSTI)

...preparation of D-alanrne car- boxypeptidase IA of...IA, because a mutant defective in D-alanine carbox...both activities were defective or both were normal...residual D-alanine car- boxypeptidase IA activity...and to obtain a mutant defective in PBP-6 are in progress...

Y Nishimura; H Suzuki; Y Hirota; J T Park

1980-07-01T23:59:59.000Z

206

Stellar Populations and the White Dwarf Mass Function: Connections To Supernova Ia Luminosities  

E-Print Network [OSTI]

We discuss the luminosity function of SNe Ia under the assumption that recent evidence for dispersion in this standard candle is related to variations in the white dwarf mass function (WDMF) in the host galaxies. We develop a simple parameterization of the WDMF as a function of age of a stellar population and apply this to galaxies of different morphological types. We show that this simplified model is consistent with the observed WDMF of Bergeron et al. (1992) for the solar neighborhood. Our simple models predict that WDMF variations can produce a range of more than 1.8 mag in M$_B$(SN Ia), which is comparable to the observed value using the data of Phillips (1993) and van den Bergh (1996). We also predict a galaxy type dependence of M$_B$(SN Ia) under standard assumptions of the star formation history in these galaxies and show that M$_B$(SN Ia) can evolve with redshift. In principle both evolutionary and galaxy type corrections should be applied to recover the intrinsic range of M$_B$(SN Ia) from the observed values. Our current inadequate knowledge of the star formation history of galaxies coupled with poor physical understanding of the SN Ia mechanism makes the reliable estimation of these corrections both difficult and controversial. The predictions of our models combined with the observed galaxy and redshift correlations may have the power to discriminate between the Chandrasekhar and the sub-Chandrasekhar progenitor scenarios for SNe Ia.

Ted von Hippel; G. D. Bothun; R. A. Schommer

1997-06-11T23:59:59.000Z

207

Tension and Systematics in the Gold06 SnIa Dataset  

E-Print Network [OSTI]

The Gold06 SnIa dataset recently released in astro-ph/0611572 consists of five distinct subsets defined by the group or instrument that discovered and analyzed the corresponding data. These subsets are: the SNLS subset (47 SnIa), the HST subset (30 SnIa), the HZSST subset (41 SnIa), the SCP subset (26 SnIa) and the Low Redshift (LR) subset (38 SnIa). These subsets sum up to the 182 SnIa of the Gold06 dataset. We use Monte-Carlo simulations to study the statistical consistency of each one of the above subsets with the full Gold06 dataset. In particular, we compare the best fit $w(z)$ parameters (w_0,w_1) obtained by subtracting each one of the above subsets from the Gold06 dataset (subset truncation), with the corresponding best fit parameters (w^r_0,w^r_1) obtained by subtracting the same number of randomly selected SnIa from the same redshift range of the Gold06 dataset (random truncation). We find that the probability for (w^r_0,w^r_1)=(w_0,w_1) is large for the Gold06 minus SCP (Gold06-SCP) truncation but is less than 5% for the Gold06-SNLS, Gold06-HZSST and Gold06-HST truncations. This result implies that the Gold06 dataset is not statistically homogeneous. By comparing the values of the best fit (w_0,w_1) for each subset truncation we find that the tension among subsets is such that the SNLS and HST subsets are statistically consistent with each other and `pull' towards LCDM (w_0=-1,w_1=0) while the HZSST subset is statistically distinct and strongly `pulls' towards a varying w(z) crossing the line $w=-1$ from below (w_00). We also isolate six SnIa that are mostly responsible for this behavior of the HZSST subset.

S. Nesseris; L. Perivolaropoulos

2007-01-09T23:59:59.000Z

208

Solar abundance of manganese: a case for the existence of near Chandrasekhar-mass Type Ia supernova progenitors  

E-Print Network [OSTI]

Context: Manganese is predominantly synthesised in Type Ia supernova (SN Ia) explosions. Owing to the entropy dependence of the Mn yield in explosive thermonuclear burning, SNe Ia involving near Chandrasekhar-mass white dwarfs (WDs) are predicted to produce Mn to Fe ratios significantly exceeding those of SN Ia explosions involving sub-Chandrasekhar mass primary WDs. Of all current supernova explosion models, only SN Ia models involving near-Chandrasekhar mass WDs produce [Mn/Fe] > 0.0. Aims: Using the specific yields for competing SN Ia scenarios, we aim to constrain the relative fractions of exploding near-Chandrasekhar mass to sub-Chandrasekhar mass primary WDs in the Galaxy. Methods: We extract the Mn yields from three-dimensional thermonuclear supernova simulations referring to different initial setups and progenitor channels. We then compute the chemical evolution of Mn in the Solar neighborhood, assuming SNe Ia are made up of different relative fractions of the considered explosion models. Results: We ...

Seitenzahl, Ivo R; Roepke, Friedrich K; Ruiter, Ashley J

2013-01-01T23:59:59.000Z

209

INDECOMPOSABLE RACKS OF ORDER p2 MAT'IAS GRA"NA  

E-Print Network [OSTI]

INDECOMPOSABLE RACKS OF ORDER p2 MAT'IAS GRA"NA Abstract.We classify indecomposable racks of order p2(p a prime). There a of prime order is trivial. 1.Introduction Racks and quandles have

Graña, Matías

210

Structural studies of allosteric regulation in the class Ia Ribonucleotide reductase from Escherichia coli  

E-Print Network [OSTI]

Ribonucleotide reductase (RNR) converts ribonucleotides to deoxyribonucleotides, the building blocks for DNA replication and repair. The E. coli class Ia enzyme requires two subunits to catalyze the radical-based reduction ...

Zimanyi, Christina Marie

2013-01-01T23:59:59.000Z

211

Type Ia supernova rate at a redshift of ~;0.1  

SciTech Connect (OSTI)

We present the type Ia rate measurement based on two EROS supernova search campaigns (in 1999 and 2000). Sixteen supernovae identified as type Ia were discovered. The measurement of the detection efficiency, using a Monte Carlo simulation, provides the type Ia supernova explosion rate at a redshift {approx} 0.13. The result is 0.125{sub -0.034-0.028}{sup +0.044+0.028} h{sub 70}{sup 2} SNu where 1 SNu = 1 SN/10{sup 10} L{sub {circle_dot}}{sup B}/century. This value is compatible with the previous EROS measurement (Hardin et al. 2000), done with a much smaller sample, at a similar redshift. Comparison with other values at different redshifts suggests an evolution of the type Ia supernova rate.

Blanc, G.; Afonso, C.; Alard, C.; Albert, J.N.; Aldering, G.; Amadon, A.; Andersen, J.; Ansari, R.; Aubourg, E.; Balland, C.; Bareyre,P.; Beaulieu, J.P.; Charlot, X.; Conley, A.; Coutures, C.; Dahlen, T.; Derue, F.; Fan, X.; Ferlet, R.; Folatelli, G.; Fouque, P.; Garavini, G.; Glicenstein, J.F.; Goldman, B.; Goobar, A.; Gould, A.; Graff, D.; Gros,M.; Haissinski, J.; Hamadache, C.; Hardin, D.; Hook, I.M.; deKat, J.; Kent, S.; Kim, A.; Lasserre, T.; LeGuillou, L.; Lesquoy, E.; Loup, C.; Magneville, C.; Marquette, J.B.; Maurice, E.; Maury, A.; Milsztajn, A.; Moniez, M.; Mouchet, M.; Newberg, H.; Nobili, S.; Palanque-Delabrouille,N.; Perdereau, O.; Prevot, L.; Rahal, Y.R.; Regnault, N.; Rich, J.; Ruiz-Lapuente, P.; Spiro, M.; Tisserand, P.; Vidal-Madjar, A.; Vigroux,L.; Walton, N.A.; Zylberajch, S.

2004-05-11T23:59:59.000Z

212

~ VII -ATTiVIT EDILIZIE .. Servizio di Ateneo per lEnergIa  

E-Print Network [OSTI]

~ VII - ATTiVIT? EDILIZIE n'p. .' .. Servizio di Ateneo per lEnergIa - N AlJZ43 ········ - .·:tri

Di Pillo, Gianni

213

Infrastructure Assessment Mission: USACE Infrastructure Assessment (IA) Planning and Response Teams (PRTs) have two main  

E-Print Network [OSTI]

, and structural engineering applications; urban search & rescue (US&R) support; and water/wastewater) include pre- and post-declaration support for deploying an IA management cell, water/wastewater assessment

US Army Corps of Engineers

214

Gamma-rays from Type Ia supernova SN2014J  

E-Print Network [OSTI]

The whole set of INTEGRAL observations of type Ia supernova SN2014J, covering the period 16-162 days after the explosion has being analyzed. For spectral fitting the data are split into early and late periods covering days 16-35 and 50-162, respectively, optimized for Ni-56 and Co-56 lines. As expected for the early period much of the gamma-ray signal is confined to energies below $\\sim$200 keV, while for the late period it is most strong above 400 keV. In particular, in the late period Co-56 lines at 847 and 1248 keV are detected at 4.7 and 4.3 sigma respectively. The lightcurves in several representative energy bands are calculated for the entire period. The resulting spectra and lightcurves are compared with a subset of models. We confirm our previous finding that the gamma-ray data are broadly consistent with the expectations for canonical 1D models, such as delayed detonation or deflagration models for a near-Chandrasekhar mass WD. Late optical spectra (day 136 after the explosion) show rather symmetric ...

Churazov, E; Isern, J; Bikmaev, I; Bravo, E; Chugai, N; Grebenev, S; Jean, P; Kndlseder, J; Lebrun, F; Kuulkers, E

2015-01-01T23:59:59.000Z

215

2010-2011 Depto. Ciencia de la Computacin e IA Especialista Universitario Java Enterprise  

E-Print Network [OSTI]

© 2010-2011 Depto. Ciencia de la Computación e IA Especialista Universitario Java Enterprise Struts Sesión 4: Introducción a Struts 2 #12;© 2010-2011 Depto. Ciencia de la Computación e IA Especialista · Taglibs · Internacionalización · Validación · Conceptos nuevos en Struts 2 #12;© 2010-2011 Depto. Ciencia

Escolano, Francisco

216

Experto Universitario Java Enterprise 2012-2013 Depto. Ciencia de la Computacin e IA  

E-Print Network [OSTI]

Experto Universitario Java Enterprise © 2012-2013 Depto. Ciencia de la Computación e IA Lenguaje Java Avanzado Sesión 3: Tratamiento de errores #12;Lenguaje Java Avanzado © 2012-2013 Depto. Ciencia de · Tipos genéricos #12;Lenguaje Java Avanzado © 2012-2013 Depto. Ciencia de la Computación e IA Errores - 3

Escolano, Francisco

217

Constraining the double-degenerate scenario for Type Ia supernovae from merger ejected matter  

E-Print Network [OSTI]

We follow the mass blown during the WD-WD merger process in the Double-Degenerate (DD) scenario for type Ia supernovae (SN Ia), and find that the interaction of the SN ejecta with this wind affects the early (thermal energy and then to additional radiation. The radiation could be interpreted as an explosion originating from a progenitor having a radius of one solar radius or more, contradicting observations of SN 2011fe.

Levanon, Naveh; Garca-Berro, Enrique

2014-01-01T23:59:59.000Z

218

THE DISCOVERY OF THE MOST DISTANT KNOWN TYPE Ia SUPERNOVA AT REDSHIFT 1.914  

SciTech Connect (OSTI)

We present the discovery of a Type Ia supernova (SN) at redshift z = 1.914 from the CANDELS multi-cycle treasury program on the Hubble Space Telescope (HST). This SN was discovered in the infrared using the Wide-Field Camera 3, and it is the highest-redshift Type Ia SN yet observed. We classify this object as a SN Ia by comparing its light curve and spectrum with those of a large sample of Type Ia and core-collapse SNe. Its apparent magnitude is consistent with that expected from the {Lambda}CDM concordance cosmology. We discuss the use of spectral evidence for classification of z > 1.5 SNe Ia using HST grism simulations, finding that spectral data alone can frequently rule out SNe II, but distinguishing between SNe Ia and SNe Ib/c can require prohibitively long exposures. In such cases, a quantitative analysis of the light curve may be necessary for classification. Our photometric and spectroscopic classification methods can aid the determination of SN rates and cosmological parameters from the full high-redshift CANDELS SN sample.

Jones, David O.; Rodney, Steven A.; Riess, Adam G. [Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 (United States); Mobasher, Bahram [Department of Physics and Astronomy, University of California, Riverside, CA 92521 (United States); Dahlen, Tomas; Casertano, Stefano; Koekemoer, Anton [Space Telescope Science Institute, Baltimore, MD 21218 (United States); McCully, Curtis; Keeton, Charles R.; Patel, Brandon [Department of Physics and Astronomy, Rutgers, State University of New Jersey, Piscataway, NJ 08854 (United States); Frederiksen, Teddy F.; Hjorth, Jens [Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen (Denmark); Strolger, Louis-Gregory [Department of Physics, Western Kentucky University, Bowling Green, KY 42101 (United States); Wiklind, Tommy G. [Joint ALMA Observatory, ESO, Santiago (Chile); Challis, Peter [Harvard/Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Graur, Or [School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978 (Israel); Hayden, Brian; Garnavich, Peter [Department of Physics, University of Notre Dame, Notre Dame, IN 46556 (United States); Weiner, Benjamin J. [Department of Astronomy, University of Arizona, Tucson, AZ 85721 (United States); Filippenko, Alexei V. [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); and others

2013-05-10T23:59:59.000Z

219

CIMAT, VIII Escuela de verano, 30 de julio -12 de agos* Introducci'on a la Geometr'ia de la Mec'anic*  

E-Print Network [OSTI]

* *fluencia de una fuerza F(x) se define su energ'ia (como funci'on de su posici'on y velocidad) por E = T +* * V donde la energ'ia cin'etica T = m(x`)2=2 y la energ'ia potencial V (x) es una funci'on que(x) entonces su energ* *'ia E se mantiene constante en el tiempo (la Ley de Conservaci'on de Energ'ia

Bor, Gil

220

Who ESnet Serves  

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

Ames Laboratory (Ames, IA) ANL Argonne National Laboratory (Argonne, IL) BECHTEL-NV NSTec National Securities Technology (North Las Vegas, NV) BJC Bechtel Jacobs Corporation...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Verifying the Cosmological Utility of Type Ia Supernovae: Implications of a Dispersion in the Ultraviolet Spectra  

SciTech Connect (OSTI)

We analyze the mean rest-frame ultraviolet (UV) spectrum of Type Ia Supernovae (SNe) and its dispersion using high signal-to-noise ratio Keck-I/LRIS-B spectroscopy for a sample of 36 events at intermediate redshift (z=0.5) discovered by the Canada-France-Hawaii Telescope Supernova Legacy Survey (SNLS). We introduce a new method for removing host galaxy contamination in our spectra, exploiting the comprehensive photometric coverage of the SNLS SNe and their host galaxies, thereby providing the first quantitative view of the UV spectral properties of a large sample of distant SNe Ia. Although the mean SN Ia spectrum has not evolved significantly over the past 40percent of cosmic history, precise evolutionary constraints are limited by the absence of a comparable sample of high-quality local spectra. The mean UV spectrum of our z~;;=0.5 SNe Ia and its dispersion is tabulated for use in future applications. Within the high-redshift sample, we discover significant UV spectral variations and exclude dust extinction as the primary cause by examining trends with the optical SN color. Although progenitor metallicity may drive some of these trends, the variations we see are much larger than predicted in recent models and do not follow expected patterns. An interesting new result is a variation seen in the wavelength of selected UV features with phase. We also demonstrate systematic differences in the SN Ia spectral features with SN light curve width in both the UV and the optical. We show that these intrinsic variations could represent a statistical limitation in the future use of high-redshift SNe Ia for precision cosmology. We conclude that further detailed studies are needed, both locally and at moderate redshift where the rest-frame UV can be studied precisely, in order that future missions can confidently be planned to fully exploit SNe Ia as cosmological probes.

Nugent, Peter E; Ellis, R.S.; Sullivan, M.; Nugent, P.E.; Howell, D.A.; Gal-Yam, A.; Astier, P.; Balam, D.; Balland, C.; Basa, S.; Carlberg, R.; Conley, A.; Fouchez, D.; Guy, J.; Hardin, D.; Hook, I.; Pain, R.; Perrett, K.; Pritchet, C.J.; Regnault, N.

2008-02-28T23:59:59.000Z

222

Utilizing Type Ia Supernovae in a Large, Fast, Imaging Survey to Constrain Dark Energy  

E-Print Network [OSTI]

We study the utility of a large sample of type Ia supernovae that might be observed in an imaging survey that rapidly scans a large fraction of the sky for constraining dark energy. We consider information from the traditional luminosity distance test as well as the spread in SNeIa fluxes at fixed redshift induced by gravitational lensing. We include a treatment of photometric redshift uncertainties in our analysis. Our primary result is that the information contained in the mean distance moduli of SNeIa and the dispersion among SNeIa distance moduli complement each other, breaking a degeneracy between the present dark energy equation of state and its time variation without the need for a high-redshift supernova sample. To address photometric redshift uncertainties, we present dark energy constraints as a function of the size of an external set of spectroscopically-observed SNeIa that may be used for redshift calibration, nspec. We find that an imaging survey can constrain the dark energy equation of state at the epoch where it is best constrained with a 1-sigma error of sigma(wpiv)~0.03-0.09$, depending upon various assumptions. In addition, the marginal improvement in the error sigma(wpiv) from an increase in the spectroscopic calibration sample drops once nspec ~ 10^3. This result is important because it is of the order of the size of calibration samples likely to be compiled in the coming decade and because, for samples of this size, the spectroscopic and imaging surveys individually place comparable constraints on the dark energy equation of state. In all cases, it is best to calibrate photometric redshifts with a set of spectroscopically-observed SNeIa with relatively more objects at high redshift than the parent sample of imaging SNeIa.

Andrew R. Zentner; Suman Bhattacharya

2008-12-01T23:59:59.000Z

223

Development of a MATLAB/STK TLE Accuracy Assessment Tool, in support of the NASA Ames Space Traffic Management Project  

E-Print Network [OSTI]

In order to improve the effectiveness of conjunction analysis using publically available Two Line Elements (TLEs) a number of strategies are being investigated as part of the Space Traffic Management project at NASA Ames Research Center. To assist in evaluating the effectiveness of these approaches a tool was developed in the MATLAB programming language that interfaces with the AGI Satellite Toolkit and with Microsoft Excel. The TLEs and any available truth ephemerides are read in by the tool and propagated orbits are compared using STK to estimate the errors. This tool is employed to determine the covariance and investigate the growth of errors in propagating the orbit of the CNESStella geodetic satellite. The different sources of error are assessed and future improvements to the tool are suggested.

Mason, James

2013-01-01T23:59:59.000Z

224

Discovering the Nature of Dark Energy: Towards Better Distances from Type Ia Supernovae -- Final Technical Report  

SciTech Connect (OSTI)

Type Ia supernovae (SNe Ia; exploding white-dwarf stars) were the key to the Nobel-worthy 1998 discovery and subsequent verification that the expansion of the Universe is accelerating, driven by the effects of dark energy. Understanding the nature of this mysterious, yet dominant, component of the Universe is at the forefront of research in cosmology and fundamental physics. SNe Ia will continue to play a leading role in this enterprise, providing precise cosmological distances that improve constraints on the nature of dark energy. However, for this effort to succeed, we need to more thoroughly understand relatively nearby SNe Ia, because our conclusions come only from comparisons between them and distant (high-redshift) SNe Ia. Thus, detailed studies of relatively nearby SNe Ia are the focus of this research program. Many interesting results were obtained during the course of this project; these were published in 32 refereed research papers that acknowledged the grant. A major accomplishment was the publication of supernova (SN) rates derived from about a decade of operation of the Lick Observatory Supernova Search (LOSS) with the 0.76-meter Katzman Automatic Imaging Telescope (KAIT). We have determined the most accurate rates for SNe of different types in large, nearby galaxies in the present-day Universe, and these can be compared with SN rates far away (and hence long ago in the past) to set constraints on the types of stars that explode. Another major accomplishment was the publication of the light curves (brightness vs. time) of 165 SNe Ia, along with optical spectroscopy of many of these SNe as well as other SNe Ia, providing an extensive, homogeneous database for detailed studies. We have conducted intensive investigations of a number of individual SNe Ia, including quite unusual examples that allow us to probe the entire range of SN explosions and provide unique insights into these objects and the stars before they explode. My team's studies have also led to the identification of subsamples of SNe Ia that can be used to provide the most reliable cosmological distances, and we developed ways to deal with the dust that makes SNe Ia appear fainter than they really are. Using the KAIT/LOSS sample, we produced an excellent Hubble diagram (galaxy recession speed vs. distance), accurately showing the expansion of the Universe. Even smaller scatter was achieved when spectroscopic characteristics were taken into account. Another high-quality Hubble diagram was constructed with SNe Ia from the Sloan Digital Sky Survey (SDSS). These Hubble diagrams provide useful new constraints on the nature of the dark energy that is accelerating the expansion of the Universe. As an added bonus of our research, we also studied core-collapse SNe, which differ fundamentally from SNe Ia.

Filippenko, Alexei Vladimir [Univ. California, Berkeley

2014-05-09T23:59:59.000Z

225

CfA4: LIGHT CURVES FOR 94 TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

We present multi-band optical photometry of 94 spectroscopically confirmed Type Ia supernovae (SNe Ia) in the redshift range 0.0055-0.073, obtained between 2006 and 2011. There are a total of 5522 light-curve points. We show that our natural-system SN photometry has a precision of {approx}< 0.03 mag in BVr'i', {approx}< 0.06 mag in u', and {approx}< 0.07 mag in U for points brighter than 17.5 mag and estimate that it has a systematic uncertainty of 0.014, 0.010, 0.012, 0.014, 0.046, and 0.073 mag in BVr'i'u'U, respectively. Comparisons of our standard-system photometry with published SN Ia light curves and comparison stars reveal mean agreement across samples in the range of {approx}0.00-0.03 mag. We discuss the recent measurements of our telescope-plus-detector throughput by direct monochromatic illumination by Cramer et al. This technique measures the whole optical path through the telescope, auxiliary optics, filters, and detector under the same conditions used to make SN measurements. Extremely well characterized natural-system passbands (both in wavelength and over time) are crucial for the next generation of SN Ia photometry to reach the 0.01 mag accuracy level. The current sample of low-z SNe Ia is now sufficiently large to remove most of the statistical sampling error from the dark-energy error budget. But pursuing the dark-energy systematic errors by determining highly accurate detector passbands, combining optical and near-infrared (NIR) photometry and spectra, using the nearby sample to illuminate the population properties of SNe Ia, and measuring the local departures from the Hubble flow will benefit from larger, carefully measured nearby samples.

Hicken, Malcolm; Challis, Peter; Kirshner, Robert P.; Bakos, Gaspar; Berlind, Perry; Brown, Warren R.; Caldwell, Nelson; Calkins, Mike; Falco, Emilio; Fernandez, Jose; Friedman, Andrew S.; Groner, Ted; Hartman, Joel [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States); Rest, Armin [Space Telescope Science Institute, Baltimore, MD 21218 (United States); Cramer, Claire E. [NIST (National Institute of Standards and Technology), Gaithersburg, MD 20899 (United States); Wood-Vasey, W. Michael [Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 (United States); Currie, Thayne [NASA, Goddard Space Flight Center, Greenbelt, MD 20771 (United States); De Kleer, Kathy [Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States); Esquerdo, Gil; Everett, Mark, E-mail: mhicken@cfa.harvard.edu [Planetary Science Institute, 1700 East Fort Lowell Road, Tucson, AZ 85719 (United States); and others

2012-06-01T23:59:59.000Z

226

IAS15: a fast, adaptive, high-order integrator for gravitational dynamics, accurate to machine precision over a billion orbits  

Science Journals Connector (OSTI)

......error behaves like a random walk. Our tests show that ias15 is superior to a mixed-variable...that ias15 follows Brouwer's law. We test our integrator in a wide variety of cases...focus on the two-body problem, a simple test case where we know the correct answer......

Hanno Rein; David S. Spiegel

2015-01-01T23:59:59.000Z

227

FROM RACKS TO POINTED HOPF ALGEBRAS AS ANDRUSKIEWITSCH AND MAT IAS GRA ~  

E-Print Network [OSTI]

FROM RACKS TO POINTED HOPF ALGEBRAS NICOL #19; AS ANDRUSKIEWITSCH AND MAT #19; IAS GRA ~ NA (C X; c q ), where X is a rack and q is a 2-cocycle on X with values in C #2; . Racks and cohomology of racks appeared also in the work of topologists. This leads us to the study of the structure of racks

Graña, Matías

228

Flames in Type Ia Supernova: Deflagration-Detonation Transition in the Oxygen Burning Flame  

E-Print Network [OSTI]

Flames in Type Ia Supernova: Deflagration-Detonation Transition in the Oxygen Burning Flame S. E of these regions can be supersonic and could initiate a detonation. Subject headings: supernovae: general a late time transition of the thermonuclear burning to a detonation wave (e.g., Hoflich et al. 1995

229

Section I. Summary of Project Activities Section I-A. 2008-2009 Project Summary  

E-Print Network [OSTI]

Section I. Summary of Project Activities Section I-A. 2008-2009 Project Summary University year, we accomplished the following: · Established a dual career opportunity procedure vetted to address, communicate procedures for the new daycare facility, and to explore the potential

Farritor, Shane

230

SEASONAL V A R IA TIONS IN STRUCTURE AND CIRCULATION IN THE RED SEA  

E-Print Network [OSTI]

SEASONAL V A R IA TIONS IN STRUCTURE AND CIRCULATION IN THE RED SEA A DISSERTATION SUBMITTE D and surface circulation in the Red Sea, occur r ing along the north-south axis of the Sea and extending fr om on in the northern Red Sea is frorn the nor th-northwest throughout the year' during the winter ( fr om October

Luther, Douglas S.

231

Seminar Ia, cetrti letnik, stari program LONGITUDINAL DYNAMICS OF PARTICLES IN ACCELERATORS  

E-Print Network [OSTI]

Seminar Ia, cetrti letnik, stari program LONGITUDINAL DYNAMICS OF PARTICLES IN ACCELERATORS Author motion of charged particles in particle accelerators. The technique of acceleration by electromagnetic waves is explored and the stability of motion under such acceleration is inspected. The seminar

?umer, Slobodan

232

Final Technical Report: Discovering the Nature of Dark Energy: Towards Better Distances from Type Ia Supernovae  

SciTech Connect (OSTI)

The final technical report from the project "Discovering the Nature of Dark Energy: Towards Better Distances from Type Ia Supernovae" led at Rutgers the State University of New Jersey by Prof. Saurabh W. Jha is presented, including all publications resulting from this award.

Saurabh W. Jha

2012-10-03T23:59:59.000Z

233

SponSored by http://www.ntu.edu.sg/ias/oCpA8  

E-Print Network [OSTI]

SponSored by http://www.ntu.edu.sg/ias/oCpA8 International Conference on physics education · Statistical and Nonlinear physics · Science Education · Women in Physics Sir Michael PEPPER Univ. College or poster presentations. All posters at the conference will be considered for the 2014 OCPA-APS Outstanding

Faraon, Andrei

234

THE CARNEGIE SUPERNOVA PROJECT: SECOND PHOTOMETRY DATA RELEASE OF LOW-REDSHIFT TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

The Carnegie Supernova Project (CSP) was a five-year observational survey conducted at Las Campanas Observatory that obtained, among other things, high-quality light curves of {approx}100 low-redshift Type Ia supernovae (SNe Ia). Presented here is the second data release of nearby SN Ia photometry consisting of 50 objects, with a subset of 45 having near-infrared follow-up observations. Thirty-three objects have optical pre-maximum coverage with a subset of 15 beginning at least five days before maximum light. In the near-infrared, 27 objects have coverage beginning before the epoch of B-band maximum, with a subset of 13 beginning at least five days before maximum. In addition, we present results of a photometric calibration program to measure the CSP optical (uBgVri) bandpasses with an accuracy of {approx}1%. Finally, we report the discovery of a second SN Ia, SN 2006ot, similar in its characteristics to the peculiar SN 2006bt.

Stritzinger, Maximilian D. [The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, 10691 Stockholm (Sweden); Phillips, M. M.; Campillay, Abdo; Morrell, Nidia; Krzeminski, Wojtek; Roth, Miguel [Carnegie Observatories, Las Campanas Observatory, La Serena (Chile); Boldt, Luis N. [Argelander Institut fuer Astronomie, Universitaet Bonn, D-53111 Bonn (Germany); Burns, Chris; Freedman, Wendy L.; Madore, Barry F.; Persson, Sven E. [Observatories of the Carnegie Institution for Science, Pasadena, CA 91101 (United States); Contreras, Carlos [Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Victoria 3122 (Australia); Gonzalez, Sergio [Atacama Large Millimeter/Submillimeter Array, European Southern Observatory (Chile); Folatelli, Gaston [Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan); Salgado, Francisco [Leiden Observatory, Leiden University, NL-2300 RA Leiden (Netherlands); DePoy, D. L.; Marshall, J. L.; Rheault, Jean-Philippe; Suntzeff, Nicholas B. [George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A and M University, College Station, TX 77843 (United States); Hamuy, Mario, E-mail: max.stritzinger@astro.su.se, E-mail: max@dark-cosmology.dk, E-mail: mstritzinger@lco.cl [Departamento de Astronomia, Universidad de Chile, Santiago (Chile)

2011-11-15T23:59:59.000Z

235

Abstract IA08: PTEN and PI3K signaling in brain development and disease  

Science Journals Connector (OSTI)

...Abstract IA08: PTEN and PI3K signaling in brain development and disease Suzanne J. Baker...an increased genetic susceptibility to brain tumors. However, inherited mutation of...and tumor suppression in the mammalian brain. Recently, germline or somatic mutations...

Suzanne J. Baker

2014-12-01T23:59:59.000Z

236

Turbulent Oxygen Flames in Type Ia Supernovae A. J. Aspden1  

E-Print Network [OSTI]

Turbulent Oxygen Flames in Type Ia Supernovae A. J. Aspden1 , J. B. Bell1 , and S. E. Woosley2 oxygen flames. The two aims of the paper are to examine the response of the inductive oxygen flame to intense levels of turbulence, and to explore the possibility of transition to detonation in the oxygen

237

The superconducting spin valve and triplet superconductivity I.A. Garifullin a,n  

E-Print Network [OSTI]

The superconducting spin valve and triplet superconductivity I.A. Garifullin a,n , P.V. Leksin s t r a c t A review of our recent results on the spin valve effect is presented. We have used coefficient DF and the exchange splitting I of the conduction band in the F layer [1]. For pure Fe the value

Fominov, Yakov

238

CIMAT, VIII Escuela de verano, 30 de julio -12 de ago* Introducci'on a la Geometr'ia de la Mec'ani*  

E-Print Network [OSTI]

con un valor fijo de la energ* *'ia corresponden a secciones del cono del inciso (a) por * *energ'ia tienen el mismo semi-eje mayor. 11.Demuestra la tercera ley de Kepler: toda soluci'on peri Introducci'on a la Geometr'ia de la Mec'ani* *ca Cl'asica Problemas 7 - 12

Bor, Gil

239

Recovery and Characterization of ?-Zein from Corn Fermentation Coproducts  

Science Journals Connector (OSTI)

Recovery and Characterization of ?-Zein from Corn Fermentation Coproducts ... Commercial DDGS was obtained from Lincolnway Energy, Ames, IA. ...

Ilankovan Paraman; Buddhi P. Lamsal

2011-03-09T23:59:59.000Z

240

The NASA Ames PAH IR Spectroscopic Database Version 2.00: Updated Content, Web Site, and On(Off)line Tools  

Science Journals Connector (OSTI)

A significantly updated version of the NASA Ames PAH IR Spectroscopic Database, the first major revision since its release in 2010, is presented. The current version, version 2.00, contains 700 computational and 75 experimental spectra compared, respectively, with 583 and 60 in the initial release. The spectra span the 2.5-4000 ?m (4000-2.5 cm-1) range. New tools are available on the site that allow one to analyze spectra in the database and compare them with imported astronomical spectra as well as a suite of IDL object classes (a collection of programs utilizing IDL's object-oriented programming capabilities) that permit offline analysis called the AmesPAHdbIDLSuite. Most noteworthy among the additions are the extension of the computational spectroscopic database to include a number of significantly larger polycyclic aromatic hydrocarbons (PAHs), the ability to visualize the molecular atomic motions corresponding to each vibrational mode, and a new tool that allows one to perform a non-negative least-squares fit of an imported astronomical spectrum with PAH spectra in the computational database. Finally, a methodology is described in the Appendix, and implemented using the AmesPAHdbIDLSuite, that allows the user to enforce charge balance during the fitting procedure.

C. Boersma; C. W. Bauschlicher, Jr.; A. Ricca; A. L. Mattioda; J. Cami; E. Peeters; F. Snchez de Armas; G. Puerta Saborido; D. M. Hudgins; L. J. Allamandola

2014-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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.


241

Complex Hydrides - A New Frontier for Future Energy Applications - DOE Hydrogen and Fuel Cells Program FY 2012 Annual Progress Report  

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

5 5 FY 2012 Annual Progress Report DOE Hydrogen and Fuel Cells Program Vitalij K. Pecharsky, 1 Marek Pruski, 2 L. Scott Chumbley, 3 Duane D. Johnson, 4 Takeshi Kobayashi 5 1 FWP Leader: Ames Laboratory, 253 Spedding Hall, Ames, IA 50011, Email: vitkp@ameslab.gov, Phone: (515) 294-8220 2 PI: Ames Laboratory, 230 Spedding Hall, Ames, IA 50011, Email: mpruski@iastate.edu, Phone: (515) 294-2017 3 PI: Ames Laboratory, 214 Wilhelm Hall, Ames, IA 50011, Email: chumbley@iastate.edu, Tel.: 515-2947903; 4 PI: Ames Laboratory, 311 TASF, Ames, IA 50011, Email: ddj@ameslab.gov, Phone: (515) 2949649 5 Ames Laboratory, 229 Spedding Hall, Ames, IA 50011, Email: takeshi@iastate.edu, Phone: (515)-294-6823 DOE Program Officer: Dr. Refik Kortan

242

IA REP0 SAND85-2809 Unlimited Release UC-92A  

Office of Scientific and Technical Information (OSTI)

IA REP0 SAND85-2809 Unlimited Release UC-92A IA REP0 SAND85-2809 Unlimited Release UC-92A Printed July 1986 High Energy Gas Fracture Experiments in Fluid-Filled Boreholes-Potential Geothermal Application J. F. Cuderman, T. Y. Chu, J. Jung, R. D. Jacobson Prepared by Sandia National Laboratories Albuquerque, New Mexico 87 185 and Livermore, California 94550 for the United States Department of Energy under Contract DE-AC04-76DP00789 DISCLAIMER This report was prepared as an account of work sponsored by an agency of the United States Government. Neither the United States Government nor any agency Thereof, nor any of their employees, makes any warranty, express or implied, or assumes any legal liability or responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process

243

File:USDA-CE-Production-GIFmaps-IA.pdf | Open Energy Information  

Open Energy Info (EERE)

IA.pdf IA.pdf Jump to: navigation, search File File history File usage Iowa Ethanol Plant Locations Size of this preview: 776 × 600 pixels. Full resolution ‎(1,650 × 1,275 pixels, file size: 303 KB, MIME type: application/pdf) Description Iowa Ethanol Plant Locations Sources United States Department of Agriculture Related Technologies Biomass, Biofuels, Ethanol Creation Date 2010-01-19 Extent State Countries United States UN Region Northern America States Iowa External links http://www.nass.usda.gov/Charts_and_Maps/Ethanol_Plants/ File history Click on a date/time to view the file as it appeared at that time. Date/Time Thumbnail Dimensions User Comment current 16:13, 27 December 2010 Thumbnail for version as of 16:13, 27 December 2010 1,650 × 1,275 (303 KB) MapBot (Talk | contribs) Automated bot upload

244

Mechanistic studies of proton-coupled electron transfer in aminotyrosine- and fluorotyrosine- substituted class Ia Ribonucleotide reductase  

E-Print Network [OSTI]

Ribonucleotide reductase (RNR) catalyzes the conversion of nucleotides to 2'- deoxynucleotides in all organisms. The class Ia RNR from Escherichia coli is active as an a2p2 complex and utilizes an unprecedented mechanism ...

Minnihan, Ellen Catherine

2012-01-01T23:59:59.000Z

245

Generation of a stable, aminotyrosyl radical-induced ?2?2 complex of Escherichia coli class Ia ribonucleotide reductase  

E-Print Network [OSTI]

Ribonucleotide reductase (RNR) catalyzes the conversion of nucleoside diphosphates to deoxynucleoside diphosphates (dNDPs). The Escherichia coli class Ia RNR uses a mechanism of radical propagation by which a cysteine in ...

Minnihan, Ellen Catherine

246

IA --"-IScience Service Featuse 'I WHY T i E IJEAYIiER ?  

E-Print Network [OSTI]

No. 591 April 3 IA --"-IScience Service Featuse 'I WHY T i E IJEAYIiER ? II city located oa the Ice.pp';g a% Bidialo, The ice c h i l l s a t h i n laye:. of a i r aver the Sake aridto laewwd. NOW$ vhen r may be srrfficionl t o produce a sheet cloud and g i ~ eBuffalo a day not oalg dwnt arid chilly Lu

247

Especialista Universitario Java Enterprise 2010-2011 Depto. Ciencia de la Computacin e IA  

E-Print Network [OSTI]

Especialista Universitario Java Enterprise © 2010-2011 Depto. Ciencia de la Computación e IA Sesión 1: Introducción a JMS #12;Servicios de Mensajes con JMS © 2010-2011 Depto. Ciencia de la Computación · Una Aplicación JMS · PTP · Pub/Sub #12;Servicios de Mensajes con JMS © 2010-2011 Depto. Ciencia de la

Escolano, Francisco

248

On the Thermonuclear Runaway in Type Ia Supernovae: How to Run Away?  

Science Journals Connector (OSTI)

Type Ia supernovae (SNe Ia) are thought to be thermonuclear explosions of massive white dwarfs (WDs). We present the first study of multidimensional effects during the final hours prior to the thermonuclear runaway that leads to the explosion. The calculations utilize an implicit, two-dimensional hydrodynamic code. Mixing and the ignition process are studied in detail. We find that the initial chemical structure of the WD is changed, but the material is not fully homogenized. In particular, the exploding WD sustains a central region with a low C/O ratio. This implies that the explosive nuclear burning will begin in a partially carbon-depleted environment. The thermonuclear runaway happens in a well-defined region close to the center. It is induced by compressional heat when matter is brought inward by convective flows. We find no evidence for multiple spot or strong off-center ignition. Convective velocities in the WD are on the order of 100 km s-1, which is well above the effective burning speeds in SNe Ia previously expected right after the runaway. In our calculations, the ignition occurs near the center. Then, for ? 0.5-1 s, the speed of the burning front will neither be determined by the laminar speed nor the Rayleigh-Taylor instabilities but by convective flows produced prior to the runaway. The consequences are discussed for our understanding of the detailed physics of the flame propagation, the deflagration to detonation transition, and the nucleosynthesis in the central layers. Our results strongly suggest the preconditioning of the progenitor as a key factor for our understanding of the diversity in SNe Ia.

P. Hflich; J. Stein

2002-01-01T23:59:59.000Z

249

Testing the DistanceDuality Relation with Galaxy Clusters and Type Ia Supernovae  

Science Journals Connector (OSTI)

In this Letter, we propose a new and model-independent cosmological test for the distance-duality (DD) relation, ? = DL (z)(1 + z)2/DA (z) = 1, where DL and DA are, respectively, the luminosity and angular diameter distances. For DL we consider two sub-samples of Type Ia supernovae (SNe Ia) taken from Constitution data whereas DA distances are provided by two samples of galaxy clusters compiled by De Filippis etal. and Bonamente etal. by combining Sunyaev-Zeldovich effect and X-ray surface brightness. The SNe Ia redshifts of each sub-sample were carefully chosen to coincide with the ones of the associated galaxy cluster sample (?z DA (z) ? DL (z), we have tested the DD relation by assuming that ? is a function of the redshift parameterized by two different expressions: ?(z) = 1 + ?0 z and ?(z) = 1 + ?0 z/(1 + z), where ?0 is a constant parameter quantifying a possible departure from the strict validity of the reciprocity relation (?0 = 0). In the best scenario (linear parameterization), we obtain ?0 = 0.28+0.44 0.44 (2?, statistical + systematic errors) for the De Filippis etal. sample (elliptical geometry), a result only marginally compatible with the DD relation. However, for the Bonamente etal. sample (spherical geometry) the constraint is ?0 = 0.42+0.34 0.34 (3?, statistical + systematic errors), which is clearly incompatible with the duality-distance relation.

R. F. L. Holanda; J. A. S. Lima; M. B. Ribeiro

2010-01-01T23:59:59.000Z

250

Evaluation of copper for divider subassembly in MCO Mark IA and Mark IV scrap fuel baskets  

SciTech Connect (OSTI)

The K Basin Spent Nuclear Fuel (SNF) Project Multi-Canister Overpack (MCO) subprojection eludes the design and fabrication of a canister that will be used to confine, contain, and maintain fuel in a critically safe array to enable its removal from the K Basins, vacuum drying, transport, staging, hot conditioning, and interim storage (Goldinann 1997). Each MCO consists of a shell, shield plug, fuel baskets (Mark IA or Mark IV), and other incidental equipment. The Mark IA intact and scrap fuel baskets are a safety class item for criticality control and components necessary for criticality control will be constructed from 304L stainless steel. It is proposed that a copper divider subassembly be used in both Mark IA and Mark IV scrap baskets to increase the safety basis margin during cold vacuum drying. The use of copper would increase the heat conducted away from hot areas in the baskets out to the wall of the MCO by both radiative and conductive heat transfer means. Thus copper subassembly will likely be a safety significant component of the scrap fuel baskets. This report examines the structural, cost and corrosion consequences associated with using a copper subassembly in the stainless steel MCO scrap fuel baskets.

Graves, C.E.

1997-09-29T23:59:59.000Z

251

Observational constraints from SNe Ia and Gamma-Ray Bursts on a clumpy universe  

E-Print Network [OSTI]

The luminosity distance describing the effect of local inhomogeneities in the propagation of light proposed by Zeldovich-Kantowski-Dyer-Roeder (ZKDR) is tested with two probes for two distinct ranges of redshifts: supernovae Ia (SNe Ia) in 0.015 gamma-ray bursts (GRBs) in 1.547 < z < 3.57. Our analysis is performed by a Markov Chain Monte Carlo (MCMC) code that allows us to constrain the matter density parameter \\Omega_m as well as the smoothness parameter $\\alpha$ that measures the inhomogeneous-homogeneous rate of the cosmic fluid in a flat \\LambdaCDM model. The obtained best fits are (\\Omega_m=0.285^{+0.019}_{-0.018}, \\alpha= 0.856^{+0.106}_{-0.176}) from SNe Ia and (\\Omega_m=0.259^{+0.028}_{-0.028}, \\alpha=0.587^{+0.201}_{-0.202}) from GRBs, while from the joint analysis the best fits are (\\Omega_m=0.284^{+0.021}_{-0.020}, \\alpha= 0.685^{+0.164}_{-0.171}) with a \\chi^2_{\\rm red}=0.975. The value of the smoothness parameter $\\alpha$ indicates a clumped universe however it does not have an impact on the amount of dark energy (cosmological constant) needed to fit observations. This result may be an indication that the Dyer-Roeder approximation does not describe in a precise form the effects of clumpiness in the expansion of the universe.

Nora Bretn; Ariadna Montiel

2013-03-06T23:59:59.000Z

252

Especialista Universitario Java Enterprise Componentes de presentacin 2012-2013 Depto. Ciencia de la Computacin e IA Sesin 4  

E-Print Network [OSTI]

Especialista Universitario Java Enterprise Componentes de presentación © 2012-2013 Depto. Ciencia presentación © 2012-2013 Depto. Ciencia de la Computación e IA Sesión 4 Experto Universitario Java Enterprise Componentes de presentación © 2012-2013 Depto. Ciencia de la Computación e IA Sesión 4 Experto Universitario

Escolano, Francisco

253

Experto Universitario Java Enterprise Componentes de presentacin 2012-2013 Depto. Ciencia de la Computacin e IA Sesin 1  

E-Print Network [OSTI]

Experto Universitario Java Enterprise Componentes de presentación © 2012-2013 Depto. Ciencia de la Universitario Java Enterprise Componentes de presentación © 2012-2013 Depto. Ciencia de la Computación e IA Componentes de presentación © 2012-2013 Depto. Ciencia de la Computación e IA Sesión 1 Experto Universitario

Escolano, Francisco

254

Utilizing Type Ia Supernovae in a Large, Fast, Imaging Survey to Constrain Dark Energy  

Science Journals Connector (OSTI)

We study the utility of a large sample of Type Ia supernovae (SNe Ia) that might be observed in an imaging survey that rapidly scans a large fraction of the sky for constraining dark energy. We consider both the information contained in the traditional luminosity distance test as well as the spread in Ia SN fluxes at fixed redshift induced by gravitational lensing. As would be required from an imaging survey, we include a treatment of photometric redshift uncertainties in our analysis. Our primary result is that the information contained in the mean distance moduli of SNe Ia and the dispersion of SN Ia distance moduli complement each other, breaking a degeneracy between the present dark energy equation of state and its time variation without the need for a high-redshift (z 0.8) SN sample. Including lensing information also allows for some internal calibration of photometric redshifts. To address photometric redshift uncertainties, we present dark energy constraints as a function of the size of an external set of spectroscopically observed SNe that may be used for redshift calibration, N spec. Depending upon the details of potentially available, external SN data sets, we find that an imaging survey can constrain the dark energy equation of state at the epoch where it is best constrained w p, with a 1? error of ?(w p) ? 0.03-0.09. In addition, the marginal improvement in the error ?(w p) from an increase in the spectroscopic calibration sample drops once N spec ~ a few ? 103. This result is important because it is of the order of the size of calibration samples likely to be compiled in the coming decade and because, for samples of this size, the spectroscopic and imaging surveys individually place comparable constraints on the dark energy equation of state. In all cases, it is best to calibrate photometric redshifts with a set of spectroscopically observed SNe with relatively more objects at high redshift (z 0.5) than the parent sample of imaging SNe.

Andrew R. Zentner; Suman Bhattacharya

2009-01-01T23:59:59.000Z

255

levin | The Ames Laboratory  

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

of Education and the Ministry of Science and Technology, Lviv State University, Lviv, Ukraine, 1988 - 1998 Visiting Scientist (periodically) at the International Laboratory of...

256

nfang | The Ames Laboratory  

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

nanoparticles because they require no contact and make minimal intrusion to the sample Chemical and biological discovery through the development and use of a novel optical...

257

Committees | The Ames Laboratory  

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

Committees The Director has several standing and ad hoc committees including the Safety Review Committee (Kevin Dennis, Chair) Environmental Management System Steering Committee...

258

The Ames Laboratory  

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

515-294-2368 Naresh Eedugurala Grad Asst-RA 2236 Hach eedug1n@iastate.edu 515-294-6342 James Evans Associate 315 Wilhelm evans@ameslab.gov 515-294-1638 William Everett Grad...

259

antropov | The Ames Laboratory  

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

Ph.D. Condensed Matter Physics, Institute of Physics of Metals, Yekaterinburg, Russia, 1987 M. D. Theoretical Physics, Ural Polytechnical Institute, Yekaterinburg, Russia,...

260

The Ames Laboratory  

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

Kaitlin Bratlie Associate 2220 Hoover kbratlie@iastate.edu 515-294-7297 Serguei Budko Scientist I A111 Zaffarano budko@ameslab.gov 515-294-3986 David Byrd Asst Scientist I...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Directory | The Ames Laboratory  

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

294-4360 Director's Office 311 TASF 294-2770 Documents and Records 151 TASF 294-9972 Engineering Services 158 Metals Development 294-3757 Environment, Safety, Health &...

262

Purchasing | The Ames Laboratory  

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

Metals Office Supplies Scientific Equipment Software Services purchased: ArchitecturalEngineering Services Construction Equipment Repair and Maintenance Professional Analysis...

263

Video | The Ames Laboratory  

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

Video Solidification of LaNi5-xSnx in an plasmaarc furnace Arc casting of intermetallics may sound mundane, however, depending on the solidification behavior of the constituents...

264

Highlights | The Ames Laboratory  

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

valuable H2, while the other removes an atom of carbon and oxygen and produces carbon monoxide. Typically carbon monoxide inhibits the removal of hydrogen, but the use of...

265

The Ames Laboratory  

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

a group of mainland Chinese students who served as interpreters with the Chinese engineers installing the steam engine. You can read the full issue inside. Read Full Story...

266

Equipment | The Ames Laboratory  

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

Stanat Rolling Mill 75 Ton Wabash Platten Press Rotary Die Swaging Loma Hydraulic Wire Drawing Bench Innovare Hydrostatic Extrusion Press...

267

andersoi | The Ames Laboratory  

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

joining problems including lead-free solders, braze alloys, resistance welding, and ceramic composite bonding Honors & Awards: Iowa State University Intellectual Property Award,...

268

The Ames Laboratory  

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

Sunday, March 1, 2015 Prev Next Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 1 2 3 4...

269

The Ames Laboratory  

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

Thursday, January 1, 2015 Prev Next Sun Mon Tue Wed Thu Fri Sat 28 29 30 31 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31...

270

biswasr | The Ames Laboratory  

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

Design of photonic band gap crystals with electromagnetic simulations Light management in solar cell structures Sharp infrared emitters using photonic crystals Development of novel...

271

jonesll | The Ames Laboratory  

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

1991 Areas of Expertise: Preparation and purification of alkaline, refractory, and rare earth elements Development of high temperature melting and casting techniques for the...

272

Highlights | The Ames Laboratory  

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

researchers are able to trick iron into having magnetic properties like those of rare-earth elements.Rare-earth magnets are stronger than typical iron-based magnets and have high...

273

mark | The Ames Laboratory  

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

and on surfaces New methods for treating the effects of solvation, for interfacing electronic structure calculations with dynamics, for obtaining accurate wave functions and...

274

The Ames Laboratory  

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

Rhonda Deshong Program Asst II 105 TASF deshong@ameslab.gov 515-294-0931 Amy Harris-Tehan Program Coord III 151 TASF ajotehan@ameslab.gov 515-294-1376 Rhonda Hill Clerk...

275

Publications | The Ames Laboratory  

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

"Approaching quantum criticality in a partially geometrically frustrated heavy-fermion metal," Physical Review B89 (5), 054416 (2014). 6 C. L. Wang, J. D. Zou, J. Liu, Y. Mudryk,...

276

Education | The Ames Laboratory  

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

The MFRC has established a network of Midwest crime laboratories and university-based forensic science programs. This network has two general goals: help universities become better...

277

Projects | The Ames Laboratory  

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

for Tool Mark Characterization Development of an AccuTOF-DART Database for Use by Forensic Laboratories Forensic Technology Center of Excellence MFRC Training Development &...

278

Training | The Ames Laboratory  

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

Advanced Bloodstain Pattern Analysis Workshop Dates: March 31-April 4, 2014 Northeast Forensic Training Center, Bethlehem, Pennsylvania Instructors: Toby Wolson, MS and LeeAnn...

279

chumbley | The Ames Laboratory  

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

microscopy techniques for K-12 education Characterization of tool marked surfaces for forensic applications Instructor of undergraduate and graduate courses in electron microscopy...

280

Overview | The Ames Laboratory  

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

Resource Center (MFRC), work to provide resources to improve the practice of forensic science through our programs in Casework Assistance, Training, Education, Research,...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

CIMAT, VI Escuela de verano, 25 de julio 7 de agosto 1999 Introducci'on a la Geometr'ia de la Mec'anica Cl'asica  

E-Print Network [OSTI]

parametrizada por (x(t); ?? x(t)): (d) Dibujar las gr'aficas de su energ'ia cin'etica T = ( ?? x) 2 =2 y potencial­ vaci'on de energ'ia, E = T + V = constante: (e) Repetir los 4 incisos anteriores con x(1) = 2; ?? x(0CIMAT, VI Escuela de verano, 25 de julio ­ 7 de agosto 1999 Introducci'on a la Geometr'ia de la Mec

Bor, Gil

282

CIMAT, VI Escuela de verano, 25 de julio -7 de agosto 1999 Introducci'on a la Geometr'ia de la Mec'anica Cl'asica  

E-Print Network [OSTI]

(t), `x(t)). (d)Dibujar las gr'aficas de su energ'ia cin'etica T = (x`)2=2 y potencial* * V = x2- vaci'on de energ'ia, E = T + V = constante. (e)Repetir los 4 incisos anteriores con x(1) = 2, `x CIMAT, VI Escuela de verano, 25 de julio - 7 de agosto 1999 Introducci'on a la Geometr'ia de la

Bor, Gil

283

Study of the Detonation Phase in the Gravitationally Confined Detonation Model of Type Ia Supernovae  

Science Journals Connector (OSTI)

We study the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia) through the detonation phase and into homologous expansion. In the GCD model, a detonation is triggered by the surface flow due to single-point, off-center flame ignition in carbon-oxygen white dwarfs (WDs). The simulations are unique in terms of the degree to which nonidealized physics is used to treat the reactive flow, including weak reaction rates and a time-dependent treatment of material in nuclear statistical equilibrium (NSE). Careful attention is paid to accurately calculating the final composition of material which is burned to NSE and frozen out in the rapid expansion following the passage of a detonation wave over the high-density core of the WD; and an efficient method for nucleosynthesis postprocessing is developed which obviates the need for costly network calculations along tracer particle thermodynamic trajectories. Observational diagnostics are presented for the explosion models, including abundance stratifications and integrated yields. We find that for all of the ignition conditions studied here a self-regulating process comprised of neutronization and stellar expansion results in final 56Ni masses of ~1.1M ?. But, more energetic models result in larger total NSE and stable Fe-peak yields. The total yield of intermediate mass elements is ~0.1M ? and the explosion energies are all around 1.5 ? 1051 erg. The explosion models are briefly compared to the inferred properties of recent SN Ia observations. The potential for surface detonation models to produce lower-luminosity (lower 56Ni mass) SNe is discussed.

Casey A. Meakin; Ivo Seitenzahl; Dean Townsley; George C. Jordan IV; James Truran; Don Lamb

2009-01-01T23:59:59.000Z

284

IS WX CEN A POSSIBLE TYPE Ia SUPERNOVA PROGENITOR WITH WIND-DRIVEN MASS TRANSFER?  

SciTech Connect (OSTI)

WX Cen is one of a few compact binary supersoft X-ray sources (CBSS) in the Galaxy that is a possible Type Ia supernova (SN Ia) progenitor. The supersoft X-ray radiation is explained as hydrostatic nuclear burning on the surface of the white dwarf component that is accreting hydrogen from a stellar companion at a high rate. If the mass donor in this system has a low mass, as has been suggested in the literature, one would expect a high wind-driven mass transfer rate. In that case, the orbital period of the system should increase. To test this theoretical prediction, we have monitored the system photometrically since 2010. By using four newly determined eclipse timings together with those collected from the literature, we discovered that the orbital period is decreasing at a rate of dP/dt = -5.15 Multiplication-Sign 10{sup -7} days yr{sup -1}. The long-term decrease in the orbital period is contrary to the prediction that the system is powered by wind-driven accretion. It therefore seems plausible that the mass donor could be more massive than the white dwarf, and that the mass transfer is driven by the thermal instability of the donor star. This finding suggests that WX Cen is a key object to check the physical mechanisms of mass accretion in CBSS. The corresponding timescale of the period change is about P/P-dot {approx} 0.81 x 10{sup 6} yr, indicating that WX Cen may evolve into an SNe Ia within one million years in the Galaxy.

Qian, S.-B.; Shi, G.; Zhu, L.-Y.; Liu, L.; Zhao, E.-G.; Li, L.-J. [Yunnan Observatories, Chinese Academy of Sciences (CAS), P.O. Box 110, 650011 Kunming (China); Fernandez Lajus, E.; Di Sisto, R. P., E-mail: qsb@ynao.ac.cn [Facultad de Ciencias Astronomicas y Geofisicas, Universidad Nacional de La Plata, 1900 La Plata, Buenos Aires (Argentina)

2013-08-01T23:59:59.000Z

285

On the Thermonuclear Runaway in Type Ia Supernovae: How to run away?  

E-Print Network [OSTI]

Type Ia Supernovae are thought to be thermonuclear explosions of massive white dwarfs (WD). We present the first study of multi-dimensional effects during the final hours prior to the thermonuclear runaway which leads to the explosion. The calculations utilize an implicit, 2-D hydro code.Mixing and the ignition process are studied in detail. We find that the initial chemical structure of the WD is changed but the material is not fully homogenized. The exploding WD sustains a central region with a low C/O ratio. This implies that the explosive nuclear burning will begin in a partially C-depleted environment. The thermonuclear runaway happens in a well defined region close to the center. It is induced by compressional heat when matter is brought inwards by convective flows. We find no evidence for multiple spot or strong off-center ignition. Convective velocities are of the order of 100 km/sec which is well above the effective burning speeds in SNe Ia previously expected right after the runaway. For about 0.5 to 1 sec, the speed of the burning front will neither be determined by the laminar speed nor the Rayleigh-Taylor instabilities but by convective flows produced prior to the runaway. The consequences are discussed for our under- standing of the detailed physics of the flame propagation, the deflagration detonation transition, and the nucleosynthesis in the central layers. Our results strongly suggest the pre-conditioning of the progenitor as a key-factor for our understanding of the diversity in SNeIa.

P. Hoeflich; J. Stein

2001-12-07T23:59:59.000Z

286

Reconstruction of Hessence Dark Energy and the Latest Type Ia Supernovae Gold Dataset  

E-Print Network [OSTI]

Recently, many efforts have been made to build dark energy models whose equation-of-state parameter can cross the so-called phantom divide $w_{de}=-1$. One of them is the so-called hessence dark energy model in which the role of dark energy is played by a non-canonical complex scalar field. In this work, we develop a simple method based on Hubble parameter $H(z)$ to reconstruct the hessence dark energy. As examples, we use two familiar parameterizations for $H(z)$ and fit them to the latest 182 type Ia supernovae Gold dataset. In the reconstruction, measurement errors are fully considered.

Hao Wei; Ningning Tang; Shuang Nan Zhang

2007-02-28T23:59:59.000Z

287

Reconstruction of a Deceleration Parameter from the Latest Type Ia Supernovae Gold Dataset  

E-Print Network [OSTI]

In this paper, a parameterized deceleration parameter $q(z)= 1/2 - a/(1 + z)^b$ is reconstructed from the latest type Ia supernovae gold dataset. It is found out that the transition redshift from decelerated expansion to accelerated expansion is at $z_T=0.35^{+0.14}_{-0.07}$ with $1\\sigma$ confidence level in this parameterized deceleration parameter. And, the best fit values of parameters in $1\\sigma$ errors are $a=1.56^{+0.99}_{-0.55}$ and $b=3.82^{+3.70}_{-2.27}$.

Lixin Xu; Chengwu Zhang; Baorong Chang; Hongya Liu

2007-01-17T23:59:59.000Z

288

On the Stability of Thermonuclear Burning Fronts in Type Ia Supernovae  

E-Print Network [OSTI]

The propagation of cellularly stabilized thermonuclear flames is investigated by means of numerical simulations. In Type Ia supernova explosions the corresponding burning regime establishes at scales below the Gibson length. The cellular flame stabilization - which is a result of an interplay between the Landau-Darrieus instability and a nonlinear stabilization mechanism - is studied for the case of propagation into quiescent fuel as well as interaction with vortical fuel flows. Our simulations indicate that in thermonuclear supernova explosions stable cellular flames develop around the Gibson scale and that deflagration-to-detonation transition is unlikely to be triggered from flame evolution effects here.

F. K. Roepke; W. Hillebrandt

2004-04-26T23:59:59.000Z

289

Unbiased Estimate of Dark Energy Density from Type Ia Supernova Data  

Science Journals Connector (OSTI)

Type Ia supernovae (SNe Ia) are currently the best probes of the dark energy in the universe. To constrain the nature of dark energy, we assume a flat universe and that the weak energy condition is satisfied, and we allow the density of dark energy, ?X(z), to be an arbitrary function of redshift. Using simulated data from a space-based SN pencil-beam survey, we find that by optimizing the number of parameters used to parameterize the dimensionless dark energy density, f(z) = ?X(z)/?X(z = 0), we can obtain an unbiased estimate of both f(z) and the fractional matter density of the universe, ?m. A plausible SN pencil-beam survey (with a square degree field of view and for an observational duration of 1 yr) can yield about 2000 SNe Ia with 0 ? z ? 2. Such a survey in space would yield SN peak luminosities with a combined intrinsic and observational dispersion of ?(mint) = 0.16 mag. We find that for such an idealized survey, ?m can be measured to 10% accuracy, and the dark energy density can be estimated to ~20% to z ~ 1.5, and ~20%-40% to z ~ 2, depending on the time dependence of the true dark energy density. Dark energy densities that vary more slowly can be more accurately measured. For the anticipated Supernova/Acceleration Probe (SNAP) mission, ?m can be measured to 14% accuracy, and the dark energy density can be estimated to ~20% to z ~ 1.2. Our results suggest that SNAP may gain much sensitivity to the time dependence of the dark energy density and ?m by devoting more observational time to the central pencil-beam fields to obtain more SNe Ia at z > 1.2. We use both a maximum likelihood analysis and a Monte Carlo analysis (when appropriate) to determine the errors of estimated parameters. We find that the Monte Carlo analysis gives a more accurate estimate of the dark energy density than the maximum likelihood analysis.

Yun Wang; Geoffrey Lovelace

2001-01-01T23:59:59.000Z

290

One-dimensional delayed-detonation models of Type Ia supernovae: Confrontation to observations at bolometric maximum  

E-Print Network [OSTI]

The delayed-detonation explosion mechanism applied to a Chandrasekhar-mass white dwarf offers a very attractive model to explain the inferred characteristics of Type Ia supernovae (SNe Ia). The resulting ejecta are chemically stratified, have the same mass and roughly the same asymptotic kinetic energy, but exhibit a range in 56Ni mass. We investigate the contemporaneous photometric and spectroscopic properties of a sequence of delayed-detonation models, characterized by 56Ni masses between 0.18 and 0.81 Msun. Starting at 1d after explosion, we perform the full non-LTE, time-dependent radiative transfer with the code CMFGEN, with an accurate treatment of line blanketing, and compare our results to SNe Ia at bolometric maximum. Despite the 1D treatment, our approach delivers an excellent agreement to observations. We recover the range of SN Ia luminosities, colours, and spectral characteristics from the near-UV to 1 micron, for standard as well as low-luminosity 91bg-like SNe Ia. Our models predict an increase...

Blondin, Stphane; Hillier, D John; Khokhlov, Alexei M

2012-01-01T23:59:59.000Z

291

The p-Process in the Carbon Deflagration Model for Type Ia Supernovae and Chronology of the Solar System Formation  

SciTech Connect (OSTI)

We study nucleosynthesis of p-nuclei in the carbon deflagration model for Type Ia supernovae (SNe Ia) by assuming that seed nuclei are produced by the s-process in accreting layers on a carbon-oxygen white dwarf during mass accretion from a binary companion. We find that about 50 % of the p-nuclides are synthesized in proportion to the solar abundance and that p-isotopes of Mo and Ru which are significantly underproduced in Type II supernovae (SNe II) are produced up to a level close to other p-nuclei. Comparing the yields of iron and p-nuclei in SNe Ia we find that SNe Ia can contribute to the galactic evolution of the p-nuclei. Next, we consider nucleochronology of the solar system formation by using four radioactive nuclides and apply the result of the p-process nucleosynthesis to simple galactic chemical evolution models. We find that when assumed three phases of interstellar medium are mixed by the interdiffusion with the timescale of about 40 Myr 53Mn/55Mn value in the early solar system is consistent with a meteoritic value. In addition, we put constraints to a scenario that SNe Ia induce the core collapse of the molecular cloud, which leads to the formation of the solar system.

Kusakabe, Motohiko [Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan); National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan); Iwamoto, Nobuyuki [Japan Atomic Energy Agency, Tokai, Ibaraki 319-1195 (Japan); Nomoto, Ken'ichi [Department of Astronomy, School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033 (Japan)

2006-07-12T23:59:59.000Z

292

Stable isotope-assisted NMR characterization of interaction between lipid A and sarcotoxin IA, a cecropin-type antibacterial peptide  

SciTech Connect (OSTI)

Highlights: ? Recombinant sarcotoxin IA was successfully produced with {sup 13}C- and {sup 15}N-labeling. ? Sarcotoxin IA adopts an N-terminal ?-helix upon binding to lipid A-embedding micelles. ? Two lysine residues are involved in lipid A-mediated antibacterial activities. -- Abstract: Sarcotoxin IA is a 39-residue cecropin-type peptide from Sarcophaga peregrina. This peptide exhibits antibacterial activity against Gram-negative bacteria through its interaction with lipid A, a core component of lipopolysaccharides. To acquire detailed structural information on this specific interaction, we performed NMR analysis using bacterially expressed sarcotoxin IA analogs with {sup 13}C- and {sup 15}N-labeling along with lipid A-embedding micelles composed of dodecylphosphocholine. By inspecting the stable isotope-assisted NMR data, we revealed that the N-terminal segment (Leu3Arg18) of sarcotoxin IA formed an amphiphilic ?-helix upon its interaction with the aqueous micelles. Furthermore, chemical shift perturbation data indicated that the amino acid residues displayed on this ?-helix were involved in the specific interaction with lipid A. On the basis of these data, we successfully identified Lys4 and Lys5 as key residues in the interaction with lipid A and the consequent antibacterial activity. Therefore, these results provide unique information for designing chemotherapeutics based on antibacterial peptide structures.

Yagi-Utsumi, Maho [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan) [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan); Graduate School of Pharmaceutical Sciences, Nagoya City University, Nagoya 467-8603 (Japan); Yamaguchi, Yoshiki [Graduate School of Pharmaceutical Sciences, Nagoya City University, Nagoya 467-8603 (Japan) [Graduate School of Pharmaceutical Sciences, Nagoya City University, Nagoya 467-8603 (Japan); Advanced Science Institute, RIKEN, Wako 351-0198 (Japan); Boonsri, Pornthip [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan) [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan); Department of Chemistry, Faculty of Science, Kasetsart University, Bangkok 10900 (Thailand); Iguchi, Takeshi [Bioscience Research Laboratory, Fujiya Co., Ltd., Hadano, Kanagawa 257-0031 (Japan)] [Bioscience Research Laboratory, Fujiya Co., Ltd., Hadano, Kanagawa 257-0031 (Japan); Okemoto, Kazuo [Department of Biochemistry and Cell Biology, National Institute of Infectious Disease, Tokyo 162-8640 (Japan)] [Department of Biochemistry and Cell Biology, National Institute of Infectious Disease, Tokyo 162-8640 (Japan); Natori, Shunji [National Institute of Agrobiological Sciences, Tsukuba 305-8602 (Japan)] [National Institute of Agrobiological Sciences, Tsukuba 305-8602 (Japan); Kato, Koichi, E-mail: kkatonmr@ims.ac.jp [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan) [Institute for Molecular Science and Okazaki Institute for Integrative Bioscience, National Institutes of Natural Sciences, Okazaki 444-8787 (Japan); Graduate School of Pharmaceutical Sciences, Nagoya City University, Nagoya 467-8603 (Japan); The Glycoscience Institute, Ochanomizu University, Tokyo 135-0064 (Japan); GLYENCE Co., Ltd., Nagoya 474-0858 (Japan)

2013-02-08T23:59:59.000Z

293

Inference for the dark energy equation of state using Type IA supernova data  

E-Print Network [OSTI]

The surprising discovery of an accelerating universe led cosmologists to posit the existence of "dark energy"--a mysterious energy field that permeates the universe. Understanding dark energy has become the central problem of modern cosmology. After describing the scientific background in depth, we formulate the task as a nonlinear inverse problem that expresses the comoving distance function in terms of the dark-energy equation of state. We present two classes of methods for making sharp statistical inferences about the equation of state from observations of Type Ia Supernovae (SNe). First, we derive a technique for testing hypotheses about the equation of state that requires no assumptions about its form and can distinguish among competing theories. Second, we present a framework for computing parametric and nonparametric estimators of the equation of state, with an associated assessment of uncertainty. Using our approach, we evaluate the strength of statistical evidence for various competing models of dark energy. Consistent with current studies, we find that with the available Type Ia SNe data, it is not possible to distinguish statistically among popular dark-energy models, and that, in particular, there is no support in the data for rejecting a cosmological constant. With much more supernova data likely to be available in coming years (e.g., from the DOE/NASA Joint Dark Energy Mission), we address the more interesting question of whether future data sets will have sufficient resolution to distinguish among competing theories.

Christopher Genovese; Peter Freeman; Larry Wasserman; Robert Nichol; Christopher Miller

2008-05-27T23:59:59.000Z

294

Flame-driven deflagration-to-detonation transitions in Type Ia supernovae?  

E-Print Network [OSTI]

Although delayed detonation models of thermonuclear explosions of white dwarfs seem promising for reproducing Type Ia supernovae, the transition of the flame propagation mode from subsonic deflagration to supersonic detonation remains hypothetical. A potential instant for this transition to occur is the onset of the distributed burning regime, i.e. the moment when turbulence first affects the internal flame structure. Some studies of the burning microphysics indicate that a deflagration-to-detonation transition may be possible here, provided the turbulent intensities are strong enough. Consequently, the magnitude of turbulent velocity fluctuations generated by the deflagration flame is analyzed at the onset of the distributed burning regime in several three-dimensional simulations of deflagrations in thermonuclear supernovae. It is shown that the corresponding probability density functions fall off towards high turbulent velocity fluctuations much more slowly than a Gaussian distribution. Thus, values claimed to be necessary for triggering a detonation are likely to be found in sufficiently large patches of the flame. Although the microphysical evolution of the burning is not followed and a successful deflagration-to-detonation transition cannot be guaranteed from simulations presented here, the results still indicate that such events may be possible in Type Ia supernova explosions.

F. K. Roepke

2007-09-26T23:59:59.000Z

295

Flame Evolution During Type Ia Supernovae and the Deflagration Phase in the Gravitationally Confined Detonation Scenario  

E-Print Network [OSTI]

We develop an improved method for tracking the nuclear flame during the deflagration phase of a Type Ia supernova, and apply it to study the variation in outcomes expected from the gravitationally confined detonation (GCD) paradigm. A simplified 3-stage burning model and a non-static ash state are integrated with an artificially thickened advection-diffusion-reaction (ADR) flame front in order to provide an accurate but highly efficient representation of the energy release and electron capture in and after the unresolvable flame. We demonstrate that both our ADR and energy release methods do not generate significant acoustic noise, as has been a problem with previous ADR-based schemes. We proceed to model aspects of the deflagration, particularly the role of buoyancy of the hot ash, and find that our methods are reasonably well-behaved with respect to numerical resolution. We show that if a detonation occurs in material swept up by the material ejected by the first rising bubble but gravitationally confined to the white dwarf (WD) surface (the GCD paradigm), the density structure of the WD at detonation is systematically correlated with the distance of the deflagration ignition point from the center of the star. Coupled to a suitably stochastic ignition process, this correlation may provide a plausible explanation for the variety of nickel masses seen in Type Ia Supernovae.

D. M. Townsley; A. C. Calder; S. M. Asida; I. R. Seitenzahl; F. Peng; N. Vladimirova; D. Q. Lamb; J. W. Truran

2007-06-07T23:59:59.000Z

296

Constraining a bulk viscous matter-dominated cosmological model using SNe Ia, CMB and LSS  

E-Print Network [OSTI]

We present and constrain a cosmological model which component is a pressureless fluid with bulk viscosity as an explanation for the present accelerated expansion of the universe. We study the particular model of a constant bulk viscosity coefficient \\zeta_m. The possible values of \\zeta_m are constrained using the cosmological tests of SNe Ia Gold 2006 sample, the CMB shift parameter R from the three-year WMAP observations, the Baryon Acoustic Oscillation (BAO) peak A from the Sloan Digital Sky Survey (SDSS) and the Second Law of Thermodynamics (SLT). It was found that this model is in agreement with the SLT using only the SNe Ia test. However when the model is submitted to the three cosmological tests together (SNe+CMB+BAO) the results are: 1.- the model violates the SLT, 2.- predicts a value of H_0 \\approx 53 km sec^{-1} Mpc^{-1} for the Hubble constant, and 3.- we obtain a bad fit to data with a \\chi^2_{min} \\approx 400 (\\chi^2_{d.o.f.} \\approx 2.2). These results indicate that this model is ruled out by the observations.

Arturo Avelino; U. Nucamendi; F. S. Guzmn

2008-01-10T23:59:59.000Z

297

Parametrizing the transition to the phantom epoch with Supernovae Ia and Standard Rulers  

E-Print Network [OSTI]

The properties of some particular parametrizations of the dark energy Equation of State (EoS) are studied by using Supernovae Ia data (HST Cluster Supernova Survey) combined with Standard Ruler datasets (Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillations (BAO)). In this sense, we propose some parametrizations that may present a (fast) transition to a phantom dark energy EoS (where $w_{DE}<-1$) and compare the results with the $\\Lambda$CDM model. The best fit of the models is obtained by using Sne Ia and Standard Ruler datasets, which provides some information about whether the phantom transition may be supported by the observations. In this regard, the crossing of the phantom barrier is allowed statistically but the occurrence of a future singularity seems unlikely. Furthermore, the reconstruction of a (non-)canonical scalar field Lagrangian from the EoS parameter is studied, where shown that EoS parametrizations can be well reconstructed in terms of scalar fields.

Leanizbarrutia, Iker

2014-01-01T23:59:59.000Z

298

Verifying the Cosmological Utility of Type Ia Supernovae:Implications of a Dispersion in the Ultraviolet Spectra  

SciTech Connect (OSTI)

We analyze the mean rest-frame ultraviolet (UV) spectrum ofType Ia Supernovae(SNe) and its dispersion using high signal-to-noiseKeck-I/LRIS-B spectroscopyfor a sample of 36 events at intermediateredshift (z=0.5) discoveredby the Canada-France-Hawaii TelescopeSupernova Legacy Survey (SNLS). Weintroduce a new method for removinghost galaxy contamination in our spectra,exploiting the comprehensivephotometric coverage of the SNLS SNe and theirhost galaxies, therebyproviding the first quantitative view of the UV spectralproperties of alarge sample of distant SNe Ia. Although the mean SN Ia spectrumhas notevolved significantly over the past 40 percent of cosmic history,preciseevolutionary constraints are limited by the absence of acomparable sample ofhigh quality local spectra. The mean UV spectrum ofour z 0.5 SNe Ia and itsdispersion is tabulated for use in futureapplications. Within the high-redshiftsample, we discover significant UVspectral variations and exclude dust extinctionas the primary cause byexamining trends with the optical SN color. Although progenitormetallicity may drive some of these trends, the variations we see aremuchlarger than predicted in recent models and do not follow expectedpatterns.An interesting new result is a variation seen in the wavelengthof selected UVfeatures with phase. We also demonstrate systematicdifferences in the SN Iaspectral features with SN lightcurve width inboth the UV and the optical. Weshow that these intrinsic variations couldrepresent a statistical limitation in thefuture use of high-redshift SNeIa for precision cosmology. We conclude thatfurther detailed studies areneeded, both locally and at moderate redshift wherethe rest-frame UV canbe studied precisely, in order that future missions canconfidently beplanned to fully exploit SNe Ia as cosmological probes.

Ellis, R.S.; Sullivan, M.; Nugent, P.E.; Howell, D.A.; Gal-Yam,A.; Astier, P.; Balam, D.; Balland, C.; Basa, S.; Carlberg, R.G.; Conley,A.; Fouchez, D.; Guy, J.; Hardin, D.; Hook, I.; Pain, R.; Perrett, K.; Pritchet, C.J.; Regnault, N.

2007-11-02T23:59:59.000Z

299

CIMAT, VIII Escuela de verano, 30 de julio -10 de ago* Introducci'on a la Geometr'ia de la Mec'ani*  

E-Print Network [OSTI]

conservativo. 18.Sea A(E) el 'area dentro de una curva de fase cerrada que corresponde a nive* *l de energ'ia Introducci'on a la Geometr'ia de la Mec'ani* *ca Cl'asica Problemas 13 - 19

Bor, Gil

300

LATE-TIME SPECTRAL OBSERVATIONS OF THE STRONGLY INTERACTING TYPE Ia SUPERNOVA PTF11kx  

SciTech Connect (OSTI)

PTF11kx was a Type Ia supernova (SN Ia) that showed time-variable absorption features, including saturated Ca II H and K lines that weakened and eventually went into emission. The strength of the emission component of H{alpha} gradually increased, implying that the SN was undergoing significant interaction with its circumstellar medium (CSM). These features, and many others, were blueshifted slightly and showed a P-Cygni profile, likely indicating that the CSM was directly related to, and probably previously ejected by, the progenitor system itself. These and other observations led Dilday et al. to conclude that PTF11kx came from a symbiotic nova progenitor like RS Oph. In this work we extend the spectral coverage of PTF11kx to 124-680 rest-frame days past maximum brightness. The late-time spectra of PTF11kx are dominated by H{alpha} emission (with widths of full width at half-maximum intensity Almost-Equal-To 2000 km s{sup -1}), strong Ca II emission features ({approx}10,000 km s{sup -1} wide), and a blue 'quasi-continuum' due to many overlapping narrow lines of Fe II. Emission from oxygen, He I, and Balmer lines higher than H{alpha} is weak or completely absent at all epochs, leading to large observed H{alpha}/H{beta} intensity ratios. The H{alpha} emission appears to increase in strength with time for {approx}1 yr, but it subsequently decreases significantly along with the Ca II emission. Our latest spectrum also indicates the possibility of newly formed dust in the system as evidenced by a slight decrease in the red wing of H{alpha}. During the same epochs, multiple narrow emission features from the CSM temporally vary in strength. The weakening of the H{alpha} and Ca II emission at late times is possible evidence that the SN ejecta have overtaken the majority of the CSM and agrees with models of other strongly interacting SNe Ia. The varying narrow emission features, on the other hand, may indicate that the CSM is clumpy or consists of multiple thin shells.

Silverman, Jeffrey M. [Department of Astronomy, University of Texas, Austin, TX 78712-0259 (United States); Nugent, Peter E.; Filippenko, Alexei V.; Cenko, S. Bradley [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); Gal-Yam, Avishay [Benoziyo Center for Astrophysics, The Weizmann Institute of Science, Rehovot 76100 (Israel); Sullivan, Mark [School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ (United Kingdom); Howell, D. Andrew [Las Cumbres Observatory Global Telescope Network, Goleta, CA 93117 (United States); Pan, Yen-Chen; Hook, Isobel M., E-mail: jsilverman@astro.as.utexas.edu [Department of Physics (Astrophysics), University of Oxford, Keble Road, Oxford OX1 3RH (United Kingdom)

2013-08-01T23:59:59.000Z

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301

Type Ia supernova diversity: white dwarf central density as a secondary parameter in three-dimensional delayed detonation models  

Science Journals Connector (OSTI)

......function of redshift. The standard model of SNe Ia relies on the nuclear fusion of the initial composition (predominantly 12C and 16O) of...generated from a Monte Carlo based algorithm. The primary input parameters are the number of the ignition kernels and the......

I. R. Seitenzahl; F. Ciaraldi-Schoolmann; F. K. Rpke

2011-07-01T23:59:59.000Z

302

EARLY RADIO AND X-RAY OBSERVATIONS OF THE YOUNGEST NEARBY TYPE Ia SUPERNOVA PTF 11kly (SN 2011fe)  

SciTech Connect (OSTI)

On 2011 August 24 (UT) the Palomar Transient Factory (PTF) discovered PTF11kly (SN 2011fe), the youngest and most nearby Type Ia supernova (SN Ia) in decades. We followed this event up in the radio (centimeter and millimeter bands) and X-ray bands, starting about a day after the estimated explosion time. We present our analysis of the radio and X-ray observations, yielding the tightest constraints yet placed on the pre-explosion mass-loss rate from the progenitor system of this supernova. We find a robust limit of M-dot {approx}<10{sup -8}(w/100 km s{sup -1}) M{sub sun} yr{sup -1} from sensitive X-ray non-detections, as well as a similar limit from radio data, which depends, however, on assumptions about microphysical parameters. We discuss our results in the context of single-degenerate models for SNe Ia and find that our observations modestly disfavor symbiotic progenitor models involving a red giant donor, but cannot constrain systems accreting from main-sequence or sub-giant stars, including the popular supersoft channel. In view of the proximity of PTF11kly and the sensitivity of our prompt observations, we would have to wait for a long time (a decade or longer) in order to more meaningfully probe the circumstellar matter of SNe Ia.

Horesh, Assaf; Kulkarni, S. R.; Carpenter, John; Kasliwal, Mansi M.; Ofek, Eran O. [Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA 91125 (United States); Fox, Derek B. [Astronomy and Astrophysics, Eberly College of Science, Pennsylvania State University, University Park, PA 16802 (United States); Quimby, Robert [IPMU, University of Tokyo, Kashiwanoha 5-1-5, Kashiwa-shi, Chiba (Japan); Gal-Yam, Avishay [Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, Rehovot 76100 (Israel); Cenko, S. Bradley [Department of Astronomy, University of California, Berkeley, CA 94720-3411 (United States); De Bruyn, A. G. [Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, NL-7990 AA Dwingeloo (Netherlands); Kamble, Atish; Wijers, Ralph A. M. J. [Center for Gravitation and Cosmology, University of Wisconsin, Milwaukee, WI 53211 (United States); Van der Horst, Alexander J. [Universities Space Research Association, NSSTC, Huntsville, AL 35805 (United States); Kouveliotou, Chryssa [Space Science Office, VP-62, NASA-Marshall Space Flight Center, Huntsville, AL 35805 (United States); Podsiadlowski, Philipp; Sullivan, Mark; Maguire, Kate [Department of Physics (Astrophysics), University of Oxford, Keble Road, Oxford OX1 3RH (United Kingdom); Howell, D. Andrew [Las Cumbres Observatory Global Telescope Network, Santa Barbara, CA 93117 (United States); Nugent, Peter E. [Computational Cosmology Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720 (United States); Gehrels, Neil [NASA-Goddard Space Flight Center, Greenbelt, MD 20771 (United States); and others

2012-02-10T23:59:59.000Z

303

Experto Universitario Java Enterprise Validacin e internacionalizacin 2012-2013 Depto. Ciencia de la Computacin e IA Spring  

E-Print Network [OSTI]

Experto Universitario Java Enterprise Validación e internacionalización © 2012-2013 Depto. Ciencia #12;Experto Universitario Java Enterprise Validación e internacionalización © 2012-2013 Depto. Ciencia Java Enterprise Validación e internacionalización © 2012-2013 Depto. Ciencia de la Computación e IA

Escolano, Francisco

304

TheThe ScienceScience ForumForum (as I(as I picturepicture itit)) Scholarly work  

E-Print Network [OSTI]

#12;Robotics TheThe ScienceScience ForumForum (as I(as I picturepicture itit)) Humanities Scholarly of photonics, robotics, telematics, dynamic physical rendering and intelligent sensors served as the basis to inspire four bestselling authors. The results are four short stories which paint amusing, thought

Torras, Carme

305

EXCELLENTIA CoLumbIA ENgINEErINg66 echanical engineers think about the design, construction, material proper-  

E-Print Network [OSTI]

responsibility for understanding how engines work, how buildings can be more efficiently built, and howHEALTH EXCELLENTIA CoLumbIA ENgINEErINg66 M echanical engineers think about the design the environment affects bridge architecture. They also apply their knowledge to the workings of the human body

Hone, James

306

ANALYSIS OF LIMIT CYCLE STABILITY IN A TAP-CHANGING TRANSFORMER V. Donde I.A. Hiskens  

E-Print Network [OSTI]

ANALYSIS OF LIMIT CYCLE STABILITY IN A TAP-CHANGING TRANSFORMER V. Donde I.A. Hiskens Department of transformer tap changing and load dynamics. Lin- earization of a Poincar´e map is used to prove local of the region of attraction can then be obtained. 1. INTRODUCTION Interactions between tap-changing transformers

Hiskens, Ian A.

307

A Precision Photometric Comparison between SDSS-II and CSP Type Ia Supernova Data  

E-Print Network [OSTI]

Consistency between Carnegie Supernova Project (CSP) and SDSS-II supernova (SN) survey ugri measurements has been evaluated by comparing SDSS and CSP photometry for nine spectroscopically confirmed Type Ia supernova observed contemporaneously by both programs. The CSP data were transformed into the SDSS photometric system. Sources of systematic uncertainty have been identified, quantified, and shown to be at or below the 0.023 magnitude level in all bands. When all photometry for a given band is combined, we find average magnitude differences of equal to or less than 0.011 magnitudes in ugri, with rms scatter ranging from 0.043 to 0.077 magnitudes. The u band agreement is promising, with the caveat that only four of the nine supernovae are well-observed in u and these four exhibit an 0.038 magnitude supernova-to-supernova scatter in this filter.

Mosher, J; Corlies, L; Folatelli, G; Frieman, J; Holtzman, J; Jha, S W; Kessler, R; Marriner, J; Phillips, M M; Stritzinger, M; Morrell, N; Schneider, D P

2012-01-01T23:59:59.000Z

308

Beyond the bubble catastrophe of Type Ia supernovae: Pulsating Reverse Detonation models  

E-Print Network [OSTI]

We describe a mechanism by which a failed deflagration of a Chandrasekhar-mass carbon-oxygen white dwarf can turn into a successful thermonuclear supernova explosion, without invoking an ad hoc high-density deflagration-detonation transition. Following a pulsating phase, an accretion shock develops above a core of 1 M_sun composed of carbon and oxygen, inducing a converging detonation. A three-dimensional simulation of the explosion produced a kinetic energy of 1.05E51 ergs and 0.70 M_sun of 56Ni, ejecting scarcely 0.01 M_sun of C-O moving at low velocities. The mechanism works under quite general conditions and is flexible enough to account for the diversity of normal Type Ia supernovae. In given conditions the detonation might not occur, which would reflect in peculiar signatures in the gamma and UV-wavelengths

Eduardo Bravo; Domingo Garcia-Senz

2006-04-03T23:59:59.000Z

309

Sensitivity study of explosive nucleosynthesis in type Ia supernovae: Modification of individual thermonuclear reaction rates  

Science Journals Connector (OSTI)

Background: Type Ia supernovae contribute significantly to the nucleosynthesis of many Fe-group and intermediate-mass elements. However, the robustness of nucleosynthesis obtained via models of this class of explosions has not been studied in depth until now.Purpose: We explore the sensitivity of the nucleosynthesis resulting from thermonuclear explosions of massive white dwarfs with respect to uncertainties in nuclear reaction rates. We put particular emphasis on indentifying the individual reactions rates that most strongly affect the isotopic products of these supernovae.Method: We have adopted a standard one-dimensional delayed detonation model of the explosion of a Chandrasekhar-mass white dwarf and have postprocessed the thermodynamic trajectories of every mass shell with a nucleosynthetic code to obtain the chemical composition of the ejected matter. We have considered increases (decreases) by a factor of 10 on the rates of 1196 nuclear reactions (simultaneously with their inverse reactions), repeating the nucleosynthesis calculations after modification of each reaction rate pair. We have computed as well hydrodynamic models for different rates of the fusion reactions of 12C and of 16O. From the calculations we have selected the reactions that have the largest impact on the supernova yields, and we have computed again the nucleosynthesis using two or three alternative prescriptions for their rates, taken from the JINA REACLIB database. For the three reactions with the largest sensitivity we have analyzed as well the temperature ranges where a modification of their rates has the strongest effect on nucleosynthesis.Results: The nucleosynthesis resulting from the type Ia supernova models is quite robust with respect to variations of nuclear reaction rates, with the exception of the reaction of fusion of two 12C nuclei. The energy of the explosion changes by less than ?4% when the rates of the reactions 12C+12C or 16O+16O are multiplied by a factor of 10 or 0.1. The changes in the nucleosynthesis owing to the modification of the rates of these fusion reactions are also quite modest; for instance, no species with a mass fraction larger than 0.02 experiences a variation of its yield larger than a factor of 2. We provide the sensitivity of the yields of the most abundant species with respect to the rates of the most intense reactions with protons, neutrons, and ?. In general, the yields of Fe-group nuclei are more robust than the yields of intermediate-mass elements. Among the species with yields larger than 10?8M?, 35S has the largest sensitivity to the nuclear reaction rates. It is remarkable that the reactions involving elements with Z>22 have a tiny influence on the supernova nucleosynthesis. Among the charged-particle reactions, the most influential on supernova nucleosynthesis are 30Si+p?31P+?, 20Ne+??24Mg+?, and 24Mg+??27Al+p. The temperatures at which a modification of their rate has a larger impact are in the range 2?T?4 GK.Conclusions: The explosion model (i.e., the assumed conditions and propagation of the flame) chiefly determines the element production of type Ia supernovae and derived quantities such as their luminosity, while the nuclear reaction rates used in the simulations have a small influence on the kinetic energy and final chemical composition of the ejecta. Our results show that the uncertainty in individual thermonuclear reaction rates cannot account for discrepancies of a factor of 2 between isotopic ratios in type Ia supernovae and those in the solar system, especially within the Fe group.

Eduardo Bravo and Gabriel Martnez-Pinedo

2012-05-18T23:59:59.000Z

310

A PRECISION PHOTOMETRIC COMPARISON BETWEEN SDSS-II AND CSP TYPE Ia SUPERNOVA DATA  

SciTech Connect (OSTI)

Consistency between Carnegie Supernova Project (CSP) and SDSS-II Supernova Survey ugri measurements has been evaluated by comparing Sloan Digital Sky Survey (SDSS) and CSP photometry for nine spectroscopically confirmed Type Ia supernova observed contemporaneously by both programs. The CSP data were transformed into the SDSS photometric system. Sources of systematic uncertainty have been identified, quantified, and shown to be at or below the 0.023 mag level in all bands. When all photometry for a given band is combined, we find average magnitude differences of equal to or less than 0.011 mag in ugri, with rms scatter ranging from 0.043 to 0.077 mag. The u-band agreement is promising, with the caveat that only four of the nine supernovae are well observed in u and these four exhibit an 0.038 mag supernova-to-supernova scatter in this filter.

Mosher, J.; Sako, M.; Corlies, L. [Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States); Folatelli, G. [Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan); Frieman, J.; Kessler, R. [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Holtzman, J. [Department of Astronomy, MSC 4500, New Mexico State University, P.O. Box 30001, Las Cruces, NM 88003 (United States); Jha, S. W. [Department of Physics and Astronomy, Rutgers, the State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States); Marriner, J. [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States); Phillips, M. M.; Morrell, N. [Las Campanas Observatory, Carnegie Observatories, Casilla 601, La Serena (Chile); Stritzinger, M. [Oskar Klein Centre for Cosmo Particle Physics, AlbaNova University Center, 106 91 Stockholm (Sweden); Schneider, D. P., E-mail: jmosher@sas.upenn.edu [Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States)

2012-07-15T23:59:59.000Z

311

A Precision Photometric Comparison between SDSS-II and CSP Type Ia Supernova Data  

SciTech Connect (OSTI)

Consistency between Carnegie Supernova Project (CSP) and SDSS-II Supernova Survey ugri measurements has been evaluated by comparing Sloan Digital Sky Survey (SDSS) and CSP photometry for nine spectroscopically confirmed Type Ia supernova observed contemporaneously by both programs. The CSP data were transformed into the SDSS photometric system. Sources of systematic uncertainty have been identified, quantified, and shown to be at or below the 0.023 mag level in all bands. When all photometry for a given band is combined, we find average magnitude differences of equal to or less than 0.011 mag in ugri, with rms scatter ranging from 0.043 to 0.077 mag. The u-band agreement is promising, with the caveat that only four of the nine supernovae are well observed in u and these four exhibit an 0.038 mag supernova-to-supernova scatter in this filter.

Mosher, J.; /Pennsylvania U.; Sako, M.; /Pennsylvania U.; Corlies, L.; /Pennsylvania U. /Columbia U.; Folatelli, G.; /Tokyo U. /Carnegie Inst. Observ.; Frieman, J.; /Chicago U., KICP /Chicago U., Astron. Astrophys. Ctr.; Holtzman, J.; /New Mexico State U.; Jha, S.W.; /Rutgers U., Piscataway; Kessler, R.; /Chicago U., Astron. Astrophys. Ctr. /Chicago U., KICP; Marriner, J.; /Fermilab; Phillips, M.M.; /Carnegie Inst. Observ.; Stritzinger, M.; /Aarhus U. /Stockholm U., OKC /Bohr Inst. /Carnegie Inst. Observ.

2012-06-01T23:59:59.000Z

312

{chi}{sup 2} versus median statistics in supernova type Ia data analysis  

SciTech Connect (OSTI)

In this paper we compare the performances of the {chi}{sup 2} and median likelihood analysis in the determination of cosmological constraints using type Ia supernovae data. We perform a statistical analysis using the 307 supernovae of the Union 2 compilation of the Supernova Cosmology Project and find that the {chi}{sup 2} statistical analysis yields tighter cosmological constraints than the median statistic if only supernovae data is taken into account. We also show that when additional measurements from the cosmic microwave background and baryonic acoustic oscillations are considered, the combined cosmological constraints are not strongly dependent on whether one applies the {chi}{sup 2} statistic or the median statistic to the supernovae data. This indicates that, when complementary information from other cosmological probes is taken into account, the performances of the {chi}{sup 2} and median statistics are very similar, demonstrating the robustness of the statistical analysis.

Barreira, A. [Centro de Fisica do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Departamento de Fisica da Faculdade de Ciencias da Universidade do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Avelino, P. P. [Departamento de Fisica da Faculdade de Ciencias da Universidade do Porto, Rua do Campo Alegre 687, 4169-007 Porto (Portugal); Centro de Astrofisica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto (Portugal)

2011-10-15T23:59:59.000Z

313

Small-scale Interaction of Turbulence with Thermonuclear Flames in Type Ia Supernovae  

E-Print Network [OSTI]

Microscopic turbulence-flame interactions of thermonuclear fusion flames occuring in Type Ia Supernovae were studied by means of incompressible direct numerical simulations with a highly simplified flame description. The flame is treated as a single diffusive scalar field with a nonlinear source term. It is characterized by its Prandtl number, Pr << 1, and laminar flame speed, S_L. We find that if S_L ~ u', where u' is the rms amplitude of turbulent velocity fluctuations, the local flame propagation speed does not significantly deviate from S_L even in the presence of velocity fluctuations on scales below the laminar flame thickness. This result is interpreted in the context of subgrid-scale modeling of supernova explosions and the mechanism for deflagration-detonation-transitions.

J. C. Niemeyer; W. K. Bushe; G. R. Ruetsch

1999-05-07T23:59:59.000Z

314

Initiation of the Detonation in the Gravitationally Confined Detonation Model of Type Ia Supernovae  

Science Journals Connector (OSTI)

We study the initiation of the detonation in the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia). In this model, ignition occurs at one or several off-center points, resulting in a burning bubble of hot ash that rises rapidly, breaks through the surface of the star, and collides at a point on the stellar surface opposite the breakout, producing a high-velocity inwardly directed flow. Initiation of the detonation occurs spontaneously in a region where the length scale of the temperature gradient extending from the flow (in which carbon burning is already occurring) into unburned fuel is commensurate to the range of critical length scales which have been derived from one-dimensional simulations that resolve the initiation of a detonation. By increasing the maximum resolution in a truncated cone that encompasses this region, beginning somewhat before initiation of the detonation occurs, we successfully simulate in situ the first gradient-initiated detonation in a whole-star simulation. The detonation emerges when a compression wave overruns a pocket of fuel situated in a Kelvin-Helmholtz cusp at the leading edge of the inwardly directed jet of burning carbon. The compression wave preconditions the temperature in the fuel in such a way that the Zel'dovich gradient mechanism can operate and a detonation ensues. We explore the dependence of the length scale of the temperature gradient on spatial resolution and discuss the implications for the robustness of this detonation mechanism. We find that the time and the location at which initiation of the detonation occurs varies with resolution. In particular, initiation of a detonation had not yet occurred in our highest resolution simulation by the time we ended the simulation because of the computational demand it required. However, it may detonate later. We suggest that the turbulent shear layer surrounding the inwardly directed jet provides the most favorable physical conditions, and therefore the most likely location, for initiation of a detonation in the GCD model.

Ivo R. Seitenzahl; Casey A. Meakin; Don Q. Lamb; James W. Truran

2009-01-01T23:59:59.000Z

315

Study of the Detonation Phase in the Gravitationally Confined Detonation Model of Type Ia Supernovae  

E-Print Network [OSTI]

We study the gravitationally confined detonation (GCD) model of Type Ia supernovae through the detonation phase and into homologous expansion. In the GCD model, a detonation is triggered by the surface flow due to single point, off-center flame ignition in carbon-oxygen white dwarfs. The simulations are unique in terms of the degree to which non-idealized physics is used to treat the reactive flow, including weak reaction rates and a time dependent treatment of material in nuclear statistical equilibrium (NSE). Careful attention is paid to accurately calculating the final composition of material which is burned to NSE and frozen out in the rapid expansion following the passage of a detonation wave over the high density core of the white dwarf; and an efficient method for nucleosynthesis post-processing is developed which obviates the need for costly network calculations along tracer particle thermodynamic trajectories. Observational diagnostics are presented for the explosion models, including abundance stratifications and integrated yields. We find that for all of the ignition conditions studied here, a self regulating process comprised of neutronization and stellar expansion results in final \\iso{Ni}{56} masses of $\\sim$1.1\\msun. But, more energetic models result in larger total NSE and stable Fe peak yields. The total yield of intermediate mass elements is $\\sim0.1$\\msun and the explosion energies are all around 1.5$\\times10^{51}$ ergs. The explosion models are briefly compared to the inferred properties of recent Type Ia supernova observations. The potential for surface detonation models to produce lower luminosity (lower \\iso{Ni}{56} mass) supernovae is discussed.

Casey A. Meakin; Ivo Seitenzahl; Dean Townsley; George C. Jordan IV; James Truran; Don Lamb

2008-06-30T23:59:59.000Z

316

Initiation of the detonation in the gravitationally confined detonation model of type Ia supernovae.  

SciTech Connect (OSTI)

We study the initiation of the detonation in the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia). In this model, ignition occurs at one or several off-center points, resulting in a burning bubble of hot ash that rises rapidly, breaks through the surface of the star, and collides at a point on the stellar surface opposite the breakout, producing a high-velocity inwardly directed flow. Initiation of the detonation occurs spontaneously in a region where the length scale of the temperature gradient extending from the flow (in which carbon burning is already occurring) into unburned fuel is commensurate to the range of critical length scales which have been derived from one-dimensional simulations that resolve the initiation of a detonation. By increasing the maximum resolution in a truncated cone that encompasses this region, beginning somewhat before initiation of the detonation occurs, we successfully simulate in situ the first gradient-initiated detonation in a whole-star simulation. The detonation emerges when a compression wave overruns a pocket of fuel situated in a Kelvin-Helmholtz cusp at the leading edge of the inwardly directed jet of burning carbon. The compression wave preconditions the temperature in the fuel in such a way that the Zel'dovich gradient mechanism can operate and a detonation ensues. We explore the dependence of the length scale of the temperature gradient on spatial resolution and discuss the implications for the robustness of this detonation mechanism. We find that the time and the location at which initiation of the detonation occurs varies with resolution. In particular, initiation of a detonation had not yet occurred in our highest resolution simulation by the time we ended the simulation because of the computational demand it required. However, it may detonate later. We suggest that the turbulent shear layer surrounding the inwardly directed jet provides the most favorable physical conditions, and therefore the most likely location, for initiation of a detonation in the GCD model.

Seitenzahl, I. R.; Meakin, C. A.; Lamb, D. Q.; Truran, J. W. (Physics); (Univ. of Chicago); (Max-Planck-Inst. for Astrophysics); (Univ. of Arizona)

2009-07-20T23:59:59.000Z

317

Study of the detonation phase in the gravitationally confined detonation model of type Ia supernovae.  

SciTech Connect (OSTI)

We study the initiation of the detonation in the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia). In this model, ignition occurs at one or several off-center points, resulting in a burning bubble of hot ash that rises rapidly, breaks through the surface of the star, and collides at a point on the stellar surface opposite the breakout, producing a high-velocity inwardly directed flow. Initiation of the detonation occurs spontaneously in a region where the length scale of the temperature gradient extending from the flow (in which carbon burning is already occurring) into unburned fuel is commensurate to the range of critical length scales which have been derived from one-dimensional simulations that resolve the initiation of a detonation. By increasing the maximum resolution in a truncated cone that encompasses this region, beginning somewhat before initiation of the detonation occurs, we successfully simulate in situ the first gradient-initiated detonation in a whole-star simulation. The detonation emerges when a compression wave overruns a pocket of fuel situated in a Kelvin-Helmholtz cusp at the leading edge of the inwardly directed jet of burning carbon. The compression wave preconditions the temperature in the fuel in such a way that the Zeldovich gradient mechanism can operate and a detonation ensues. We explore the dependence of the length scale of the temperature gradient on spatial resolution and discuss the implications for the robustness of this detonation mechanism. We find that the time and the location at which initiation of the detonation occurs varies with resolution. In particular, initiation of a detonation had not yet occurred in our highest resolution simulation by the time we ended the simulation because of the computational demand it required. However, it may detonate later. We suggest that the turbulent shear layer surrounding the inwardly directed jet provides the most favorable physical conditions, and therefore the most likely location, for initiation of a detonation in the GCD model.

Meakin, C. A.; Seitenzahl, I.; Jordan, G. C.; Truran,, J.; Lamb, D.; Physics; Univ. of Chicago; Univ. of Arizona

2009-07-20T23:59:59.000Z

318

NUCLEOSYNTHESIS IN TWO-DIMENSIONAL DELAYED DETONATION MODELS OF TYPE Ia SUPERNOVA EXPLOSIONS  

SciTech Connect (OSTI)

For the explosion mechanism of Type Ia supernovae (SNe Ia), different scenarios have been suggested. In these, the propagation of the burning front through the exploding white dwarf (WD) star proceeds in different modes, and consequently imprints of the explosion model on the nucleosynthetic yields can be expected. The nucleosynthetic characteristics of various explosion mechanisms are explored based on three two-dimensional explosion simulations representing extreme cases: a pure turbulent deflagration, a delayed detonation following an approximately spherical ignition of the initial deflagration, and a delayed detonation arising from a highly asymmetric deflagration ignition. Apart from this initial condition, the deflagration stage is treated in a parameter-free approach. The detonation is initiated when the turbulent burning enters the distributed burning regime. This occurs at densities around 10{sup 7} g cm{sup -3}-relatively low as compared to existing nucleosynthesis studies for one-dimensional spherically symmetric models. The burning in these multidimensional models is different from that in one-dimensional simulations as the detonation wave propagates both into unburned material in the high-density region near the center of a WD and into the low-density region near the surface. Thus, the resulting yield is a mixture of different explosive burning products, from carbon-burning products at low densities to complete silicon-burning products at the highest densities, as well as electron-capture products synthesized at the deflagration stage. Detailed calculations of the nucleosynthesis in all three models are presented. In contrast to the deflagration model, the delayed detonations produce a characteristic layered structure and the yields largely satisfy constraints from Galactic chemical evolution. In the asymmetric delayed detonation model, the region filled with electron capture species (e.g., {sup 58}Ni, {sup 54}Fe) is within a shell, showing a large off-set, above the bulk of {sup 56}Ni distribution, while species produced by the detonation are distributed more spherically.

Maeda, K. [Institute for the Physics and Mathematics of the Universe (IPMU), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583 (Japan); Roepke, F.K.; Fink, M.; Hillebrandt, W.; Travaglio, C. [Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Strasse 1, 85741 Garching (Germany); Thielemann, F.-K., E-mail: keiichi.maeda@ipmu.j [Department Physik, Universitaet Basel, CH-4056 Basel (Switzerland)

2010-03-20T23:59:59.000Z

319

INITIATION OF THE DETONATION IN THE GRAVITATIONALLY CONFINED DETONATION MODEL OF TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

We study the initiation of the detonation in the gravitationally confined detonation (GCD) model of Type Ia supernovae (SNe Ia). In this model, ignition occurs at one or several off-center points, resulting in a burning bubble of hot ash that rises rapidly, breaks through the surface of the star, and collides at a point on the stellar surface opposite the breakout, producing a high-velocity inwardly directed flow. Initiation of the detonation occurs spontaneously in a region where the length scale of the temperature gradient extending from the flow (in which carbon burning is already occurring) into unburned fuel is commensurate to the range of critical length scales which have been derived from one-dimensional simulations that resolve the initiation of a detonation. By increasing the maximum resolution in a truncated cone that encompasses this region, beginning somewhat before initiation of the detonation occurs, we successfully simulate in situ the first gradient-initiated detonation in a whole-star simulation. The detonation emerges when a compression wave overruns a pocket of fuel situated in a Kelvin-Helmholtz cusp at the leading edge of the inwardly directed jet of burning carbon. The compression wave preconditions the temperature in the fuel in such a way that the Zel'dovich gradient mechanism can operate and a detonation ensues. We explore the dependence of the length scale of the temperature gradient on spatial resolution and discuss the implications for the robustness of this detonation mechanism. We find that the time and the location at which initiation of the detonation occurs varies with resolution. In particular, initiation of a detonation had not yet occurred in our highest resolution simulation by the time we ended the simulation because of the computational demand it required. However, it may detonate later. We suggest that the turbulent shear layer surrounding the inwardly directed jet provides the most favorable physical conditions, and therefore the most likely location, for initiation of a detonation in the GCD model.

Seitenzahl, Ivo R. [Department of Physics, University of Chicago, Chicago, IL 60637 (United States); Meakin, Casey A.; Truran, James W. [Joint Institute for Nuclear Astrophysics, University of Chicago, Chicago, IL 60637 (United States); Lamb, Don Q. [Center for Astrophysical Thermonuclear Flashes, University of Chicago, Chicago, IL 60637 (United States)

2009-07-20T23:59:59.000Z

320

SN 2003du: Signatures of the Circumstellar Environment in a Normal Type Ia Supernova?  

E-Print Network [OSTI]

We present observations of the Type Ia supernova 2003du and report the detectionof an unusual, high-velocity component in the Ca II infrared triplet, similar tofeatures previously observed in SN 2000cx and SN 2001el. This feature exhibits a large expansion velocity (~18,000 km/s) which is nearly constant between -7 and +2 days relative to maximum light, and disappears shortly thereafter. Otherthan this feature, the spectral evolution and light curve resemble those of a normal SN Ia. We find that the Ca II feature can plausibly be caused by a dense shell formed when circumstellar material of solar abundance is overrun by the rapidly expanding outermost layers of the SN ejecta. Model calculations show that the optical and infrared spectra are remarkably unaffected by the circumstellar interaction. In particular, no hydrogen lines are detectable in either absorption or emission. The only qualitatively different features are the strong, high-velocity feature in the Ca II IR-triplet, and a somewhat weaker O I feature near 7,300 AA. The morphology and time evolution of these features provide an estimate for the amount of accumulated matter and an indication of the mixing in the dense shell. We apply these diagnostic tools to SN 2003du and infer that about 2 x 10^{-2} M_sun of solar abundance material may have accumulated in a circumstellar shell prior to the observations. Furthermore, the early light curve data imply that the circumstellar material was originally very close to the progenitor system, perhaps from an accretion disk, Roche lobe or common envelope.

C. L. Gerardy; P. Hoeflich; R. A. Fesen; G. H. Marion; K. Nomoto; R. Quimby; B. E. Schaefer; L. Wang; J. C. Wheeler

2003-09-23T23:59:59.000Z

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321

Sensitivity study of explosive nucleosynthesis in Type Ia supernovae: I. Modification of individual thermonuclear reaction rates  

E-Print Network [OSTI]

We explore the sensitivity of the nucleosynthesis due to type Ia supernovae with respect to uncertainties in nuclear reaction rates. We have adopted a standard one-dimensional delayed detonation model of the explosion of a Chandrasekhar-mass white dwarf, and have post-processed the thermodynamic trajectories of every mass-shell with a nucleosynthetic code, with increases (decreases) by a factor of ten on the rates of 1196 nuclear reactions. We have computed as well hydrodynamic models for different rates of the fusion reactions of 12C and of 16O. For selected reactions, we have recomputed the nucleosynthesis with alternative prescriptions for their rates taken from the JINA REACLIB database, and have analyzed the temperature ranges where modifications of their rates have the strongest effect on nucleosynthesis. The nucleosynthesis resulting from the Type Ia supernova models is quite robust with respect to variations of nuclear reaction rates, with the exception of the reaction of fusion of 12C nuclei. The energy of the explosion changes by less than \\sim4%. The changes in the nucleosynthesis due to the modification of the rates of fusion reactions are as well quite modest, for instance no species with a mass fraction larger than 0.02 experiences a variation of its yield larger than a factor of two. We provide the sensitivity of the yields of the most abundant species with respect to the rates of the most intense reactions with protons, neutrons, and alphas. In general, the yields of Fe-group nuclei are more robust than the yields of intermediate-mass elements. Among the charged particle reactions, the most influential on supernova nucleosynthesis are 30Si + p \\rightleftarrows 31P + {\\gamma}, 20Ne + {\\alpha} \\rightleftarrows 24Mg + {\\gamma}, and 24Mg + {\\alpha} \\rightleftarrows 27Al + p. The temperatures at which a modification of their rate has a larger impact are in the range 2 < T < 4 GK. (abridged)

Eduardo Bravo; Gabriel Martnez-Pinedo

2012-04-09T23:59:59.000Z

322

Incompatibility of a comoving Ly-alpha forest with supernova-Ia luminosity distances  

E-Print Network [OSTI]

Recently Perlmutter et al. suggested a positive value of Einstein's cosmological constant Lambda on the basis of luminosity distances from type-Ia supernovae. However, Lambda world models had earlier been proposed by Hoell & Priester and Liebscher et al. on the basis of quasar absorption-line data. Employing more general repulsive fluids ("dark energy") encompassing the Lambda component we quantitatively compare both approaches with each other. Fitting the SN-data by a minimum-component model consisting of dark energy + dust yields a closed universe with a large amount of dust exceeding the baryonic content constrained by big-bang nucleosynthesis. The nature of the dark energy is hardly constrained. Only when enforcing a flat universe there is a clear tendency to a dark-energy Lambda fluid and the `canonical' value Omega_M = 0.3 for dust. Conversely, fitting the quasar-data by a minimum-component model yields a sharply defined, slightly closed model with a low dust density ruling out significant pressureless dark matter. The dark-energy component obtains an equation-of-state P = -0.96 epsilon close to that of a Lambda-fluid. Omega_M = 0.3 or a precisely flat spatial geometry are inconsistent with minimum-component models. It is found that quasar and supernova data sets cannot be reconciled with each other via (repulsive ideal fluid+dust+radiation)-world models. Compatibility could be reached by drastic expansion of the parameter space with at least two exotic fluids added to dust and radiation as world constituents. If considering such solutions as far-fetched one has to conclude that the quasar absorption line and the SN-Ia constraints are incompatible.

Jens Thomas; Hartmut Schulz

2001-03-18T23:59:59.000Z

323

HELIUM-IGNITED VIOLENT MERGERS AS A UNIFIED MODEL FOR NORMAL AND RAPIDLY DECLINING TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

The progenitors of Type Ia supernovae (SNe Ia) are still unknown, despite significant progress during the past several years in theory and observations. Violent mergers of two carbon-oxygen (CO) white dwarfs (WDs) are a candidate scenario suggested to be responsible for at least a significant fraction of normal SNe Ia. Here, we simulate the merger of two CO WDs using a moving-mesh code that allows for the inclusion of thin helium (He) shells (0.01 M{sub Sun }) on top of the WDs at an unprecedented numerical resolution. The accretion of He onto the primary WD leads to the formation of a detonation in its He shell. This detonation propagates around the CO WD and sends a converging shock wave into its core, known to robustly trigger a second detonation, as in the well-known double-detonation scenario for He-accreting CO WDs. However, in contrast to that scenario where a massive He shell is required to form a detonation through thermal instability, here the He detonation is ignited dynamically. Accordingly the required He-shell mass is significantly smaller, and hence its burning products are unlikely to affect the optical display of the explosion. We show that this scenario, which works for CO primary WDs with CO- as well as He-WD companions, has the potential to explain the different brightness distributions, delay times, and relative rates of normal and fast declining SNe Ia. Finally, we discuss extensions to our unified merger model needed to obtain a comprehensive picture of the full observed diversity of SNe Ia.

Pakmor, R.; Springel, V. [Heidelberger Institut fuer Theoretische Studien, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg (Germany); Kromer, M. [Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8583 (Japan); Taubenberger, S. [Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching (Germany)

2013-06-10T23:59:59.000Z

324

New Hubble Space Telescope Discoveries of Type Ia Supernovae at z > 1: Narrowing Constraints on the Early Behavior of Dark Energy  

E-Print Network [OSTI]

We have discovered 21 new Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to trace the history of cosmic expansion over the last 10 billion years. These objects, which include 13 spectroscopically confirmed SNe Ia at z > 1, were discovered during 14 epochs of reimaging of the GOODS fields North and South over two years with the Advanced Camera for Surveys on HST. Together with a recalibration of our previous HST-discovered SNe Ia, the full sample of 23 SNe Ia at z > 1 provides the highest-redshift sample known. Combined with previous SN Ia datasets, we measured H(z) at discrete, uncorrelated epochs, reducing the uncertainty of H(z>1) from 50% to under 20%, strengthening the evidence for a cosmic jerk--the transition from deceleration in the past to acceleration in the present. The unique leverage of the HST high-redshift SNe Ia provides the first meaningful constraint on the dark energy equation-of-state parameter at z >1. The result remains consistent with a cosmological constant (w(z)=-1), and rules out rapidly evolving dark energy (dw/dz >>1). The defining property of dark energy, its negative pressure, appears to be present at z>1, in the epoch preceding acceleration, with ~98% confidence in our primary fit. Moreover, the z>1 sample-averaged spectral energy distribution is consistent with that of the typical SN Ia over the last 10 Gyr, indicating that any spectral evolution of the properties of SNe Ia with redshift is still below our detection threshold.

Adam G. Riess; Louis-Gregory Strolger; Stefano Casertano; Henry C. Ferguson; Bahram Mobasher; Ben Gold; Peter J. Challis; Alexei V. Filippenko; Saurabh Jha; Weidong Li; John Tonry; Ryan Foley; Robert P. Kirshner; Mark Dickinson; Emily MacDonald; Daniel Eisenstein; Mario Livio; Josh Younger; Chun Xu; Tomas Dahlen; Daniel Stern

2006-11-17T23:59:59.000Z

325

??eia e e et ??? oa0 to 3i5ontinBoB5 PieeFi5e Hinea tiTiUation ...  

E-Print Network [OSTI]

PieeFi5e Hinea tiTiUation. I.R. de Farias JR., M. ?hao, and H. ?hao. State University of New York at jumalo. {defariasy m|haoy |hon??ia}@??ffalo.ed?.

326

LAX XXlCfl jX?iK, Idd+?KYLViG?IA  

Office of Legacy Management (LM)

f f , : I~&l, samtier cipwati8Aa CffUm - . Jiux.lCJ d,# 1754 - - _- - .- t :; . Jesse e. ahizmn*~*ter -2.' -------- - _ &tV' hi@A l f izau Bkteriala ;' . . 1 -7 I _' i' . Fpr&G& r&Q Q,&& fu &fI& L;&& -l&d 2;,i' iI,;/Qi' rIGN CQ&GgJy p;E& p;~p>gyf LAX XXlCfl jX?iK, Idd+?KYLViG?IA i-icfer~~o is &o ta yaw rwarandu3;: l P iimwmbec L?, 1953, reque&in~ a d&q.&ti of khority tA A&sister prog= for th+zz developmrrrl, Ii-&k& & acyui8itti ef c;uYletit*type and reswitlitc-type urtim bi:aPing eres and far t3-u jx*uctim and acquisitian 6f W ;aniU CCm- csa:ratc~ fhzi awes wit2n Lhe Six&e of Pemlsyzvania. 1 da not b&i- the projscrt fmr the pkcch2670 +S eroa from i&d.&

327

Direct numerical simulations of type Ia supernovae flames I: The landau-darrieus instability  

SciTech Connect (OSTI)

Planar flames are intrinsically unstable in open domains due to the thermal expansion across the burning front--the Landau-Darrieus instability. This instability leads to wrinkling and growth of the flame surface, and corresponding acceleration of the flame, until it is stabilized by cusp formation. We look at the Landau-Darrieus in stability for C/O thermonuclear flames at conditions relevant to the late stages of a Type Ia supernova explosion. Two-dimensional direct numerical simulations of both single-mode and multi-mode perturbations using a low Mach number hydrodynamics code are presented. We show the effect of the instability on the flame speed as a function of both the density and domain size, demonstrate the existence of the small scale cutoff to the growth of the instability, and look for the proposed breakdown of the non-linear stabilization at low densities. The effects of curvature on the flame as quantified through measurements of the growth rate and computation of the corresponding Markstein number. While accelerations of a few percent are observed, they are too small to have any direct outcome on the supernova explosion.

Bell, J.B.; Day, M.S.; Rendleman, C.A.; Woosley, S.E.; Zingale, M.

2003-11-24T23:59:59.000Z

328

Thermonuclear .Ia Supernovae from Helium Shell Detonations: Explosion Models and Observables  

Science Journals Connector (OSTI)

During the early evolution of an AM Canum Venaticorum system, helium is accreted onto the surface of a white dwarf under conditions suitable for unstable thermonuclear ignition. The turbulent motions induced by the convective burning phase in the He envelope become strong enough to influence the propagation of burning fronts and may result in the onset of a detonation. Such an outcome would yield radioactive isotopes and a faint rapidly rising thermonuclear ".Ia" supernova. In this paper, we present hydrodynamic explosion models and observable outcomes of these He shell detonations for a range of initial core and envelope masses. The peak UVOIR bolometric luminosities range by a factor of 10 (from 5 ? 1041 to 5 ? 1042 erg s1), and the R-band peak varies from M R,peak = 15 to 18. The rise times in all bands are very rapid (40Ca through 56Ni) and unburnt He. Thus, the spectra around peak light lack signs of intermediate-mass elements and are dominated by CaII and TiII features, with the caveat that our radiative transfer code does not include the nonthermal effects necessary to produce He features.

Ken J. Shen; Dan Kasen; Nevin N. Weinberg; Lars Bildsten; Evan Scannapieco

2010-01-01T23:59:59.000Z

329

Comparison of the Legacy and Gold SnIa Dataset Constraints on Dark Energy Models  

E-Print Network [OSTI]

We have performed a comparative analysis of three recent and reliable SnIa datasets available in the literature: the Full Gold (FG) dataset (157 data points $0dataset (140 data points $0dataset (115 data points $0datasets are consistent with each other at the 95% confidence level, the latest (SNLS) dataset shows distinct trends which are not shared by the Gold datasets. We find that the best fit dynamical $w(z)$ obtained from the SNLS dataset does not cross the PDL $w=-1$ and remains above and close to the $w=-1$ line for the whole redshift range $0datasets (FG and TG) clearly crosses the PDL and departs significantly from the PDL $w=-1$ line while the LCDM parameter values are about $2\\sigma$ away from the best fit $w(z)$. In addition, the $(\\Omega_{0m},\\Omega_\\Lambda)$ parameters in a LCDM parametrization without a flat prior, fit by the SNLS dataset, favor the minimal flat LCDM concordance model. The corresponding fit with the Gold datasets mildly favors a closed universe and the flat LCDM parameter values are $1\\sigma - 2\\sigma$ away from the best fit $(\\Omega_{0m},\\Omega_\\Lambda)$.

S. Nesseris; L. Perivolaropoulos

2005-12-02T23:59:59.000Z

330

Phenomenology for Supernova Ia Data Based on a New Cosmic Time  

E-Print Network [OSTI]

A new phenomenological theory for the expansion of our universe is presented. Because fundamental supporting theory is still in development, its discussion is not presented in this paper. The theory is based on a new algebraic expression for cosmic time G Rho t^2=3/32Pi, which correctly predicts the WMAP measured cosmological constants and the fundamental Hubble parameter H(t) for the expansion of the universe. A replacement for dark matter, called here "dark mass", is proposed which scales as with the expansion and incorporated. It does not react with ordinary matter, except gravitationally, and produces flat rotational curves for spiral galaxies. Also a new expression for the approaching velocity of radiation in a closed 3-sphere expanding universe is given that accounts for the early degrading negative approach of radiation for z > 1.7. The expression is v = Hr-c. Combining these three elements produces a luminosity distance dL that successfully predicts the apparent magnitude of exploding supernova Ia stars and even the new gamma ray bursts with no need for dark energy or acceleration of the expansion of the universe.

Charles B. Leffert

2007-07-26T23:59:59.000Z

331

Evaluating Systematic Dependencies of Type Ia Supernovae: The Influence of Deflagration to Detonation Density  

E-Print Network [OSTI]

We explore the effects of the deflagration to detonation transition (DDT) density on the production of Ni-56 in thermonuclear supernova explosions (type Ia supernovae). Within the DDT paradigm, the transition density sets the amount of expansion during the deflagration phase of the explosion and therefore the amount of nuclear statistical equilibrium (NSE) material produced. We employ a theoretical framework for a well-controlled statistical study of two-dimensional simulations of thermonuclear supernovae with randomized initial conditions that can, with a particular choice of transition density, produce a similar average and range of Ni-56 masses to those inferred from observations. Within this framework, we utilize a more realistic "simmered" white dwarf progenitor model with a flame model and energetics scheme to calculate the amount of Ni-56 and NSE material synthesized for a suite of simulated explosions in which the transition density is varied in the range 1-3x10^7 g/cc. We find a quadratic dependence ...

Jackson, Aaron P; Townsley, Dean M; Chamulak, David A; Brown, Edward F; Timmes, F X

2010-01-01T23:59:59.000Z

332

A Test of Tully-Fisher Distance Estimates Using Cepheids and Type Ia Supernovae  

E-Print Network [OSTI]

We update and extend the results of Shanks (1997, MNRAS, 290, L77) by making a direct test of Tully-Fisher distance estimates to thirteen spiral galaxies with HST Cepheid distances and to ten spiral galaxies with Type Ia supernova (SNIa) distances. The results show that the Tully-Fisher distance moduli are too short with respect to the Cepheid distances by 0.46+-0.11mag and too short with respect to the SNIa distances by 0.49+-0.18mag. Combining the HST Cepheid and the best SNIa data suggests that, overall, previous Tully-Fisher distances at v~1000 kms-1 were too short by 0.43+-0.09mag, a result which is significant at the 4.6 sigma level. These data therefore indicate that previous Tully-Fisher distances should be revised upwards by 22+-5% implying, for example, a Virgo distance of 19.0+-1.8Mpc. The value of Ho from Tully-Fisher estimates is correspondingly revised downwards from Ho=84+-10kms-1Mpc-1 to Ho=69+-8kms-1Mpc-1. There is evidence that the Tully-Fisher relation at large distances is affected by Malmquist bias. In this case, we argue that Ho<50kms-1Mpc-1 cannot be ruled out by Tully-Fisher considerations.

T. Shanks

1999-01-24T23:59:59.000Z

333

Parametrizing the transition to the phantom epoch with Supernovae Ia and Standard Rulers  

E-Print Network [OSTI]

The reconstruction of a (non)canonical scalar field Lagrangian from the dark energy Equation of State (EoS) parameter is studied, where it is shown that any EoS parametrization can be well reconstructed in terms of scalar fields. Several examples of EoS parameters are studied and the particular scalar field Lagrangian is reconstructed. Then, we propose some new parametrizations that may present a (fast) transition to a phantom dark energy EoS (where $w_{DE}dark energy EoS are studied by using supernovae Ia data (HST Cluster Supernova Survey) combined with Standard Ruler datasets [Cosmic Microwave Background (CMB) and Baryon Acoustic Oscillations (BAO)] and its comparison with the $\\Lambda$CDM model is analyzed. Then, the best fit of the models is obtained, which provides some information about whether a phantom transition may be supported by the observations. In this regard, the crossing of the phantom barrier is allowed statistically but the occurrence of a future singularity seems unlikely.

Iker Leanizbarrutia; Diego Sez-Gmez

2014-04-14T23:59:59.000Z

334

A POSSIBLE EVOLUTIONARY SCENARIO OF HIGHLY MAGNETIZED SUPER-CHANDRASEKHAR WHITE DWARFS: PROGENITORS OF PECULIAR TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

Several recently discovered peculiar Type Ia supernovae seem to demand an altogether new formation theory that might help explain the puzzling dissimilarities between them and the standard Type Ia supernovae. The most striking aspect of the observational analysis is the necessity of invoking super-Chandrasekhar white dwarfs having masses {approx}2.1-2.8 M{sub Sun }, M{sub Sun} being the mass of Sun, as their most probable progenitors. Strongly magnetized white dwarfs having super-Chandrasekhar masses have already been established as potential candidates for the progenitors of peculiar Type Ia supernovae. Owing to the Landau quantization of the underlying electron degenerate gas, theoretical results yielded the observationally inferred mass range. Here, we sketch a possible evolutionary scenario by which super-Chandrasekhar white dwarfs could be formed by accretion on to a commonly observed magnetized white dwarf, invoking the phenomenon of flux freezing. This opens multiple possible evolution scenarios ending in supernova explosions of super-Chandrasekhar white dwarfs having masses within the range stated above. We point out that our proposal has observational support, such as the recent discovery of a large number of magnetized white dwarfs by the Sloan Digital Sky Survey.

Das, Upasana; Mukhopadhyay, Banibrata [Department of Physics, Indian Institute of Science, Bangalore 560012 (India); Rao, A. R., E-mail: upasana@physics.iisc.ernet.in, E-mail: bm@physics.iisc.ernet.in, E-mail: arrao@tifr.res.in [Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai 400005 (India)

2013-04-10T23:59:59.000Z

335

Type Ia Supernovae with Bi-Modal Explosions Are Common -- Possible Smoking Gun for Direct Collisions of White-Dwarfs  

E-Print Network [OSTI]

We discover clear doubly-peaked line profiles in 3 out of ~20 type Ia supernovae (SNe Ia) with high-quality nebular-phase spectra. The profiles are consistently present in three well-separated Co/Fe emission features. The two peaks are respectively blue-shifted and red-shifted relative to the host galaxies and are separated by ~5000 km/s. The doubly-peaked profiles directly reflect a bi-modal velocity distribution of the radioactive Ni56 in the ejecta that powers the emission of these SNe. Due to their random orientations, only a fraction of SNe with intrinsically bi-modal velocity distributions will appear as doubly-peaked spectra. Therefore SNe with intrinsic bi-modality are likely common, especially among the SNe in the low-luminosity (~40% of all SNe Ia) part on the Philips relation \\Delta m15(B) >~ 1.3. Bi-modality is naturally expected from direct collisions of white dwarfs (WDs) due to the detonation of both WDs and is demonstrated in a 3D 0.64 M_Sun-0.64 M_Sun WD collision simulation.

Dong, Subo; Kushnir, Doron; Prieto, Jose L

2014-01-01T23:59:59.000Z

336

Three-Dimensional Simulations of the Deflagration Phase of the Gravitationally Confined Detonation Model of Type Ia Supernovae  

E-Print Network [OSTI]

We report the results of a series of three-dimensional (3-D) simulations of the deflagration phase of the gravitationally confined detonation mechanism for Type Ia supernovae. In this mechanism, ignition occurs at one or several off-center points, resulting in a burning bubble of hot ash that rises rapidly, breaks through the surface of the star, and collides at a point opposite breakout on the stellar surface. We find that detonation conditions are robustly reached in our 3-D simulations for a range of initial conditions and resolutions. Detonation conditions are achieved as the result of an inwardly-directed jet that is produced by the compression of unburnt surface material when the surface flow collides with itself. A high-velocity outwardly-directed jet is also produced. The initial conditions explored in this paper lead to conditions at detonation that can be expected to produce large amounts of $^{56}$Ni and small amounts of intermediate mass elements. These particular simulations are therefore relevant only to high luminosity Type Ia supernovae. Recent observations of Type Ia supernovae imply a compositional structure that is qualitatively consistent with that expected from these simulations.

G C Jordan IV; R T Fisher; D M Townsley; A C Calder; C Graziani; S Asida; D Q Lamb; J W Truran

2007-03-21T23:59:59.000Z

337

The Joint Efficient Dark-energy Investigation (JEDI): Measuring the cosmic expansion history from type Ia supernovae  

E-Print Network [OSTI]

JEDI (Joint Efficient Dark-energy Investigation) is a candidate implementation of the NASA-DOE Joint Dark Energy Mission (JDEM). JEDI will probe dark energy in three independent methods: (1) type Ia supernovae, (2) baryon acoustic oscillations, and (3) weak gravitational lensing. In an accompanying paper, an overall summary of the JEDI mission is given. In this paper, we present further details of the supernova component of JEDI. To derive model-independent constraints on dark energy, it is important to precisely measure the cosmic expansion history, H(z), in continuous redshift bins from z \\~ 0-2 (the redshift range in which dark energy is important). SNe Ia at z > 1 are not readily accessible from the ground because the bulk of their light has shifted into the near-infrared where the sky background is overwhelming; hence a space mission is required to probe dark energy using SNe. Because of its unique near-infrared wavelength coverage (0.8-4.2 microns), JEDI has the advantage of observing SNe Ia in the rest frame J band for the entire redshift range of 0 energy are discussed, with special emphasis on the improved precision afforded by the rest frame near-infrared data.

M. M. Phillips; Peter Garnavich; Yun Wang; David Branch; Edward Baron; Arlin Crotts; J. Craig Wheeler; Edward Cheng; Mario Hamuy; for the JEDI Team

2006-06-28T23:59:59.000Z

338

Constraining the dark energy and smoothness parameter with typeIa supernovae and gamma-ray bursts  

Science Journals Connector (OSTI)

The existence of inhomogeneities in the observed Universe modifies the distance-redshift relations thereby affecting the results of cosmological tests in comparison to the ones derived assuming spatially uniform models. By modeling the inhomogeneities through a Zeldovich-Kantowski-Dyer-Roeder approach which is phenomenologically characterized by a smoothness parameter ?, we rediscuss the constraints on the cosmic parameters based on typeIa supernovae (SNeIa) and gamma-ray bursts (GRBs) data. The present analysis is restricted to a flat ?CDM model with the reasonable assumption that ? does not clump. A ?2 analysis using 557 SNeIa data from the Union2 compilation data (R. Amanullah et al., Astrophys. J. 716, 712 (2010).) constrains the pair of parameters (?m, ?) to ?m=0.27-0.03+0.08 (2?) and ??0.25. A similar analysis based only on 59 Hymnium GRBs (H. Wei, J. Cosmol. Astropart. Phys. 08 (2010) 020.) constrains the matter density parameter to be ?m=0.35-0.24+0.62 (2?) while all values for the smoothness parameter are allowed. By performing a joint analysis, it is found that ?m=0.27-0.03+0.06 and ??0.52. As a general result, although considering that current GRB data alone cannot constrain the smoothness ? parameter, our analysis provides an interesting cosmological probe for dark energy even in the presence of inhomogeneities.

V. C. Busti; R. C. Santos; J. A. S. Lima

2012-05-07T23:59:59.000Z

339

THE HUBBLE SPACE TELESCOPE CLUSTER SUPERNOVA SURVEY. III. CORRELATED PROPERTIES OF TYPE Ia SUPERNOVAE AND THEIR HOSTS AT 0.9 < z < 1.46  

SciTech Connect (OSTI)

Using the sample of Type Ia supernovae (SNe Ia) discovered by the Hubble Space Telescope (HST) Cluster Supernova Survey and augmented with HST-observed SNe Ia in the Great Observatories Origins Deep Survey (GOODS) fields, we search for correlations between the properties of SNe and their host galaxies at high redshift. We use galaxy color and quantitative morphology to determine the red sequence in 25 clusters and develop a model to distinguish passively evolving early-type galaxies from star-forming galaxies in both clusters and the field. With this approach, we identify 6 SN Ia hosts that are early-type cluster members and 11 SN Ia hosts that are early-type field galaxies. We confirm for the first time at z > 0.9 that SNe Ia hosted by early-type galaxies brighten and fade more quickly than SNe Ia hosted by late-type galaxies. We also show that the two samples of hosts produce SNe Ia with similar color distributions. The relatively simple spectral energy distributions expected for passive galaxies enable us to measure stellar masses of early-type SN hosts. In combination with stellar mass estimates of late-type GOODS SN hosts from Thomson and Chary, we investigate the correlation of host mass with Hubble residual observed at lower redshifts. Although the sample is small and the uncertainties are large, a hint of this relation is found at z > 0.9. By simultaneously fitting the average cluster galaxy formation history and dust content to the red-sequence scatters, we show that the reddening of early-type cluster SN hosts is likely E(B - V) {approx}< 0.06. The similarity of the field and cluster early-type host samples suggests that field early-type galaxies that lie on the red sequence may also be minimally affected by dust. Hence, the early-type-hosted SNe Ia studied here occupy a more favorable environment to use as well-characterized high-redshift standard candles than other SNe Ia.

Meyers, J.; Barbary, K.; Fakhouri, H. K.; Goldhaber, G. [Department of Physics, University of California Berkeley, Berkeley, CA 94720 (United States); Aldering, G.; Faccioli, L.; Hsiao, E. [E.O. Lawrence Berkeley National Lab, 1 Cyclotron Rd., Berkeley, CA 94720 (United States); Barrientos, L. F. [Departmento de Astronomia, Pontificia Universidad Catolica de Chile, Santiago (Chile); Brodwin, M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Dawson, K. S. [Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112 (United States); Deustua, S.; Fruchter, A. S. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Doi, M.; Ihara, Y. [Institute of Astronomy, Graduate School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015 (Japan); Eisenhardt, P. [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States); Gilbank, D. G. [Department of Physics and Astronomy, University Of Waterloo, Waterloo, Ontario, N2L 3G1 (Canada); Gladders, M. D. [Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 (United States); Gonzalez, A. H. [Department of Astronomy, University of Florida, Gainesville, FL 32611 (United States); Hattori, T. [Subaru Telescope, National Astronomical Observatory of Japan, 650 North Aohaku Place, Hilo, HI 96720 (United States); Kashikawa, N., E-mail: jmeyers314@berkeley.edu [National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Japan); Collaboration: Supernova Cosmology Project; and others

2012-05-01T23:59:59.000Z

340

PULSATING REVERSE DETONATION MODELS OF TYPE Ia SUPERNOVAE. I. DETONATION IGNITION  

SciTech Connect (OSTI)

Observational evidences point to a common explosion mechanism of Type Ia supernovae based on a delayed detonation of a white dwarf (WD). Although several scenarios have been proposed and explored by means of one, two, and three-dimensional simulations, the key point still is the understanding of the conditions under which a stable detonation can form in a destabilized WD. One of the possibilities that have been invoked is that an inefficient deflagration leads to the pulsation of a Chandrasekhar-mass WD, followed by formation of an accretion shock around a carbon-oxygen rich core. The accretion shock confines the core and transforms kinetic energy from the collapsing halo into thermal energy of the core, until an inward moving detonation is formed. This chain of events has been termed Pulsating Reverse Detonation (PRD). In this work we explore the robustness of the detonation ignition for different PRD models characterized by the amount of mass burned during the deflagration phase, M {sub defl}. The evolution of the WD up to the formation of the accretion shock has been followed with a three-dimensional hydrodynamical code with nuclear reactions turned off. We found that detonation conditions are achieved for a wide range of M {sub defl}. However, if the nuclear energy released during the deflagration phase is close to the WD binding energy ({approx}0.46 x 10{sup 51} erg {yields} M {sub defl} {approx} 0.30 M {sub sun}) the accretion shock cannot heat and confine the core efficiently and detonation conditions are not robustly achieved.

Bravo, Eduardo; GarcIa-Senz, Domingo [Department de FIsica i Enginyeria Nuclear, Universitat Politecnica de Catalunya, Diagonal 647, 08028 Barcelona (Spain)], E-mail: eduardo.bravo@upc.edu, E-mail: domingo.garcia@upc.edu

2009-04-20T23:59:59.000Z

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341

The effect of turbulent intermittency on the deflagration to detonation transition in SN Ia explosions  

E-Print Network [OSTI]

We examine the effects of turbulent intermittency on the deflagration to detonation transition (DDT) in Type Ia supernovae. The Zel'dovich mechanism for DDT requires the formation of a nearly isothermal region of mixed ash and fuel that is larger than a critical size. We primarily consider the hypothesis by Khokhlov et al. and Niemeyer and Woosley that the nearly isothermal, mixed region is produced when the flame makes the transition to the distributed regime. We use two models for the distribution of the turbulent velocity fluctuations to estimate the probability as a function of the density in the exploding white dwarf that a given region of critical size is in the distributed regime due to strong local turbulent stretching of the flame structure. We also estimate lower limits on the number of such regions as a function of density. We find that the distributed regime, and hence perhaps DDT, occurs in a local region of critical size at a density at least a factor of 2-3 larger than predicted for mean conditions that neglect intermittency. This factor brings the transition density to be much larger than the empirical value from observations in most situations. We also consider the intermittency effect on the more stringent conditions for DDT by Lisewski et al. and Woosley. We find that a turbulent velocity of $10^8$ cm/s in a region of size $10^6$ cm, required by Lisewski et al., is rare. We expect that intermittency gives a weaker effect on the Woosley model with stronger criterion. The predicted transition density from this criterion remains below $10^7$ g/cm$^3$ after accounting for intermittency using our intermittency models.

Liubin Pan; J. Craig Wheeler; John Scalo

2008-03-12T23:59:59.000Z

342

THE DETONATION MECHANISM OF THE PULSATIONALLY ASSISTED GRAVITATIONALLY CONFINED DETONATION MODEL OF Type Ia SUPERNOVAE  

SciTech Connect (OSTI)

We describe the detonation mechanism composing the 'pulsationally assisted' gravitationally confined detonation (GCD) model of Type Ia supernovae. This model is analogous to the previous GCD model reported in Jordan et al.; however, the chosen initial conditions produce a substantively different detonation mechanism, resulting from a larger energy release during the deflagration phase. The resulting final kinetic energy and {sup 56}Ni yields conform better to observational values than is the case for the 'classical' GCD models. In the present class of models, the ignition of a deflagration phase leads to a rising, burning plume of ash. The ash breaks out of the surface of the white dwarf, flows laterally around the star, and converges on the collision region at the antipodal point from where it broke out. The amount of energy released during the deflagration phase is enough to cause the star to rapidly expand, so that when the ash reaches the antipodal point, the surface density is too low to initiate a detonation. Instead, as the ash flows into the collision region (while mixing with surface fuel), the star reaches its maximally expanded state and then contracts. The stellar contraction acts to increase the density of the star, including the density in the collision region. This both raises the temperature and density of the fuel-ash mixture in the collision region and ultimately leads to thermodynamic conditions that are necessary for the Zel'dovich gradient mechanism to produce a detonation. We demonstrate feasibility of this scenario with three three-dimensional (3D), full star simulations of this model using the FLASH code. We characterized the simulations by the energy released during the deflagration phase, which ranged from 38% to 78% of the white dwarf's binding energy. We show that the necessary conditions for detonation are achieved in all three of the models.

Jordan, G. C. IV; Graziani, C.; Weide, K.; Norris, J.; Hudson, R.; Lamb, D. Q. [Flash Center for Computational Science, University of Chicago, Chicago, IL 60637 (United States); Fisher, R. T. [Department of Physics, University of Massachusetts Dartmouth, 285 Old Westport Road, North Dartmouth, MA 02740 (United States); Townsley, D. M. [Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487 (United States); Meakin, C. [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States); Reid, L. B. [NTEC Environmental Technology, Subiaco WA 6008 (Australia)

2012-11-01T23:59:59.000Z

343

Off-center ignition in type Ia supernova: I. Initial evolution and implications for delayed detonation  

E-Print Network [OSTI]

The explosion of a carbon-oxygen white dwarf as a Type Ia supernova is known to be sensitive to the manner in which the burning is ignited. Studies of the pre-supernova evolution suggest asymmetric, off-center ignition, and here we explore its consequences in two- and three-dimensional simulations. Compared with centrally ignited models, one-sided ignitions initially burn less and release less energy. For the distributions of ignition points studied, ignition within two hemispheres typically leads to the unbinding of the white dwarf, while ignition within a small fraction of one hemisphere does not. We also examine the spreading of the blast over the surface of the white dwarf that occurs as the first plumes of burning erupt from the star. In particular, our studies test whether the collision of strong compressional waves can trigger a detonation on the far side of the star as has been suggested by Plewa et al. (2004). The maximum temperature reached in these collisions is sensitive to how much burning and expansion has already gone on, and to the dimensionality of the calculation. Though detonations are sometimes observed in 2D models, none ever happens in the corresponding 3D calculations. Collisions between the expansion fronts of multiple bubbles also seem, in the usual case, unable to ignite a detonation. "Gravitationally confined detonation" is therefore not a robust mechanism for the explosion. Detonation may still be possible in these models however, either following a pulsation or by spontaneous detonation if the turbulent energy is high enough.

F. K. Roepke; S. E. Woosley; W. Hillebrandt

2006-09-04T23:59:59.000Z

344

A Three-Dimensional Picture of the Delayed-Detonation Model of Type Ia Supernovae  

E-Print Network [OSTI]

Deflagration models poorly explain the observed diversity of SNIa. Current multidimensional simulations of SNIa predict a significant amount of, so far unobserved, carbon and oxygen moving at low velocities. It has been proposed that these drawbacks can be resolved if there is a sudden jump to a detonation (delayed detonation), but this kind of models has been explored mainly in one dimension. Here we present new three-dimensional delayed detonation models in which the deflagraton-to-detonation transition (DDT) takes place in conditions like those favored by one-dimensional models. We have used a SPH code adapted to SNIa with algorithms devised to handle subsonic as well as supersonic combustion fronts. The starting point was a C-O white dwarf of 1.38 solar masses. When the average density on the flame surface reached 2-3x10^7 g/cm^3 a detonation was launched. The detonation wave processed more than 0.3 solar masses of carbon and oxygen, emptying the central regions of the ejecta of unburned fuel and raising its kinetic energy close to the fiducial 10^51 ergs expected from a healthy Type Ia supernova. The final amount of 56Ni synthesized also was in the correct range. However, the mass of carbon and oxygen ejected is still too high. The three-dimensional delayed detonation models explored here show an improvement over pure deflagration models, but they still fail to coincide with basic observational constraints. However, there are many aspects of the model that are still poorly known (geometry of flame ignition, mechanism of DDT, properties of detonation waves traversing a mixture of fuel and ashes). Therefore, it will be worth pursuing its exploration to see if a good SNIa model based on the three-dimensional delayed detonation scenario can be obtained.

Eduardo Bravo; Domingo Garcia-Senz

2007-12-04T23:59:59.000Z

345

Timescale stretch parameterization of Type Ia supernova B-band light curves  

SciTech Connect (OSTI)

R-band intensity measurements along the light curve of Type Ia supernovae discovered by the Cosmology Project (SCP) are fitted in brightness to templates allowing a free parameter the time-axis width factor w identically equal to s times (1+z). The data points are then individually aligned in the time-axis, normalized and K-corrected back to the rest frame, after which the nearly 1300 normalized intensity measurements are found to lie on a well-determined common rest-frame B-band curve which we call the ''composite curve.'' The same procedure is applied to 18 low-redshift Calan/Tololo SNe with Z < 0.11; these nearly 300 B-band photometry points are found to lie on the composite curve equally well. The SCP search technique produces several measurements before maximum light for each supernova. We demonstrate that the linear stretch factor, s, which parameterizes the light-curve timescale appears independent of z, and applies equally well to the declining and rising parts of the light curve. In fact, the B band template that best fits this composite curve fits the individual supernova photometry data when stretched by a factor s with chi 2/DoF {approx} 1, thus as well as any parameterization can, given the current data sets. The measurement of the data of explosion, however, is model dependent and not tightly constrained by the current data. We also demonstrate the 1 + z light-cure time-axis broadening expected from cosmological expansion. This argues strongly against alternative explanations, such as tired light, for the redshift of distant objects.

Goldhaber, G.; Groom, D.E.; Kim, A.; Aldering, G.; Astier, P.; Conley, A.; Deustua, S.E.; Ellis, R.; Fabbro, S.; Fruchter, A.S.; Goobar, A.; Hook, I.; Irwin, M.; Kim, M.; Knop, R.A.; Lidman, C.; McMahon, R.; Nugent, P.E.; Pain, R.; Panagia, N.; Pennypacker, C.R.; Perlmutter, S.; Ruiz-Lapuente, P.; Schaefer, B.; Walton, N.A.; York, T.

2001-04-01T23:59:59.000Z

346

Exploring Cosmological Expansion Parametrizations with the Gold SnIa Dataset  

E-Print Network [OSTI]

We use the SnIa Gold dataset to compare LCDM with 10 representative parametrizations of the recent Hubble expansion history $H(z)$. For the comparison we use two statistical tests; the usual $\\chi_{min}^2$ which is insensitive to the parametrization number of parameters, and a statistic we call the p-test which depends on both the value of $\\chi_{min}^2$ and the number $n$ of the parametrization parameters. The p-test measures the confidence level to which the parameter values corresponding to LCDM are excluded from the viewpoint of the parametrization tested. For example, for a linear equation of state parametrization $w(z)=w_0 + w_1 z$ the LCDM parameter values ($w_0=-1$, $w_1=0$) are excluded at 75% confidence level. We use a flat prior and $\\Omega_{0m}=0.3$. All parametrizations tested are consistent with the Gold dataset at their best fit. According to both statistical tests, the worst fits among the 10 parametrizations, correspond to the Chaplygin gas, the brane world and the Cardassian parametrizations. The best fit is achieved by oscillating parametrizations which can exclude the parameter values corresponding to LCDM at 85% confidence level. Even though this level of significance does not provide a statistically significant exclusion of LCDM (it is less than $2\\sigma$) and does not by itself constitute conclusive evidence for oscillations in the cosmological expansion, when combined with similar independent recent evidence for oscillations coming from the CMB and matter power spectra it becomes an issue worth of further investigation.

R. Lazkoz; S. Nesseris; L. Perivolaropoulos

2005-11-10T23:59:59.000Z

347

Power System Extreme Event Detection: The Vulnerability Frontier  

E-Print Network [OSTI]

Contingencies in Electric Power Networks, proceedings ofthe North American Power Symposium, Ames, IA, OctoberScreening in Electric Power Systems, submitted to the IEEE

Lesieutre, Bernard C.; Pinar, Ali; Roy, Sandip

2007-01-01T23:59:59.000Z

348

Table 2 -Lime use and practices on Corn, major producing states, 2001 CO GA IL IN IA KS KY MI MN MO NE NY NC ND OH PA SD TX WI Area  

E-Print Network [OSTI]

Table 2 - Lime use and practices on Corn, major producing states, 2001 CO GA IL IN IA KS KY MI MN.7 Table 2 - Lime use and practices on Corn, major producing states, 2000 CO IL IN IA KS KY MI MN MO NE NY use and practices on Corn, major producing states, 1999 CO IL IN IA KS KY MI MN MO NE NC OH SD TX WI

Kammen, Daniel M.

349

Fisica Geral IA (2010/1) Nome 1 2 3 R1 R2 R3 Media Conc  

E-Print Network [OSTI]

Fisica Geral IA (2010/1) Nome 1 2 3 R1 R2 R3 M´edia Conc 1 ANDERSON SILVEIRA SALDANHA 0.5 5.2 4.7 0.7 3.5 4.5 1.5 - - 3.57 D M´edia 2.60 4.64 5.93 5.54 6.08 8.37 4.60 #12;20 40 60 80 100 A B C D FF 23

Stariolo, Daniel Adrián

350

Ames Laboratory Ames, Iowa Argonne National Laboratory Argonne...  

Office of Environmental Management (EM)

critical technology behind many of today's electric vehicles, solar panels, and wind turbines, the National Labs have pushed the boundaries of the nation's energy technology...

351

Journal articles published by Ames Laboratory interns | The Ames...  

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

Physical Review Letters, PRL 106, 215501 (2011), 27 May 2011. Joseph H. WendelJames Evans (2010): Catalytic conversion reactions mediated by single-file diffusion in...

352

Ames Laboratory Plasma Spray (ALPS) Facility | The Ames Laboratory  

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

molten materials that are very reactive and have high melting temperatures. HVOF and Plasma spray guns and an atmospheric chamber are available. Following the early...

353

Ames Laboratory Excels in Scientific Performance | The Ames Laboratory  

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

lplaboratory-appraisal-processfy-2014. Since 2006, a standardized Performance Evaluation and Measurement Plan, or PEMP, has been utilized as a means of appraising the...

354

Ames Laboratory Forms and Documents | The Ames Laboratory  

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Research & Development Materials Preparation Center Materials Transportation Midwest Forensic Resource Center Occupational Medicine Operations Plant Protection Property Services...

355

AmesLab-ISUMap2  

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HALL CATT HALL HORTICULTURE HALL FARM HOUSE MUSEUM ROSS HALL CURTISS HALL AGRONOMY HALL LANDSCAPE ARCHITECTURE HAMILTON HALL FOOD SCIENCES BUILDING HEADY HALL EAST HALL GENERAL...

356

Scientific Programs | The Ames Laboratory  

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of Energy are used in modern clean energy technologies, including wind turbines, solar panels, electric vehicles, and energy-efficient lighting Division of Chemical and...

357

Media Resources | The Ames Laboratory  

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are brief descriptions of research projects and efforts at the Lab. You can enter search terms on the Find an Expert page to tap the expertise of our researchers as a source...

358

Training Program | The Ames Laboratory  

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

with resources on how to use some of the Laboratory's task-based systems, such as Cyber Train. To access your institutional training record, please log into Cyber Train. Remember...

359

Computer Wallpaper | The Ames Laboratory  

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Computer Wallpaper We've incorporated the tagline, Creating Materials and Energy Solutions, into a computer wallpaper so you can display it on your desktop as a constant reminder....

360

Chemical Physics | The Ames Laboratory  

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Physics FWPProject Description: Project Leader(s): James Evans, Mark Gordon Principal Investigators: James Evans, Mark Gordon, Klaus Ruedenberg, Theresa Windus Key Scientific...

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While these samples are representative of the content of NLEBeta,
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We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


361

Postdoc Fellowships | The Ames Laboratory  

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technologies in renewable energy sources of biomass, wind, water, solar energy, geothermal energy, and hydrogen and fuel cells, and energy efficiency in vehicles, industry, and...

362

Research Projects | The Ames Laboratory  

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Research Projects Basic Energy Science Projects AA (Fossil Energy) Projects EERE-VT Projects EERE-ED Projects ARPA-E Projects...

363

Travel Policy | The Ames Laboratory  

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Policy Travel Policy Travel Policy for Contractor Personnel Travel Policy Changes October 1, 2009 Per Diem Adjustments for Meals Memo or EXAMPLE...

364

Nanomaterials Information | The Ames Laboratory  

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Industrial Hygiene Nanomaterials Information Nanotechnology Awareness Training through ISU EHS Approach to Nanomaterials The Safe Handling of Unbound Engineered Nanoparticles...

365

Highlights Archive | The Ames Laboratory  

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Deformation Behavior in Materials The Long and the Short of It: Nanostructure of Thermoelectric Materials Predicting Unusual Deformation Behavior in Materials Anomaly...

366

MPC Equipment | The Ames Laboratory  

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With capabilities from simple arc casting techniques, single crystal preparation, VIM casting, to plasma spraying and high-pressure gas atomization the MPC can assist...

367

Our History | The Ames Laboratory  

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Project's existing physics program. Nobel Physicist Enrico Fermi was sure a self-sustaining chain reaction could be triggered by bombarding the uranium nucleus with thermal...

368

SULI Alumni | The Ames Laboratory  

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sector hand-drillers for water wells. The long-term goal of his work is to build a self-sustaining network for well drilling that does not require subsidization by government...

369

Readiness Review | The Ames Laboratory  

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is documented on a Readiness Review Activity Approval Form. Once the agreed upon conditions and requirements are met the review is finalized through Operational Approval...

370

Saving Energy | The Ames Laboratory  

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

the use of technology that requires less energy to perform the same function. A compact fluorescent light bulb that uses less energy than an incandescent bulb to produce the same...

371

Ombuds Program | The Ames Laboratory  

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concerns, problems or project-related ambiguities. Section 11 of the Technology Transfer Commercialization Act of 2000, Public Law 106-404 directs each USDOE National Laboratory...

372

Journal Articles | The Ames Laboratory  

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Journal Articles Journal of Forensic Sciences Bommarito, C., Sturdevant, A. and D. Szymanski. 2007. Analysis of Forensic Soil Samples via HPLC and IC. Volume 52 (1), pp. 24-30. PDF...

373

EPSCI Home | The Ames Laboratory  

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monitoring, nonproliferation of weapons of mass destruction, homeland security, and forensic science. Overview Click here to find out more about our program. Projects Current...

374

Forensic Sites | The Ames Laboratory  

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Forensic Sites Meetings, Conferences, and Short Courses MFRC Training Calendar Reports of Interest NAS Report A Guide for Forensic Science Laboratories, Educational Institutions...

375

First detection of $^{56}$Co gamma-ray lines from type Ia supernova (SN2014J) with INTEGRAL  

E-Print Network [OSTI]

We report the first ever detection of $^{56}$Co lines at 847 and 1237 keV and a continuum in the 200-400 keV band from the Type Ia supernova SN2014J in M82 with INTEGRAL observatory. The data were taken between 50th and 100th day since the SN2014J outburst. The line fluxes suggest that $0.62\\pm0.13~M\\odot$ of radioactive $^{56}$Ni were synthesized during the explosion. Line broadening gives a characteristic ejecta expansion velocity $V_e\\sim 2100\\pm 500~{\\rm km~s^{-1}}$. The flux at lower energies (200-400 keV) flux is consistent with the three-photon positronium annihilation, Compton downscattering and absorption in the $\\sim~1.4~M\\odot$ ejecta composed from equal fractions of iron-group and intermediate-mass elements and a kinetic energy $E_k\\sim 1.4~10^{51}~{\\rm erg}$. All these parameters are in broad agreement with a "canonical" model of an explosion of a Chandrasekhar-mass White Dwarf (WD), providing an unambiguous proof of the nature of Type Ia supernovae as a thermonuclear explosion of a solar mass co...

Churazov, E; Isern, J; Kndlseder, J; Jean, P; Lebrun, F; Chugai, N; Grebenev, S; Bravo, E; Sazonov, S; Renaud, M

2014-01-01T23:59:59.000Z

376

Chasing the phantom: A closer look at type Ia supernovae and the dark energy equation of state  

Science Journals Connector (OSTI)

Some recent observations provide >2? evidence for phantom dark energya value of the dark energy equation of state less than the cosmological-constant value of ?1. We focus on constraining the equation of state by combining current data from the most mature geometrical probes of dark energy: type Ia supernovae (SNe Ia) from the Supernova Legacy Survey (SNLS3), the Supernova Cosmology Project (Union2.1), and the Pan-STARRS1 survey (PS1); cosmic microwave background measurements from Planck and WMAP9; and a combination of measurements of baryon acoustic oscillations. The combined data are consistent with w=?1 for the Union2.1 sample, though they present moderate (?1.9?) evidence for a phantom value when either the SNLS3 or PS1 sample is used instead. We study the dependence of the constraints on the redshift, stretch, color, and host galaxy stellar mass of SNe, but we find no unusual trends. In contrast, the constraints strongly depend on any external H0 prior: a higher adopted value for the direct measurement of the Hubble constant (H0?71??km/s/Mpc) leads to ?2? evidence for phantom dark energy. Given Planck data, we can therefore make the following statement at 2? confidence: either the SNLS3 and PS1 data have systematics that remain unaccounted for or the Hubble constant is below 71??km/s/Mpc; else the dark energy equation of state is indeed phantom.

Daniel L. Shafer and Dragan Huterer

2014-03-06T23:59:59.000Z

377

Type Ia Supernova Discoveries at z>1 From the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution  

E-Print Network [OSTI]

We have discovered 16 Type Ia supernovae (SNe Ia) with the Hubble Space Telescope (HST) and have used them to provide the first conclusive evidence for cosmic deceleration that preceded the current epoch of cosmic acceleration. These objects, discovered during the course of the GOODS ACS Treasury program, include 6 of the 7 highest-redshift SNe Ia known, all at z>1.25, and populate the Hubble diagram in unexplored territory. The luminosity distances to these and 170 previous SNe Ia are provided. A purely kinematic interpretation of the SN Ia sample provides evidence at the > 99% confidence level for a transition from deceleration to acceleration or similarly, strong evidence for a cosmic jerk. Using a simple model of the expansion history, the transition between the two epochs is constrained to be at z=0.46 +/- 0.13. The data are consistent with the cosmic concordance model of Omega_M ~ 0.3, Omega_Lambda~0.7 (chi^2_dof=1.06), and are inconsistent with a simple model of evolution or dust as an alternative to dark energy. For a flat Universe with a cosmological constant. When combined with external flat-Universe constraints we find w=-1.02 + 0.13 - 0.19 (and $dark energy, P = w\\rho c^2. Joint constraints on both the recent equation of state of dark energy, $w_0$, and its time evolution, dw/dz, are a factor of ~8 more precise than its first estimate and twice as precise as those without the SNe Ia discovered with HST. Our constraints are consistent with the static nature of and value of w expected for a cosmological constant (i.e., w_0 = -1.0, dw/dz = 0), and are inconsistent with very rapid evolution of dark energy. We address consequences of evolving dark energy for the fate of the Universe.

Adam G. Riess; Louis-Gregory Strolger; John Tonry; Stefano Casertano; Henry C. Ferguson; Bahram Mobasher; Peter Challis; Alexei V. Filippenko; Saurabh Jha; Weidong Li; Ryan Chornock; Robert P. Kirshner; Bruno Leibundgut; Mark Dickinson; Mario Livio; Mauro Giavalisco; Charles C. Steidel; Narciso Benitez; Zlatan Tsvetanov

2004-02-23T23:59:59.000Z

378

Failed-detonation Supernovae: Subluminous Low-velocity Ia Supernovae and their Kicked Remnant White Dwarfs with Iron-rich Cores  

Science Journals Connector (OSTI)

Type Ia supernovae (SNe Ia) originate from the thermonuclear explosions of carbon-oxygen (C-O) white dwarfs (WDs). The single-degenerate scenario is a well-explored model of SNe Ia where unstable thermonuclear burning initiates in an accreting, Chandrasekhar-mass WD and forms an advancing flame. By several proposed physical processes, the rising, burning material triggers a detonation, which subsequently consumes and unbinds the WD. However, if a detonation is not triggered and the deflagration is too weak to unbind the star, a completely different scenario unfolds. We explore the failure of the gravitationally confined detonation mechanism of SNe Ia, and demonstrate through two-dimensional and three-dimensional simulations the properties of failed-detonation SNe. We show that failed-detonation SNe expel a few 0.1 M ? of burned and partially burned material and that a fraction of the material falls back onto the WD, polluting the remnant WD with intermediate-mass and iron-group elements that likely segregate to the core forming a WD whose core is iron rich. The remaining material is asymmetrically ejected at velocities comparable to the escape velocity from the WD, and in response, the WD is kicked to velocities of a few hundred km s1. These kicks may unbind the binary and eject a runaway/hypervelocity WD. Although the energy and ejected mass of the failed-detonation SN are a fraction of typical thermonuclear SNe, they are likely to appear as subluminous low-velocity SNe Ia. Such failed detonations might therefore explain or are related to the observed branch of peculiar SNe Ia, such as the family of low-velocity subluminous SNe (SN 2002cx/SN 2008ha-like SNe).

George C. Jordan, IV; Hagai B. Perets; Robert T. Fisher; Daniel R. van Rossum

2012-01-01T23:59:59.000Z

379

FAILED-DETONATION SUPERNOVAE: SUBLUMINOUS LOW-VELOCITY Ia SUPERNOVAE AND THEIR KICKED REMNANT WHITE DWARFS WITH IRON-RICH CORES  

SciTech Connect (OSTI)

Type Ia supernovae (SNe Ia) originate from the thermonuclear explosions of carbon-oxygen (C-O) white dwarfs (WDs). The single-degenerate scenario is a well-explored model of SNe Ia where unstable thermonuclear burning initiates in an accreting, Chandrasekhar-mass WD and forms an advancing flame. By several proposed physical processes, the rising, burning material triggers a detonation, which subsequently consumes and unbinds the WD. However, if a detonation is not triggered and the deflagration is too weak to unbind the star, a completely different scenario unfolds. We explore the failure of the gravitationally confined detonation mechanism of SNe Ia, and demonstrate through two-dimensional and three-dimensional simulations the properties of failed-detonation SNe. We show that failed-detonation SNe expel a few 0.1 M{sub Sun} of burned and partially burned material and that a fraction of the material falls back onto the WD, polluting the remnant WD with intermediate-mass and iron-group elements that likely segregate to the core forming a WD whose core is iron rich. The remaining material is asymmetrically ejected at velocities comparable to the escape velocity from the WD, and in response, the WD is kicked to velocities of a few hundred km s{sup -1}. These kicks may unbind the binary and eject a runaway/hypervelocity WD. Although the energy and ejected mass of the failed-detonation SN are a fraction of typical thermonuclear SNe, they are likely to appear as subluminous low-velocity SNe Ia. Such failed detonations might therefore explain or are related to the observed branch of peculiar SNe Ia, such as the family of low-velocity subluminous SNe (SN 2002cx/SN 2008ha-like SNe).

Jordan, George C. IV; Van Rossum, Daniel R. [Center for Astrophysical Thermonuclear Flashes, University of Chicago, Chicago, IL 60637 (United States); Perets, Hagai B. [Physics Department, Technion, Israel Institute of Technology, Haifa 32000 (Israel); Fisher, Robert T. [Department of Physics, University of Massachusetts Dartmouth, 285 Old Westport Road, North Dartmouth, MA 02740 (United States)

2012-12-20T23:59:59.000Z

380

He H`ike no ka Ho`opihapiha `ia o ka Pepa Noi Komo no ka Papahana Ho`omkaukau Kumu `iwi `o Kahuawaiola  

E-Print Network [OSTI]

45 a `oi ma ka pae 300 a ma luna a`e paha a e k ana n koina `lelo a mo`omeheu Hawai`i e helu `ia nei`omeheu Hawai`i. 7. ka puka `ana ma ho`okahi o n papa penei: HWST 205, 471, 472, 473, 474; a i `ole ka `ae a ka `ekolu kau kona l`ihi i kkulu `ia no ka ho`omkaukau `ana i n kumu Mauli Ola Hawai`i no ka ho`ona`auao ma

Wiegner, Tracy N.

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Testing Models of Intrinsic Brightness Variations in Type Ia Supernovae, and their Impact on Measuring Cosmological Parameters  

E-Print Network [OSTI]

For spectroscopically confirmed type Ia supernovae we evaluate models of intrinsic brightness variations with detailed data/Monte-Carlo comparisons of the dispersion in the following quantities: Hubble-diagram scatter, color difference (B-V-c) between the true B-V color and the fitted color (c) from the SALT-II light curve model, and photometric redshift residual. The data sample includes 251 ugriz light curves from the 3-season Sloan Digital Sky Survey-II, and 191 griz light curves from the Supernova Legacy Survey 3-year data release. We find that the simplest model of a wavelength independent (coherent) scatter is not adequate, and that to describe the data the intrinsic scatter model must have wavelength-dependent variations. We use Monte Carlo simulations to examine the standard approach of adding a coherent scatter term in quadrature to the distance-modulus uncertainty in order to bring the reduced chi2 to unity when fitting a Hubble diagram. If the light curve fits include model uncertainties with the c...

Kessler, Richard; Marriner, John; Betoule, Marc; Brinkmann, Jon; Cinabro, David; El-Hage, Patrick; Frieman, Joshua; Jha, Saurabh; Mosher, Jennifer; Schneider, Donald P

2012-01-01T23:59:59.000Z

382

THE EFFECT OF THE PRE-DETONATION STELLAR INTERNAL VELOCITY PROFILE ON THE NUCLEOSYNTHETIC YIELDS IN TYPE Ia SUPERNOVA  

SciTech Connect (OSTI)

A common model of the explosion mechanism of Type Ia supernovae is based on a delayed detonation of a white dwarf. A variety of models differ primarily in the method by which the deflagration leads to a detonation. A common feature of the models, however, is that all of them involve the propagation of the detonation through a white dwarf that is either expanding or contracting, where the stellar internal velocity profile depends on both time and space. In this work, we investigate the effects of the pre-detonation stellar internal velocity profile and the post-detonation velocity of expansion on the production of {alpha}-particle nuclei, including {sup 56}Ni, which are the primary nuclei produced by the detonation wave. We perform one-dimensional hydrodynamic simulations of the explosion phase of the white dwarf for center and off-center detonations with five different stellar velocity profiles at the onset of the detonation. In order to follow the complex flows and to calculate the nucleosynthetic yields, approximately 10,000 tracer particles were added to every simulation. We observe two distinct post-detonation expansion phases: rarefaction and bulk expansion. Almost all the burning to {sup 56}Ni occurs only in the rarefaction phase, and its expansion timescale is influenced by pre-existing flow structure in the star, in particular by the pre-detonation stellar velocity profile. We find that the mass fractions of the {alpha}-particle nuclei, including {sup 56}Ni, are tight functions of the empirical physical parameter {rho}{sub up}/v{sub down}, where {rho}{sub up} is the mass density immediately upstream of the detonation wave front and v{sub down} is the velocity of the flow immediately downstream of the detonation wave front. We also find that v{sub down} depends on the pre-detonation flow velocity. We conclude that the properties of the pre-existing flow, in particular the internal stellar velocity profile, influence the final isotopic composition of burned matter produced by the detonation.

Kim, Yeunjin; Jordan, G. C. IV; Graziani, Carlo; Lamb, D. Q.; Truran, J. W. [Astronomy Department, University of Chicago, Chicago, IL 60637 (United States); Meyer, B. S. [Physics and Astronomy Department, Clemson University, Clemson, SC 29634 (United States)

2013-07-01T23:59:59.000Z

383

Neutron Diffraction Residual Strain Tensor Measurements Within The Phase IA Weld Mock-up Plate P-5  

SciTech Connect (OSTI)

Oak Ridge National Laboratory (ORNL) has worked with NRC and EPRI to apply neutron and X-ray diffraction methods to characterize the residual stresses in a number of dissimilar metal weld mockups and samples. The design of the Phase IA specimens aimed to enable stress measurements by several methods and computational modeling of the weld residual stresses. The partial groove in the 304L stainless steel plate was filled with weld beads of Alloy 82. A summary of the weld conditions for each plate is provided in Table 1. The plates were constrained along the long edges during and after welding by bolts with spring-loaded washers attached to the 1-inch thick Al backing plate. The purpose was to avoid stress relief due to bending of the welded stainless steel plate. The neutron diffraction method was one of the methods selected by EPRI for non-destructive through thickness strain and stress measurement. Four different plates (P-3 to P-6) were studied by neutron diffraction strain mapping, representing four different welding conditions. Through thickness neutron diffraction strain mappings at NRSF2 for the four plates and associated strain-free d-zero specimens involved measurement along seven lines across the weld and at six to seven depths. The mountings of each plate for neutron diffraction measurements were such that the diffraction vector was parallel to each of the three primary orthogonal directions of the plate: two in-plane directions, longitudinal and transverse, and the direction normal to the plate (shown in left figure within Table 1). From the three orthogonal strains for each location, the residual stresses along the three plate directions were calculated. The principal axes of the strain and stress tensors, however, need not necessarily align with the plate coordinate system. To explore this, plate P-5 was selected for examination of the possibility that the principal axes of strain are not along the sample coordinate system axes. If adequate data could be collected the goal would be to determine the strain tensor's orientation and magnitude of strain along each principle axis direction.

Hubbard, Camden R [ORNL

2011-09-01T23:59:59.000Z

384

TESTING MODELS OF INTRINSIC BRIGHTNESS VARIATIONS IN TYPE Ia SUPERNOVAE AND THEIR IMPACT ON MEASURING COSMOLOGICAL PARAMETERS  

SciTech Connect (OSTI)

For spectroscopically confirmed Type Ia supernovae we evaluate models of intrinsic brightness variations with detailed data/Monte Carlo comparisons of the dispersion in the following quantities: Hubble-diagram scatter, color difference (B - V - c) between the true B - V color and the fitted color (c) from the SALT-II light curve model, and photometric redshift residual. The data sample includes 251 ugriz light curves from the three-season Sloan Digital Sky Survey-II and 191 griz light curves from the Supernova Legacy Survey 3 year data release. We find that the simplest model of a wavelength-independent (coherent) scatter is not adequate, and that to describe the data the intrinsic-scatter model must have wavelength-dependent variations resulting in a {approx}0.02 mag scatter in B - V - c. Relatively weak constraints are obtained on the nature of intrinsic scatter because a variety of different models can reasonably describe this photometric data sample. We use Monte Carlo simulations to examine the standard approach of adding a coherent-scatter term in quadrature to the distance-modulus uncertainty in order to bring the reduced {chi}{sup 2} to unity when fitting a Hubble diagram. If the light curve fits include model uncertainties with the correct wavelength dependence of the scatter, we find that this approach is valid and that the bias on the dark energy equation-of-state parameter w is much smaller ({approx}0.001) than current systematic uncertainties. However, incorrect model uncertainties can lead to a significant bias on the distance moduli, with up to {approx}0.05 mag redshift-dependent variation. This bias is roughly reduced in half after applying a Malmquist bias correction. For the recent SNLS3 cosmology results, we estimate that this effect introduces an additional systematic uncertainty on w of {approx}0.02, well below the total uncertainty. This uncertainty depends on the choice of viable scatter models and the choice of supernova (SN) samples, and thus this small w-uncertainty is not guaranteed in future cosmology results. For example, the w-uncertainty for SDSS+SNLS (dropping the nearby SNe) increases to {approx}0.04.

Kessler, Richard; Frieman, Joshua A. [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States)] [Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Avenue, Chicago, IL 60637 (United States); Guy, Julien; Betoule, Marc; El-Hage, Patrick [Laboratoire de Physique Nucleaire et des Hautes Energies, UPMC Univ. Paris 6, UPD Univ. Paris 7, CNRS IN2P3, 4 place Jussieu, F-75005 Paris (France)] [Laboratoire de Physique Nucleaire et des Hautes Energies, UPMC Univ. Paris 6, UPD Univ. Paris 7, CNRS IN2P3, 4 place Jussieu, F-75005 Paris (France); Marriner, John [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States)] [Center for Particle Astrophysics, Fermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510 (United States); Brinkmann, Jon [Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349 (United States)] [Apache Point Observatory, P.O. Box 59, Sunspot, NM 88349 (United States); Cinabro, David [Department of Physics, Wayne State University, Detroit, MI 48202 (United States)] [Department of Physics, Wayne State University, Detroit, MI 48202 (United States); Jha, Saurabh [Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States)] [Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States); Mosher, Jennifer [Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104 (United States)] [Department of Physics and Astronomy, University of Pennsylvania, 203 South 33rd Street, Philadelphia, PA 19104 (United States); Schneider, Donald P., E-mail: kessler@kicp.uchicago.edu [Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA 16802 (United States)

2013-02-10T23:59:59.000Z

385

Gorchakova-IA  

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

Mokhov Oboukhov Institute of Atmospheric Physics Russian Academy of Sciences Moscow, Russia T. B. Zhuravleva Institute of Atmospheric Optics Tomsk, Russia Introduction Study of...

386

Variations ia Variscan Granites  

Science Journals Connector (OSTI)

... the compositional variations within the Caledonian belt, may both be attributed to variations in the geothermal gradient. In Nature Physical Science this week (April 2), he takes these studies ... studies a stage further by showing that the correlation within the belt between composition and geothermal gradient also applies to the Variscan granites.

1973-04-06T23:59:59.000Z

387

IA News Archive  

Office of Environmental Management (EM)

field-type-text-with-summary field-label-hidden">

U.S. Secretary of Energy Ernest Moniz traveled...

388

Competition between $\\beta$-delayed proton and $\\beta$-delayed $\\gamma$ decay of the exotic $T_z$ = -2 nucleus $^{56}$Zn and fragmentation of the IAS  

E-Print Network [OSTI]

A very exotic decay mode at the proton drip-line, $\\beta$-delayed $\\gamma$-proton decay, has been observed in the $\\beta$ decay of the $T_z$ = -2 nucleus $^{56}$Zn. Three $\\gamma$-proton sequences have been observed following the $\\beta$ decay. The fragmentation of the IAS in $^{56}$Cu has also been observed for the first time. The results were reported in a recent publication. At the time of publication the authors were puzzled by the competition between proton and $\\gamma$ decays from the main component of the IAS. Here we outline a possible explanation based on the nuclear structure properties of the three nuclei involved, namely $^{56}$Zn, $^{56}$Cu and $^{55}$Ni, close to the doubly magic nucleus $^{56}$Ni. From the fragmentation of the Fermi strength and the excitation energy of the two populated 0$^{+}$ states we could deduce the off-diagonal matrix element of the charge-dependent part of the Hamiltonian responsible for the mixing. These results are compared with the decay of $^{55}$Cu with one proton ...

Rubio, B; Fujita, Y; Blank, B; Gelletly, W; Agramunt, J; Algora, A; Ascher, P; Bilgier, B; Cceres, L; Cakirli, R B; Fujita, H; Ganioglu, E; Gerbaux, M; Giovinazzo, J; Grvy, S; Kamalou, O; Kozer, H C; Kucuk, L; Kurtukian-Nieto, T; Molina, F; Popescu, L; Rogers, A M; Susoy, G; Stodel, C; Suzuki, T; Tamii, A; Thomas, J C

2015-01-01T23:59:59.000Z

389

Expectations for the Hard X-ray Continuum and Gamma-ray Line Fluxes from the Type Ia supernova SN 2014J in M82  

E-Print Network [OSTI]

The hard X-ray continuum and gamma-ray lines from a Type Ia supernova dominate its integrated photon emissions and can provide unique diagnostics of the mass of the ejecta, the $^{56}$Ni yield and spatial distribution, its kinetic energy and expansion speed, and the mechanism of explosion. Such signatures and their time behavior "X-ray" the bulk debris field in direct fashion, and do not depend upon the oftimes problematic and elaborate UV, optical, and near-infrared spectroscopy and radiative transfer that have informed the study of these events for decades. However, to date no hard photons have ever been detected from a Type Ia supernova in explosion. With the advent of the supernova SN 2014J in M82, at a distance of $\\sim$3.5 Mpc, this situation may soon change. Both NuSTAR and INTEGRAL have the potential to detect SN 2014J, and, if spectra and light curves can be measured, would usefully constrain the various explosion models published during the last $\\sim$thirty years. In support of these observational ...

The, Lih-Sin

2014-01-01T23:59:59.000Z

390

RELATIVISTIC SHOCK BREAKOUTS-A VARIETY OF GAMMA-RAY FLARES: FROM LOW-LUMINOSITY GAMMA-RAY BURSTS TO TYPE Ia SUPERNOVAE  

SciTech Connect (OSTI)

The light from a shock breakout of stellar explosions, which carries a wealth of information, strongly depends on the shock velocity at the time of the breakout. The emission from Newtonian breakouts, typical in regular core-collapse supernovae (SNe), has been explored extensively. However, a large variety of explosions result in mildly or ultrarelativistic breakouts, where the observed signature is unknown. Here we calculate the luminosity and spectrum produced by relativistic breakouts. In order to do so, we improve the analytic description of relativistic radiation-mediated shocks and follow the system from the breakout itself, through the planar phase and into the spherical phase. We limit our calculation to cases where the post-breakout acceleration of the gas ends during the planar phase (i.e., the final gas Lorentz factor {approx}< 30). We find that spherical relativistic breakouts produce a flash of gamma rays with energy, E{sub bo}, temperature, T{sub bo}, and duration, t{sup obs} b{sub o}, that provide the breakout radius ( Almost-Equal-To 5 R{sub Sun }(t{sup obs}{sub bo}/10 s)(T{sub bo}/50 keV){sup 2}) and the Lorentz factor ( Almost-Equal-To T{sub bo}/50 keV). They also always satisfy a relativistic breakout relation (t{sup obs}{sub bo}/20 s) {approx} (E{sub bo}/10{sup 46} erg){sup 1/2}(T{sub bo}/50 keV){sup -2.68}. The breakout flare is typically followed, on longer timescales, by X-rays that carry a comparable energy. We apply our model to a variety of explosions, including Type Ia and .Ia SNe, accretion-induced collapse, energetic SNe, and gamma-ray bursts (GRBs). We find that all these events produce detectable gamma-ray signals, some of which may have already been seen. Some particular examples are: (1) relativistic shock breakouts provide a natural explanation to the energy, temperature, and timescales of low-luminosity GRBs. Indeed, all observed low-luminosity GRBs satisfy the relativistic breakout relation. (2) Nearby broad-line Type Ib/c (like SN 2002ap) may produce a detectable {gamma}-ray signal. (3) Galactic Type Ia SNe may produce detectable {gamma}-ray flares. We conclude that relativistic shock breakouts provide a generic process for the production of gamma-ray flares.

Nakar, Ehud [Raymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978 (Israel); Sari, Re'em [Racah Institute for Physics, Hebrew University, Jerusalem 91904 (Israel)

2012-03-10T23:59:59.000Z

391

Solar Wind: Manifestations of Solar Activity E N CYC LO PE D IA O F AS T R O N O MY AN D AS T R O PHYS I C S Solar Wind: Manifestations of Solar  

E-Print Network [OSTI]

Solar Wind: Manifestations of Solar Activity E N CYC LO PE D IA O F AS T R O N O MY AN D AS T R O PHYS I C S Solar Wind: Manifestations of Solar Activity The Sun's outer atmosphere, the corona, is continually heated and expands to create the solar wind. Solar activity waxes and wanes with the 11 yr cycle

Webb, David F.

392

Projected rotational velocities of WD1614+136 and WD1353+409 - implications for the rate of galactic Type Ia supernovae  

E-Print Network [OSTI]

The white dwarf stars WD1614+136 and WD1353+409 are not sufficiently massive to have formed through single star evolution. However, observations to date have not yet found any evidence for binarity. It has therefore been suggested that these stars are the result of a merger. In this paper we place an upper limit of approximately 50kms on the projected rotational velocities of both stars. This suggests that, if these stars are the results of a merger, efficient angular momentum loss with accompanying mass loss must have occurred. If the same process occurs following the merging of more massive white dwarf stars, the predicted rate of Type Ia supernovae due to merging white dwarfs may have been greatly over-estimated. Further observations to determine binarity in WD1614+136 and WD1353+409 are therefore encouraged.

P. F. L. Maxted; T. R. Marsh

1998-03-17T23:59:59.000Z

393

Chandra Observation of the Cluster of Galaxies MS 0839.9+2938 at z=0.194: the Central Excess Iron and SN Ia Enrichment  

E-Print Network [OSTI]

We present the Chandra study of the intermediately distant cluster of galaxies MS 0839.9+2938. By performing both the projected and deprojected spectral analyses, we find that the gas temperature is approximately constant at about 4 keV in 130-444h_70^-1 kpc. In the inner regions, the gas temperature descends towards the center, reaching sun yr^-1 and 96-126 M_sun yr^-1, respectively within 74h_70^-1 kpc where the gas is significantly colder. Along with the temperature drop, we detect a significant inward iron abundance increase from about 0.4 solar in the outer regions to about 1 solar within the central 37h_70^-1 kpc. Thus MS 0839.9+2938 is the cluster showing the most significant central iron excess at z>~ 0.2. We argue that most of the excess iron should have been contributed by SNe Ia. By utilizing the observed SN Ia rate and stellar mass loss rate, we estimate that the time needed to enrich the central region with excess iron is 6.4-7.9 Gyr, which is similar to those found for the nearby clusters. Coinciding with the optical extension of the cD galaxy (up to about 30h_70^-1 kpc), the observed X-ray surface brightness profile exhibits an excess beyond the distribution expected by either the beta model or the NFW model, and can be well fitted with an empirical two-beta model that leads to a relatively flatter mass profile in the innermost region.

Yu Wang; Haiguang Xu; Zhongli Zhang; Yueheng Xu; Xiang-Ping Wu; Sui-Jian Xue; Zongwei Li

2005-06-12T23:59:59.000Z

394

VFP Research Projects | The Ames Laboratory  

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

Nanotubes (Madbouly) Nanocasting for a new generation of smart nanodevices (Slowing) Exploration of multi-block polymer morphologies using high performance computing...

395

Laser Decontamination of Metals | The Ames Laboratory  

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Laser Decontamination of Metals Zapping contamination with lasers may be just the answer for safely and efficiently treating some of the waste awaiting disposal across the country....

396

Career and Training Information | The Ames Laboratory  

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

from a scene of a suspected arson. Forensic Drug Chemists analyze suspected drugs of abuse such as marihuana, cocaine, and heroin. Forensic Toxicologists analyze specimens...

397

Cook This, Not That | The Ames Laboratory  

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tender steak with the crispy crust on the outside. Duh Who doesn't? And that baked potato......oh your innocence is lost so quickly when the words "Do you want that loaded?"...

398

Office of the Director | The Ames Laboratory  

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University of Maryland, and the Colorado School of Mines. Industrial partners include Simbol Materials, Inc. (California), GM (Michigan), Arnold Magnetics Technologies (New York),...

399

Federal Laboratory Consortium | The Ames Laboratory  

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Federal Laboratory Consortium The Federal Laboratory Consortium for Technology Transfer (FLC) is the nationwide network of federal laboratories that provides the forum to develop...

400

Ames Lab 101: Growing Crystals in Space  

SciTech Connect (OSTI)

Rohit Trivedi, distinguished professor of materials science and engineering, discusses his research with NASA to grow crystals in space.

Trivedi, Rohit

2011-01-01T23:59:59.000Z

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401

AME 101 Fall 2013 Problem Set #1  

E-Print Network [OSTI]

cells? A typical Proton Exchange Membrane (PEM) fuel cell requires 1 milligram of platinum per cm2 for a 100 hp fuel cell? I get about $20,000. Note that the cost of platinum and other precious metals of fuel cell area. Each cm2 of fuel cell area can generate about 0.4 amp of current. The fuel cell voltage

402

AME 101 Fall 2014 Problem Set #1  

E-Print Network [OSTI]

about fuel cells? A typical Proton Exchange Membrane (PEM) fuel cell requires 1 milligram of platinum will the platinum cost for a 100 hp fuel cell? I get about $10,000. Note that the cost of platinum and other per cm2 of fuel cell area. Each cm2 of fuel cell area can generate about 0.4 amp of current. The fuel

403

Intellectual Property Provisions | The Ames Laboratory  

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for General Contractor (rev. July 2011) Experimental, Developmental, Demonstration or Research Contract for Small Business or Non-Profit (rev. July 2011) Experimental,...

404

Ultrasonic Characterization of Wastes | The Ames Laboratory  

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technology will be giving DOE an image of the waste in some of its underground storage tanks. "This is a quick, cost-effective method for determining what's going on inside a...

405

Cyber Train Videos | The Ames Laboratory  

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Cyber Train Videos 1. Cyber Train Overview 2. Cyber Train Opt-Out Process 3. Cyber Train Complete Training 4. Submitting Course Completion Materials...

406

What We Support | The Ames Laboratory  

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Applications Deltek Costpoint Deltek Time & Expense Cognos 10 Maximo Cyber Train (Employee Training) Halogen e-Appraisal Occupational Health Manager (OHM) Central...

407

DOE / Contractor Resources | The Ames Laboratory  

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be of interest to our constituents. The Lab Plan is an annual document submitted to the DOE that discusses our mission, core capabilities and infrastructure. The Contract is the...

408

CCI Technical Projects | The Ames Laboratory  

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presented several works in ASMS conference, and worked on various ionization methods and biomass feedstock. This study is now further expanded to understand the pyrolysis kinetics...

409

Internal Audit Policy | The Ames Laboratory  

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Policy Version Number: 2 Document Number: Policy 10300.001 Effective Date: 012014 File (public): policy10300...

410

Frequently Asked Questions | The Ames Laboratory  

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epsci esha fes human-resources is mfrc mpc occ-med oipa Operations purchasing safeguards-and-security scl smds techtransfer training travel Category Is one of Is all of Is...

411

AME 101 Fall 2013 Problem Set #2  

E-Print Network [OSTI]

engine is defined as follows: TSFC = mf QR Tc where mf is the fuel mass flow rate (units mass/time), QR points) (from a previous midterm) I calculated the power production from a new type of steam turbine, Pin and Uin are the temperature, pressure and velocity of the steam going into the turbine, Tout, Pout

412

Work continues on SIF | The Ames Laboratory  

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of the six instrument bays are lined with aluminum to eliminate potential electromagnetic interference. The service corridor will also house separate HVAC units to closely...

413

Graduate Student Fellowship Program | The Ames Laboratory  

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Graduate Student Fellowship Program DOE Office of Science Graduate Fellowship Program The Department of Energy (DOE) Office of Science (SC) has established the DOE Office of...

414

Student Research Papers | The Ames Laboratory  

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

Student Research Papers Denae Clampitt Denae Clampitt Multidrug Efflux Regulator.pdf Andrew Fidler Andrew Fidler Superconduction Froth.pdf Magdalena Furczon Magdalena Furzcon...

415

Chemistry Controls Material's Nanostructure | The Ames Laboratory  

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selenium and sulfur precursors. The more strongly bound the selenium or sulfur is to phosphorous in the precursor, the lower the reactivity. The lower the reactivity, the longer...

416

Imaging Gene Expression | The Ames Laboratory  

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

Imaging Gene Expression FWPProject Description: Project Leader(s): Marit Nilsen-Hamilton Principal Investigators: George Kraus We are developing apatmers to use as cellular...

417

Internship Program Mentors | The Ames Laboratory  

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

2012) Miller, Gordon (2005, 2007) Montazami, Reza (2013) Nikolau, Basil (2012) Nilsen-Hamilton, Marit (2008, 2009, 2010, 2012, 2013) Nutter, Forrest (2006, 2008) Pecharsky, Vitalij...

418

Like Building with LEGOS | The Ames Laboratory  

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new materials with unique electrical, optical, mechanical or transport properties. "Nanoparticle self-assembly has entered the LEGO era," Travesset said. "You can really work with...

419

Novel Nanoparticle Tracking Device | The Ames Laboratory  

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

Novel Nanoparticle Tracking Device A new technique simultaneously illuminates the location, orientation and rotation in 3D of individual gold nanorods. Gold nanorods have been used...

420

SULI Areas of Research | The Ames Laboratory  

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

(Eric Cochran) Nanostructed materials for advanced catalyst design (Igor Slowing) 3D Printing of nanostructured catalytic materials (Igor Slowing) Nanoparticle superlattices by...

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to obtain the most current and comprehensive results.


421

Cutting Biofuel Production Costs | The Ames Laboratory  

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

Cutting Biofuel Production Costs Working to use sunlight to convert biomass to biofuels, researchers have found a pathway toward reducing the energy costs associated with making...

422

Zero Tension Lysimeters | The Ames Laboratory  

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

merits of this new design, Thompson has led installation of the new lysimeters at DOE's Rocky Flats Environmental Technology Site in Golden, CO, and at a waste-water disposal...

423

Mechanical R&D | The Ames Laboratory  

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Mechanical R&D Mechanical R&D provides a wide range of design, analysis, and testing services for the Laboratory(tm)s scientific programs. Mechanical Design tests and...

424

Middle School Coach Information | The Ames Laboratory  

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

Form 2015 Adult Medical Form Coach Resources: 2015 Rules Strategies for Success Sample Academic Questions "Ask a Scientist" (a resource for K-12 teachers and students) ISU...

425

Operations Strategic Planning Committee | The Ames Laboratory  

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Mark Grootveld grootveld@ameslab.gov Maggie Haaland haaland@iastate.edu Amy Harris-Tehan ajotehan@ameslab.gov Ila Haugen haugen@ameslab.gov John Hjortshoj...

426

Document Control Program | The Ames Laboratory  

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Training, Documents, & Records Document Control Program The Document Control (DC) Plan ensures that only approved, current versions of such documents are used in the workplace or...

427

EERE-ED Projects | The Ames Laboratory  

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

ED Projects Advanced Wear-Resistant Nano-composites for Increased Energy Efficiency Nanocoatings for High-Efficiency Industrial Hydraulic and Tooling Systems Ultracoatings -...

428

Biorenewable Thermoplastic Elastomers | The Ames Laboratory  

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

Biorenewable Thermoplastic Elastomers Our research group has recently discovered how to polymerize triglycerides such as soybean oil along with common monomeric feedstocks such as...

429

CCI Program Information | The Ames Laboratory  

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

will not have parking passes for campus, so give yourself time to get here on foot or bicycle or bus. A campus map can be found in the "Maps" section above. Bring vehicle...

430

Suli Program Information - Fall | The Ames Laboratory  

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

will not have parking passes for campus, so give yourself time to get here on foot or bicycle or bus. A campus map can be found in the "Maps" section above. Bring vehicle...

431

VFP Program Information | The Ames Laboratory  

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

will not have parking passes for campus, so give yourself time to get here on foot or bicycle or bus. A campus map can be found in the "Maps" section above. Bring vehicle...

432

Midwest Forensics Resource Center | The Ames Laboratory  

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Advanced Bloodstain Pattern Analysis Workshop Dates: March 31-April 4, 2014 Northeast Forensic Training Center, Bethlehem, Pennsylvania Instructors: Toby Wolson, MS and LeeAnn...

433

Partners of the MFRC | The Ames Laboratory  

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

Police Lawrence Police Department Riley County Police Department Sedgwick Regional Forensic Science Center Kentucky Michigan Oakland County Sheriff's Department Wyoming Police...

434

Research and Development | The Ames Laboratory  

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

current practice, as well as next generation methods that will change the nature of forensic science. 2011 MFRC-Funded Projects Previously Funded Projects R&D Summaries Journal...

435

Multi-Megawatt Organic Rankine Engine power plant (MORE). Phase IA final report: system design of MORE power plant for industrial energy conservation emphasizing the cement industry  

SciTech Connect (OSTI)

The Multi-Megawatt Organic Rankine Engine (MORE) program is directed towards the development of a large, organic Rankine power plant for energy conservation from moderate temperature industrial heat streams. Organic Rankine power plants are ideally suited for use with heat sources in the temperature range below 1100/sup 0/F. Cement manufacture was selected as the prototype industry for the MORE system because of the range of parameters which can be tested in a cement application. This includes process exit temperatures of 650/sup 0/F to 1110/sup 0/F for suspension preheater and long dry kilns, severe dust loading, multi-megawatt power generation potential, and boiler exhaust gas acid dew point variations. The work performed during the Phase IA System Design contract period is described. The System Design task defines the complete MORE system and its installation to the level necessary to obtain detailed performance maps, equipment specifications, planning of supporting experiments, and credible construction and hardware cost estimates. The MORE power plant design is based upon installation in the Black Mountain Quarry Cement Plant near Victorville, California.

Bair, E.K.; Breindel, B.; Collamore, F.N.; Hodgson, J.N.; Olson, G.K.

1980-01-31T23:59:59.000Z

436

Ames Lab, CMI, NEDO hold First Meeting on Rare Metals | The Ames...  

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Director Thomas Lograsso and CMI Director Alex King in CMI attended this meeting with ad hoc Japanese members including members in NEDO to exchange information about supply...

437

Consolidative Involved-Node Proton Therapy for Stage IA-IIIB Mediastinal Hodgkin Lymphoma: Preliminary Dosimetric Outcomes From a Phase II Study  

SciTech Connect (OSTI)

Purpose: To compare the dose reduction to organs at risk (OARs) with proton therapy (PT) versus three-dimensional conformal radiotherapy (3D-CRT) and intensity-modulated radiotherapy (IMRT) in patients with mediastinal Hodgkin lymphoma (HL) enrolled on a Phase II study of involved-node radiotherapy (INRT). Methods and Materials: Between June 2009 and October 2010, 10 patients were enrolled on a University of Florida institutional review board-approved protocol for de novo 'classical' Stage IA-IIIB HL with mediastinal (bulky or nonbulky) involvement after chemotherapy. INRT was planned per European Organization for Research and Treatment of Cancer guidelines. Three separate optimized plans were developed for each patient: 3D-CRT, IMRT, and PT. The primary end point was a 50% reduction in the body V4 with PT compared with 3D-CRT or IMRT. Results: The median relative reduction with PT in the primary end point, body V4, was 51% compared with 3D-CRT (p = 0.0098) and 59% compared with IMRT (p = 0.0020), thus all patients were offered treatment with PT. PT provided the lowest mean dose to the heart, lungs, and breasts for all 10 patients compared with either 3D-CRT or IMRT. The median difference in the OAR mean dose reduction with PT compared with 3D-CRT were 10.4 Gy/CGE for heart; 5.5 Gy/CGE for lung; 0.9 Gy/CGE for breast; 8.3 Gy/CGE for esophagus; and 4.1 Gy/CGE for thyroid. The median differences for mean OAR dose reduction for PT compared with IMRT were 4.3 Gy/CGE for heart, 3.1 Gy/CGE for lung, 1.4 Gy/CGE for breast, 2.8 Gy/CGE for esophagus, and 2.7 Gy/CGE for thyroid. Conclusions: All 10 patients benefitted from dose reductions to OARs with PT compared with either 3D-CRT or IMRT. It is anticipated that these reductions in dose to OAR will translate into lower rates of late complications, but long-term follow-up on this Phase II INRT study is needed.

Hoppe, Bradford S., E-mail: bhoppe@floridaproton.org [University of Florida Proton Therapy Institute, Jacksonville, FL (United States); Flampouri, Stella; Su Zhong; Morris, Christopher G. [University of Florida Proton Therapy Institute, Jacksonville, FL (United States); Latif, Naeem [University of Florida Hematology/Oncology, Jacksonville, FL (United States); Dang, Nam H.; Lynch, James [University of Florida Hematology/Oncology, Gainesville, FL (United States); Li Zuofeng; Mendenhall, Nancy P. [University of Florida Proton Therapy Institute, Jacksonville, FL (United States)

2012-05-01T23:59:59.000Z

438

IA_50m_Wind  

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

Metadata also available as Metadata: IdentificationInformation DataQualityInformation SpatialDataOrganizationInformation SpatialReferenceInformation EntityandAttributeI...

439

+ . -. . -. . .__ .. .. -..---. ---.. . --. --. -. L IA Science Service Feature  

E-Print Network [OSTI]

, "the bent'' - i.e.9 ''Also it is P l * t l Y the A l l The thermometer reading alone merely tella us with heat vhen the thermometer the temperature of the air to be far below freezing. In Arizona people mny

440

"Report Date","U.S.",,,"PADD I",,,"PADD IA",,,"PADD IB",,,"PADD IC",,,"PADD II"  

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

Residential Heating Oil Prices (Before and After Change in Aggregation Methodology)" Residential Heating Oil Prices (Before and After Change in Aggregation Methodology)" "Report Date","U.S.",,,"PADD I",,,"PADD IA",,,"PADD IB",,,"PADD IC",,,"PADD II" ,"Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference","Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference","Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference","Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference","Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference","Old Reported Value ($ per Gallon)","New Revised Value ($ per Gallon)","Difference"

Note: This page contains sample records for the topic "ames ia 630-252-3721" from the National Library of EnergyBeta (NLEBeta).
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441

Microsoft PowerPoint - Joel Riekin.pptx  

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

University University Iowa State University of Science and Technology Simplified Powder Processing and Microstructural Control of Fe-based ODS Alloys Support from the Department of Energy-Office of Fossil Energy is gratefully acknowledged through Ames Laboratory contract no. DE-AC02-07CH11358 J. R. Rieken 1 , I.E. Anderson 2 , and M.J. Kramer 2 1 Materials Science and Engineering, Iowa State University, Ames, IA 2 Division of Materials Sciences and Engineering, Ames Laboratory (USDOE), Ames, IA "Fe-Based ODS Alloys: Role and Future Applications" Fabrication, Microstructure Preservation & Mechanical Properties University of California-San Diego: November 18th, 2010, San Diego, CA Iowa State University Iowa State University of Science and Technology Future Generation Power Reactors

442

SciTech Connect: "light emitting diode"  

Office of Scientific and Technical Information (OSTI)

"light emitting diode" Find "light emitting diode" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office,

443

SciTech Connect: enriched uranium  

Office of Scientific and Technical Information (OSTI)

enriched uranium Find enriched uranium Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

444

SciTech Connect: auroras  

Office of Scientific and Technical Information (OSTI)

auroras Find auroras Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

445

SciTech Connect: "plasma science"  

Office of Scientific and Technical Information (OSTI)

plasma science" Find plasma science" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

446

SciTech Connect: "Greenhouse Effect"  

Office of Scientific and Technical Information (OSTI)

Greenhouse Effect" Find Greenhouse Effect" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

447

SciTech Connect: higgs  

Office of Scientific and Technical Information (OSTI)

higgs Find higgs Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

448

SciTech Connect: "fuel cells"  

Office of Scientific and Technical Information (OSTI)

fuel cells" Find fuel cells" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

449

SciTech Connect: plasma  

Office of Scientific and Technical Information (OSTI)

plasma Find plasma Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

450

SciTech Connect: "enriched uranium"  

Office of Scientific and Technical Information (OSTI)

enriched uranium" Find enriched uranium" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

451

SciTech Connect: "high temperature superconductivity"  

Office of Scientific and Technical Information (OSTI)

high temperature superconductivity" Find high temperature superconductivity" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office,

452

SciTech Connect: "oil shale"  

Office of Scientific and Technical Information (OSTI)

oil shale" Find oil shale" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

453

SciTech Connect: "higgs boson"  

Office of Scientific and Technical Information (OSTI)

higgs boson" Find higgs boson" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

454

SciTech Connect: "geomagnetic storms"  

Office of Scientific and Technical Information (OSTI)

geomagnetic storms" Find geomagnetic storms" Find How should I search Scitech Connect ... Basic or Advanced? Basic Search Advanced × Advanced Search Options Full Text: Bibliographic Data: Creator / Author: Name Name ORCID Title: Subject: Identifier Numbers: Research Org.: Sponsoring Org.: Site: All Alaska Power Administration, Juneau, Alaska (United States) Albany Research Center (ARC), Albany, OR (United States) Albuquerque Complex - NNSA Albuquerque Operations Office, Albuquerque, NM (United States) Amarillo National Resource Center for Plutonium, Amarillo, TX (United States) Ames Laboratory (AMES), Ames, IA (United States) Argonne National Laboratory (ANL), Argonne, IL (United States) Argonne National Laboratory-Advanced Photon Source (United States) Atlanta Regional Office, Atlanta, GA (United States) Atmospheric Radiation Measurement (ARM)

455

Ames Lake, Washington: Energy Resources | Open Energy Information  

Open Energy Info (EERE)

328784°, -121.9662307° 328784°, -121.9662307° 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":47.6328784,"lon":-121.9662307,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

456

Cost Share-Cost Reimbursement Invoice Format Example | The Ames...  

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

Share-Cost Reimbursement Invoice Format Example Effective Date: 102014 File (public): Cost Share-Cost...

457

Ames Laboratory | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

and Productivity of R&D) NA Construction and Operation of Research Facilities B+ S&T ProjectProgram Management B+ Contractor LeadershipStewardship B+ Environment, Safety...

458

Intern experience NASA Ames Research Center: an internship report  

E-Print Network [OSTI]

year 1986) and bringing the project in within budget. When contact was made with NASA Headquarters to inquire about early release of funds, the first response was a question as to why the project was five months behind schedule. A constraint... Code EEF. This project was assigned to Code EEE instead as a means of both broadening EEE's experience and reducing the workload of EEF. Further, the project required early design and bidding of the compressor system for the project which...

Steinle, Frank W.

2013-03-13T23:59:59.000Z

459

Simulation and Modeling of Transient Electronics | The Ames Laboratory  

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Simulation and Modeling of Transient Electronics Transient materials is an emerging area of materials design with the key attribute being the ability to physically dissolve into...

460

Making Maps of the Molecules in Seeds | The Ames Laboratory  

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

Making Maps of the Molecules in Seeds Scientists have advanced methods to make maps of the locations of molecules within plant materials. Resolution of 10 to 50 microns, less than...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Environmentally Benign Repair of Composites | The Ames Laboratory  

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

of this project is to design and evaluate a new class of environmentally benign, low viscosity resins reinforced with nanosize alumina particles. The use temperature for these...

462

Ames Lab 101: BAM (Boron-Aluminum-Magnesium)  

ScienceCinema (OSTI)

Materials scientist, Bruce Cook, discusses the super hard, low friction, and lubricious alloy know as BAM (Boron-Aluminum-Magnesium). BAM was discovered by Bruce Cook and his team a

Bruce Cook

2013-06-05T23:59:59.000Z

463

Ames Laboratory | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Directed Research and Development (LDRD) Management & Operating (M&O) Contracts Technology Transfer Work for Others Contact Information Laboratory Policy U.S. Department of Energy...

464

Ames Laboratory to Lead New Research Effort to Address Shortages...  

Energy Savers [EERE]

"Rare earth metals and other critical materials are essential to manufacturing wind turbines, electric vehicles, advanced batteries and a host of other products that are...

465

Critical Materials and Rare Futures: Ames Laboratory Signs a...  

Energy Savers [EERE]

and lasers, as well as clean-energy technologies such as electric vehicles and wind turbines. For example, the best magnets for efficient electric motors - which can be found...

466

AME 436, 2nd Midterm Exam Study Guide  

E-Print Network [OSTI]

BACKWARDS AND FORWARDS! · Otto and Diesel cycles and variations (e.g. complete expansion) · Cycle in unsteady flow engines · Knock · What is it and why is it bad? · Effect of fuel type and fuel structure) (5 points) Would this engine be more or less likely to knock than the same engine (i.e. same

467

Warning: Single Lane Tunnel Ahead | The Ames Laboratory  

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

Catalytic Reaction in Nanoporous Materials Author(s): David M. Ackerman, Jing Wang, and James W. Evans Article Link: http:dx.doi.org10.1103PhysRevLett.108.228301 Journal...

468

Kinetic Theory of Turbulent Multiphase Phase | The Ames Laboratory  

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

of such processes include coalbiomass gasifiers, petrochemical processing and polyethylene manufacture. In these applications, robust control of the process depends on...

469

Forensic Science Education Programs in the Midwest | The Ames...  

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

Science Education Programs in the Midwest Carroll University Bachelor of Science Degree (B.S.), Chemistry Major with a Forensic Science emphasis Chemistry Program | Forensic...

470

Two Ames Laboratory Science Interns are Awarded Prestigious Scholarshi...  

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

journals following their SULI appointments -- Grajeda in a 2012 issue of Chemistry of Materials and Lindemann in a 2013 issue of Journal of Organic Electronics. Since...

471

A Mystery at Cryogenic Temperatures | The Ames Laboratory  

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

A Mystery at Cryogenic Temperatures Scientists have discovered a fascinating secret about praseodymium aluminide. When PrAl2 is cooled, its crystal structure changes from high...

472

Road Blocks Yield Key Information about a Catalyst | The Ames...  

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

Road Blocks Yield Key Information about a Catalyst Researchers systematically blocked key chemical reaction pathways to get unambiguous information about how carbon-nitrogen bonds...

473

Cooperative Catalyst leads to Transformative Results | The Ames...  

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

Cooperative Catalyst leads to Transformative Results Capitalizing on the concept that everything proceeds faster with a little cooperation, researchers showed how designing...

474

Expulsion Leads to a New Catalyst | The Ames Laboratory  

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

Expulsion Leads to a New Catalyst Locating a catalyst and reactants in confined spaces makes catalytic reactions go faster in the desired direction. Of course, the reaction...

475

Spedding entry closed due to falling debris | The Ames Laboratory  

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Spedding entry closed due to falling debris Facilities and Engineering Services, with concurrence from ESH&A, has closed the front (north) entrance of Spedding Hall to all but...

476

Information Technology Advisory Group (iTAG) | The Ames Laboratory  

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

consists of: Diane Den Adel (Information Services Representative) Terry Herrman (Engineering Services Group Representative) Nathan Humeston (Science and Technology...

477

Travel Policy for Contractor Personnel | The Ames Laboratory  

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

Travel Policy for Contractor Personnel Version Number: 3 Document Number: Policy 48300.005 Effective Date: 022013 File (public): Policy48300.005rev3.pdf...

478

Insider turns 25 this month | The Ames Laboratory  

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

students who served as interpreters with the Chinese engineers installing the steam engine. Inside the first issue, was an article with photos of the service award winners,...

479

PROHIBITED PURCHASES for the Ames Laboratory Purchase Card  

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

USB Flash Memory Services Any service requiring a signed contract Advertising (unless approved by the Accounting Manager) Construction Services & Repair of...

480

Seminar by Brain Laird (Friday, October 24) | The Ames Laboratory  

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

Seminar by Brain Laird (Friday, October 24) Brain Laird, University of Kansas Department of Chemistry Chair, and Professor, will present "Premelting and Prefreezing at the...

Note: This page contains sample records for the topic "ames ia 630-252-3721" 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

Forensic Science Education Programs in the Midwest | The Ames...  

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

Forensic Science Education Programs in the Midwest Carroll University Bachelor of Science Degree (B.S.), Chemistry Major with a Forensic Science emphasis Chemistry Program |...

482

3D Printing of nanostructured catalytic materials | The Ames...  

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

3D Printing of nanostructured catalytic materials Over the last couple of decades, scientists have been able to develop a tremendous control over the synthesis and properties of...

483

AME CURRICULUM GUIDE SPRING 2014 AUDIO AND MUSIC ENGINEERING  

E-Print Network [OSTI]

choose to earn a Master of Science degree in Electrical Engineering with as little as one additional year manufacturing, audio software development, music and audio recording and production, core audio and signal processing technologies and component manufacturing, musical instruments and audio equipment manufacturing

Mahon, Bradford Z.

484

Making Materials out of Hairy Nanocubes | The Ames Laboratory  

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

out of Hairy Nanocubes Researchers have developed the first theoretical model of the self-assembly of nanocubes that have been coated with polymers, including DNA and have...

485

Ames Lab 101: BAM (Boron-Aluminum-Magnesium)  

SciTech Connect (OSTI)

Materials scientist, Bruce Cook, discusses the super hard, low friction, and lubricious alloy know as BAM (Boron-Aluminum-Magnesium). BAM was discovered by Bruce Cook and his team a

Bruce Cook

2012-08-18T23:59:59.000Z

486

MFRC Blood Pattern Analysis Videos | The Ames Laboratory  

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

15Aa2 Coughed blood 15Ab2 Gentle exhalation over two drops of blood on lips 15Ac3 Cough through bloodied lips 15Ad2 Blood expelled from nose 1Aa2 Blood dripping from a wrench...

487

Funded LDRD Projects FY2014 | The Ames Laboratory  

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

13 to 9302016 PI: Igor Slowing Title: Customized Assembly of Catalytic Systems by 3D Printing Technology Strategic Initiative: Catalysis (GRACE) Category: Chemistry Mission:...

488

Ames Laboratory 3D printing technology research taking shape...  

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

3D printing technology research taking shape Contacts: For Release: Sept. 23, 2014 Igor Slowing, Chemical and Biological Sciences, 515-294-1959 Laura Millsaps, Public Affairs,...

489

3D Tracking at the Nanoscale | The Ames Laboratory  

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

3D Tracking at the Nanoscale A new theory shows that reactivity at catalytic sites inside narrow pores is controlled by how molecules move at the pore openings. Like cars...

490

Ames Lab Interns Make Their Research Mark in Industry, Academia...  

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

model catalytic activation, which has applications in energy conversion and environmental remediation. George Scott, Science Undergraduate Laboratory Internship - 2007 M.S.,...

491

Decades-long Mystery Solved | The Ames Laboratory  

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

The Fenton reaction involves iron and hydrogen peroxide and is used to treat wastewater worldwide. Does the reaction involve a radical intermediate? Or, is it the...

492

Turtles and spooks invade Lab for Halloween | The Ames Laboratory  

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

as the TMNTs' sensei, Splinter and Deb Covey came as April O'Neil, a TV reporter and turtle companion. Rounding out the crew were four apprentice turtles: Diamond Vogel (Melinda...

493

Neutron Spin Resonance in Iron-based Superconductors | The Ames...  

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Neutron Spin Resonance in Iron-based Superconductors The propagation of a novel magnetic excitation in the superconducting state, called a spin resonance, has been observed in iron...

494

Nuclear Computational Low Energy Initiative (NUCLEI) | The Ames...  

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in nuclei, few body systems, and electroweak processes), NIF (light-ion thermonuclear reactions in a terrestrially controlled plasma environment), MAJORANA and FNPB...

495

Physical Organic Chemistry of Reactive Intermediates | The Ames...  

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

Physical Organic Chemistry of Reactive Intermediates The Jenks group specializes in physical organic chemistry, the "how" of organic reactions. Much of the work has centered on...

496

Watching the Nanoparticles Go Round and Round | The Ames Laboratory  

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

Nanoparticles Go Round and Round Until now, watching the detailed spinning motion of nano-objects within living cells has been impossible. Combining an existing technique, known...

497

New Catalysts for Green Diesel | The Ames Laboratory  

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

New Catalysts for Green Diesel A new economical and efficient catalyst for upgrading renewable feedstocks to green diesel has been created. Green diesel, produced by converting...

498

Biobased Adhesives from biodiesel coproduct streams | The Ames...  

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

Biobased Adhesives from biodiesel coproduct streams Our research group has recently discovered how to polymerize triglycerides such as soybean oil along with common monomeric...

499

Hints for a healthy heart (month) | The Ames Laboratory  

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

Hints for a healthy heart (month) So January is over and we start the month of February knowing that Cupid is supposed to show up on February 14th and shoot an arrow in our butt...

500

Analytical Instrumentation for the MFRC | The Ames Laboratory  

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

These systems were acquired to allow more hands-on training opportunities for forensic scientists through the MFRC training programs, as well as to provide research...