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Note: This page contains sample records for the topic "difference star center" from the National Library of EnergyBeta (NLEBeta).
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they are not comprehensive nor are they the most current set.
We encourage you to perform a real-time search of NLEBeta
to obtain the most current and comprehensive results.


1

ENERGY STAR Score for Data Centers  

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

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

2

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

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

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

3

ENERGY STAR Success Story: The Virginia Beach Convention Center | ENERGY  

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

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

4

ENERGY STAR Success Story San Diego Convention Center  

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

ENERGY STAR Success Story ENERGY STAR Success Story San Diego Convention Center Since opening 20 years ago, San Diego's bayside convention facility has been a green industry leader and continues to receive accolades for environmental stewardship. The San Diego Convention Center Corporation (SDCCC) joined the Environmental Protection Agency's (EPA) ENERGY STAR program as a partner in 2008. Using the EPA's online energy management and tracking tool, Portfolio Manager, the SDCCC tracked its energy consumption and has improved the facility's overall performance. Since then, the San Diego Convention Center has become a model for other convention and meeting facilities demonstrating the value of benchmarking to improve efficiency and to save money. . The Convention Center is managed and marketed by the SDCCC, a non-profit public

5

Discovery of hot supergiant stars near the Galactic center  

E-Print Network [OSTI]

We report new results of a campaign to find Wolf-Rayet and O (WR/O) stars and high-mass X-ray binaries (HMXBs) in the Galactic center. We searched for candidates by cross-correlating the 2MASS catalog with a deep Chandra catalog of X-ray point sources in the Radio Arches region. Following up with K-band spectroscopy, we found two massive stellar counterparts to CXOGC J174555.3-285126 and CXOGC J174617.0-285131, which we classify as a broad-lined WR star of sub-type WN6b and an O Ia supergiant, respectively. Their X-ray properties are most consistent with those of known colliding-wind binaries in the Galaxy and the Large Magellanic Cloud, although a scenario involving low-rate accretion onto a compact object is also possible. The O Ia star lies 4.4 pc in projection from the Quintuplet cluster, and has a radial velocity consistent with that of the Quintuplet, suggesting that this star might have escaped from the cluster. We also present the discovery of a B2 Ia supergiant, which we identified as a candidate massive star using 8 micron Spitzer maps of the Galactic center in a region near the known massive X-ray-emitting star CXOGC J174516.1-290315. We discuss the origin of these stars in the context of evolving stellar clusters in the Galactic center.

Jon C. Mauerhan; Michael P. Muno; Mark Morris

2007-03-08T23:59:59.000Z

6

Industrial energy management information center | ENERGY STAR Buildings &  

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

energy management information center energy management information center Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance Industrial service and product providers Earn recognition Market impacts: Improvements in the industrial sector

7

ENERGY STAR Success Story VA Beach Convention Center  

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

STAR Success Story: STAR Success Story: The Virginia Beach Convention Center Located in Virginia's most populous city, the Virginia Beach Convention Center (VBCC) comprises more than 516,000 square feet and typically hosts 400 events a year. Fully opened in 2007, the VBCC has served as the anchor for the successful revitalization of Virginia Beach's old beach district. With historical references and maritime themes integrated into the structure's modern design, the Center features many technological advances that make it a prime location for meetings, conferences, and trade shows. However, even with a newly constructed building, the VBCC has demonstrated an important energy management principle: all buildings, regardless of their age and building systems they employ, can reduce energy consumption, save money, and offset greenhouse gas

8

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

Quarterly Sampling, STAR Center, Largo, FL Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F33211 Sampling Dates: 07/13/05 - 07/14/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

9

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

Quarterly Sampling, STAR Center, Largo, FL Quarterly Sampling, STAR Center, Largo, FL 7030-226 Accutest Job Number: F27229 Sampling Date: 10/07/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

10

ENERGY STAR Success Story Fleet Science Center Dec 2009  

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

ENERGY STAR Success Story: Reuben H. Fleet Science Center The Reuben H. Fleet Science Center (the Fleet) is one of twenty-four arts, science, and cultural institutions that are part of San Diego's Balboa Park Cultural Partnership. The Partnership launched a sustainability initiative in 2008 along with the City of San Diego and San Diego Gas & Electric ® (SDG&E) with the goal of improving energy efficiency and reducing resource consumption at the Park's cultural institutions. To date, Balboa Park venues have decreased electricity usage by more than 3.5 million kWh and 87,000 therms of natural gas, realizing savings of $530,000. Built in 1973, the Fleet serves as a leader and a model in environmental sustainability to venues of Balboa Park and other entertainment facilities across the country. For over a decade, the Fleet has

11

S M Stoller Star Center-B100  

Office of Legacy Management (LM)

/19/06 /19/06 Technical Report for S M Stoller Star Center-B100 110406202 7031-877 Accutest Job Number: F41217 Sampling Date: 06/02/06 Report to: US Dept of Energy, Grand Jct Office 2597 B3/4 Road Grand Junction, CO 81503 ATTN: Contracts Department, PO# 24231 x Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference

12

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

2/04 2/04 Technical Report for S M Stoller Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F25409 Sampling Dates: 07/13/04 - 07/14/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

13

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

0/06 0/06 Technical Report for S M Stoller Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F39137 Sampling Dates: 03/08/06 - 03/09/06 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

14

PROJECT SCIENTIST II NOAA NESDIS Center for Satellite Applications and Research (STAR)  

E-Print Network [OSTI]

PROJECT SCIENTIST II NOAA NESDIS Center for Satellite Applications and Research (STAR) College Park Visiting Scientist Programs is seeking a Project Scientist II to work at the NOAA NESDIS Center design and implementation and the development of common tools and procedures for STAR researchers

Droegemeier, Kelvin K.

15

Blue Star Memorial By-Way Dedication: Weldon Spring Interpretive Center |  

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

Blue Star Memorial By-Way Dedication: Weldon Spring Interpretive Blue Star Memorial By-Way Dedication: Weldon Spring Interpretive Center Blue Star Memorial By-Way Dedication: Weldon Spring Interpretive Center July 12, 2013 - 1:04pm Addthis Since 2003, the Lewis and Clark Garden Club (LCGC) of St. Charles County, Missouri, has held their monthly meetings in the Weldon Spring Interpretive Center (WSIC). The LCGC has 22 active members and takes care of 2 garden beds at the WSIC Native Plant Educational Garden under the site's Adopt-A-Garden program. In 2010 the LCGC contacted the U.S. Department of Energy (DOE), seeking approval to install a Blue Star Memorial By-Way Marker as a tribute to the nation's armed forces (see bottom of page for a history of the Blue Star Memorials). A 2,300-pound pink mica memorial marker was placed

16

1STAR Seminar, NOAA Science Center, 8 Jan 2008 Impact of GOES Spacecraft Stabilization  

E-Print Network [OSTI]

Programs, NSOF, 30 Oct 2007 Lessons learned during a major transition are useful to both MTG and GOES-R #12 at the Earth #12;6STAR Seminar, NOAA Science Center, 8 Jan 2008 The process of quantitatively defining

Kuligowski, Bob

17

S M Stoller Star Center-B100 Monthly/Effluent; Largo, FL  

Office of Legacy Management (LM)

Water Date Received: 010506 Percent Solids: na Project: Star Center-B100 General Chemistry Analyte Result RL Units DF Analyzed By Method Hardness, Total as CaCO3 372 4.0 mgl...

18

Ejection of hypervelocity stars by the (binary) black hole(s) in the Galactic center  

E-Print Network [OSTI]

We study three processes that eject hypervelocity (>10^3 km/s) stars from the Galactic center: (i) close encounters of two single stars; (ii) tidal breakup of binary stars by the central black hole, as originally proposed by Hills; and (iii) three-body interactions between a star and a binary black hole (BBH). Mechanism (i) expels hypervelocity stars to the solar radius at a negligible rate, ~10^{-11}/yr. Mechanism (ii) expels hypervelocity stars at a rate ~ 10^{-5}(\\eta/0.1)/yr, where \\eta is the fraction of stars in binaries with semimajor axis a_b<~0.3 AU. For solar-mass stars, the corresponding number of hypervelocity stars within the solar radius R_0=8 kpc is ~60(\\eta/0.1)(a_b/0.1 AU)^{1/2}. For mechanism (iii), Sgr A^* is assumed to be one component of a BBH. We constrain the allowed parameter space (semimajor axis, mass ratio) of the BBH. In the allowed region (for example, semimajor axis of 0.5x10^{-3} pc and mass ratio of 0.01), the rate of ejecting hypervelocity stars can be as large as ~10^{-4}/yr and the expected number of hypervelocity stars within the solar radius can be as large as ~10^3. Hypervelocity stars may be detectable by the next generation of large-scale optical surveys.

Qingjuan Yu; Scott Tremaine

2003-09-03T23:59:59.000Z

19

Coronal versus photospheric abundances of stars with different activity levels  

E-Print Network [OSTI]

We report a detailed analysis of the coronal abundance of 4 stars with varying levels of activity and with accurately known photospheric abundances. The coronal abundance is determined here using a line flux analysis and a full determination of the differential emission measure. Photospheric abundance values are taken from literature works. Previous coronal abundance determinations have generally been compared to solar photospheric abundances; from this a number of general properties have been inferred, such as the presence of a coronal metal depletion with an inverse First Ionization Potential correlated with activity level. Here we show that, when coronal abundances are compared with real photospheric values for the individual stars, the resulting pattern can be very different. Also, we present evidence that, in some cases, the coronal metal abundance may not be uniform in the corona; in particular it can vary with the temperature of the emitting plasma.

J. Sanz-Forcada; F. Favata; G. Micela

2003-11-16T23:59:59.000Z

20

Energy Loss of Neutrinos in 20M{center_dot} Star  

SciTech Connect (OSTI)

Current ideas on neutrino oscillation plus confirmation from neutrino experiments make possible the changing of neutrino flavor due to interactions with the electrons in medium. When neutrinos pass through a medium and interact with the electrons, an effective potential energy is produced due to coherent forward scattering that occurred in the medium. This potential engenders significant changes in the neutrino masses and their mixing in the medium. Thus electron neutrinos would oscillate into different mass eigenstate and this is dependent on the energy of the neutrinos. Some of the energy will be lost in the coherent scattering with the electrons by the charged current interaction. We have calculated the energy loss of the neutrinos by using a stopping power equation for a 20M{center_dot} star.

Ahmad, Nor Sofiah; Yusof, Norhasliza; Kassim, Hasan Abu [Department of Physics, University of Malaya, 50603, Kuala Lumpur (Malaysia)

2010-08-12T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

Energy Loss of Neutrinos in 20 M{sub {center_dot}} and 40 M{sub {center_dot}} Massive Stars  

SciTech Connect (OSTI)

The progress from the theoretical and experimental aspects in neutrino physics shines light into neutrino physics as well as in astrophysics. It is known that when neutrinos pass through a medium, the neutrinos interact with electrons before emerging from the stars with an effective potential energy produced due to coherent forward scatterings that occurred in the medium. This potential engenders significant changes in the neutrino masses and their mixing in the medium. Thus electron neutrinos would oscillate into different mass eigenstate and this is dependent on the energy of the neutrinos. Some of the energy will be lost in the coherent scattering with the electrons by the charged current interaction. We have calculated the energy loss of the neutrinos by using a stopping power equation for both rotating and non-rotating 20 M{sub {center_dot}} and 40 M{sub {center_dot}} stars. The total energy loss of neutrinos depends on the electron density in the stars and on the survival probability of the electron neutrino. For high electron density profile and the survival probability, the energy loss will be significant.

Sofiah Ahmad, Nor; Yusof, Norhasliza; Abu Kassim, Hasan [Department of Physics, University of Malaya, 50603 Kuala Lumpur (Malaysia)

2011-03-30T23:59:59.000Z

22

Quarterly Progress Report for the Young-Rainey STAR Center's 4.5 Acre Site  

Office of Legacy Management (LM)

3-TAC 3-TAC GJO-PIN 25.5.1 Pinellas Environmental Restoration Project January through March 2003 Quarterly Progress Report for the Young-Rainey STAR Center's 4.5 Acre Site April 2003 Grand Junction Office U.S. Department of Energy Work Performed Under DOE Contract No. for the U.S. Department of Energy DE-AC13-02GJ79491 Approved for public release; distribution is unlimited. N0060800 GJO-2003-433-TAC GJO-PIN 25.5.1 Pinellas Environmental Restoration Project Quarterly Progress Report for the Young - Rainey STAR Center's 4.5 Acre Site January through March 2003 April 2003 Prepared by U.S. Department of Energy Grand Junction Office Grand Junction, Colorado Work Performed Under DOE Contract Number DE-AC13-02GJ79491 Task Order Number ST03-107

23

S M Stoller Pinellas Environmental Restoration Project - Young - Rainey Star Center  

Office of Legacy Management (LM)

Young - Rainey Star Center Young - Rainey Star Center 110406202 Accutest Job Number: F30886 Sampling Date: 04/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

24

S M Stoller STAR Center- 4.5 Acre Site, Largo, FL  

Office of Legacy Management (LM)

STAR Center- 4.5 Acre Site, Largo, FL STAR Center- 4.5 Acre Site, Largo, FL 110406202 Accutest Job Number: F25243 Sampling Date: 07/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

25

S M Stoller Pinellas Environmental Restoration Project - Young - Rainey Star Center  

Office of Legacy Management (LM)

Young - Rainey Star Center Young - Rainey Star Center 110406202 Accutest Job Number: F35489 Sampling Date: 10/05/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

26

S M Stoller STAR Center- 4.5 Acre Site, Largo, FL  

Office of Legacy Management (LM)

STAR Center- 4.5 Acre Site, Largo, FL STAR Center- 4.5 Acre Site, Largo, FL 7030-226/Monthly Accutest Job Number: F27168 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

27

S M Stoller Pinellas Environmental Restoration Project - Young- Rainey Star Center  

Office of Legacy Management (LM)

Pinellas Environmental Restoration Project - Young- Rainey Star Center Pinellas Environmental Restoration Project - Young- Rainey Star Center 7030-226 Accutest Job Number: F29125 Sampling Date: 01/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

28

Sitewide Environmental Monitoring Quarterly Progress Report for the Young-Rainy STAR Center  

Office of Legacy Management (LM)

2-TAC 2-TAC GJO-PIN 11.6.2 Pinellas Environmental Restoration Project January through March 2003 Sitewide Environmental Monitoring Quarterly Progress Report for the Young-Rainey STAR Center April 2003 Grand Junction Office Grand Junction Office Grand Junction Office U.S. Department of Energy Work Performed Under DOE Contract No. for the U.S. Department of Energy DE-AC13-02GJ79491 Approved for public release; distribution is unlimited. N0060700 GJO-2003-432-TAC GJO-PIN 11.6.2 Pinellas Environmental Restoration Project Sitewide Environmental Monitoring Quarterly Progress Report for the Young - Rainey STAR Center January through March 2003 April 2003 Prepared by U.S. Department of Energy Grand Junction Office Grand Junction, Colorado Work Performed Under DOE Contract Number DE-AC13-02GJ79491

29

S M Stoller Pinellas Environmental Restoration Project - Young- Rainey Star Center  

Office of Legacy Management (LM)

Pinellas Environmental Restoration Project - Young- Rainey Star Center Pinellas Environmental Restoration Project - Young- Rainey Star Center 110406202 Accutest Job Number: F33039 Sampling Date: 07/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable.

30

S M Stoller STAR Center- 4.5 Acre Site, Largo, FL  

Office of Legacy Management (LM)

STAR Center- 4.5 Acre Site, Largo, FL STAR Center- 4.5 Acre Site, Largo, FL 110406202 Accutest Job Number: F23552 Sampling Date: 04/20/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

31

Economic Development Activities at the Young - Rainey Science, Technology, & Research (STAR) Center  

SciTech Connect (OSTI)

Project mission was to mitigate the adverse economic effects of closing the U.S. Department of Energy's Pinellas Plant in Largo, Florida. This project was to facilitate the physical renovation of the plant and to help maintain and create jobs for the employees that worked at the plant when DOE terminated its operations. It also included finding and attracting high technology, industrial manufacturing and related firms to utilize the space and high tech equipment to remain at the plant. Stakeholders included the affected plant employees, local government and related public organizations, and businesses and universities in the Tampa Bay Florida area. The $17.6 million funded for this project helped produce 2,780 jobs at the Young - Rainey STAR Center at an average cost of $6,328. Rental income from STAR Center tenants and third party cash input amounted to approximately $66 million over the project period of 13.3 years.

Paul S. Sacco; Carl Smeigh; John Caponiti, Jr.

2008-06-30T23:59:59.000Z

32

Best Practices Guide for Energy-Efficient Data Center Design | ENERGY STAR  

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

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

33

Trane and The American Center: SPP Success Story | ENERGY STAR Buildings &  

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

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

34

SPP marketing flyer for data centers | ENERGY STAR Buildings & Plants  

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

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

35

Stars in other universes: stellar structure with different fundamental constants  

SciTech Connect (OSTI)

Motivated by the possible existence of other universes, with possible variations in the laws of physics, this paper explores the parameter space of fundamental constants that allows for the existence of stars. To make this problem tractable, we develop a semi-analytical stellar structure model that allows for physical understanding of these stars with unconventional parameters, as well as a means to survey the relevant parameter space. In this work, the most important quantities that determine stellar properties-and are allowed to vary-are the gravitational constant G, the fine structure constant {alpha} and a composite parameter C that determines nuclear reaction rates. Working within this model, we delineate the portion of parameter space that allows for the existence of stars. Our main finding is that a sizable fraction of the parameter space (roughly one-fourth) provides the values necessary for stellar objects to operate through sustained nuclear fusion. As a result, the set of parameters necessary to support stars are not particularly rare. In addition, we briefly consider the possibility that unconventional stars (e.g. black holes, dark matter stars) play the role filled by stars in our universe and constrain the allowed parameter space.

Adams, Fred C, E-mail: fca@umich.edu [Michigan Center for Theoretical Physics, Department of Physics, University of Michigan, Ann Arbor, MI 48109 (United States)

2008-08-15T23:59:59.000Z

36

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

E-Print Network [OSTI]

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

E. P. J. van den Heuvel

2007-04-10T23:59:59.000Z

37

Quarterly Progress Report for the Young-Rainey STAR Center's 4.5 Acre Site  

Office of Legacy Management (LM)

600 600 GJO-2003-410-TAC GJO-PIN 25.5.1 Pinellas Environmental Restoration Project Quarterly Progress Report for the Young - Rainey STAR Center's 4.5 Acre Site October through December 2002 January 2003 Prepared by U.S. Department of Energy Grand Junction Office Grand Junction, Colorado Work Performed Under DOE Contract Number DE-AC13-02GJ79491 Task Order Number ST03-107 Document Number N0057600 Contents DOE/Grand Junction Office 4.5 Acre Site Quarterly Progress Report January 2003 Page iii Contents Acronyms and Abbreviations ..........................................................................................................v 1.0 Introduction ............................................................................................................................1

38

Successful Field-Scale In Situ Thermal NAPL Remediation at the Young-Rainey Star Center  

SciTech Connect (OSTI)

The U.S. Department of Energy (DOE) successfully completed a fieldscale remediation to remove non-aqueous phase liquids (NAPLs) from the subsurface at a site on the Young-Rainey Science, Technology, and Research (STAR) Center, Largo, Florida. The STAR Center is a former DOE facility. The remediation project covered an area of 930 m2 (10,000 ft2) and depths extending to 10.5 m (35 ft) below ground surface. In July 2001, DOEs contractor awarded a subcontract to SteamTech Environmental Services for removal of NAPLs from a portion of the Northeast Site. The technologies used for remediation were steam-enhanced extraction and Electro-Thermal Dynamic Stripping Process, an electrical resistive heating technology. McMillan-McGee Corporation implemented the process. Construction of the remediation system was completed in September 2002. Operations began immediately after construction, and active heating ended in February 2003. After operations were completed, confirmatory sampling was conducted over a 6-month period to verify the level of cleanup achieved. Results of the sampling showed that NAPL concentrations were reduced significantly below the required cleanup goals and, in most cases, below the regulatory maximum contaminant levels. Lessons learned relative to the design, construction, operation, confirmatory sampling approach, and subcontracting could benefit managers of similar remediation projects

Gavaskar, A.R. [ed.; Chen, A.S.C. [ed.; none,

2004-05-04T23:59:59.000Z

39

S M Stoller Pinellas Environmental Restoration Project - Young - Rainey Star Center  

Office of Legacy Management (LM)

6/06 6/06 Technical Report for S M Stoller Pinellas Environmental Restoration Project - Young - Rainey Star Center 110406202 Accutest Job Number: F43553 Sampling Date: 09/07/06 Report to: U.S. Dept of Energy, Grand Jct Office 2597 B 3/4 Road Grand Juction, CO 81503 ATTN: Contracts Department, PO# 24231 x Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference

40

Coalescing neutron stars - a step towards physical models III. Improved numerics and different neutron star masses and spins  

E-Print Network [OSTI]

(Abridged) In this paper we present a compilation of results from our most advanced neutron star merger simulations, including a description of the employed numerical procedures and a more complete overview over a large number of computed models. The three-dimensional hydrodynamic simulations were done with a code based on the Piecewise Parabolic Method with up to five levels of nested Cartesian grids. The simulations are basically Newtonian, but gravitational-wave emission and the corresponding back-reaction are taken into account. The use of a physical nuclear equation of state allows us to follow the thermodynamic history of the stellar medium and to compute the energy and lepton number loss due to the emission of neutrinos. The computed models differ concerning the neutron star masses and mass ratios, the neutron star spins, the numerical resolution expressed by the cell size of the finest grid and the number of grid levels, and the calculation of the temperature from the solution of the entropy equation instead of the energy equation. Our simulations show that the details of the gravitational-wave emission are still sensitive to the numerical resolution, even in our highest-quality calculations. The amount of mass which can be ejected from neutron star mergers depends strongly on the angular momentum of the system. Our results do not support the initial conditions of temperature and proton-to-nucleon ratio assumed in recent work for producing a solar r-process pattern for nuclei around and above the A approx 130 peak. The improved models confirm our previous conclusion that gamma-ray bursts are not powered by neutrino emission during the dynamical phase of the merging of two neutron stars.

M. Ruffert; H. -Th. Janka

2001-06-13T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" from the National Library of EnergyBeta (NLEBeta).
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41

KECK OBSERVATIONS OF THE GALACTIC CENTER SOURCE G2: GAS CLOUD OR STAR?  

SciTech Connect (OSTI)

We present new observations and analysis of G2-the intriguing red emission-line object which is quickly approaching the Galaxy's central black hole. The observations were obtained with the laser guide star adaptive optics systems on the W. M. Keck I and II telescopes (2006-2012) and include spectroscopy (R {approx} 3600) centered on the hydrogen Br{gamma} line as well as K' (2.1 {mu}m) and L' (3.8 {mu}m) imaging. Analysis of these observations shows the Br{gamma} line emission has a positional offset from the L' continuum. This offset is likely due to background source confusion at L'. We therefore present the first orbital solution derived from Br{gamma} line astrometry, which, when coupled with radial velocity measurements, results in a later time of closest approach (2014.21 {+-} 0.14), closer periastron (130 AU, 1600 R{sub s}), and higher eccentricity (0.9814 {+-} 0.0060) compared to a solution using L' astrometry. It is shown that G2 has no K' counterpart down to K' {approx} 20 mag. G2's L' continuum and the Br{gamma} line emission appears unresolved in almost all epochs, which implies that the bulk of the emission resides in a compact region. The observations altogether suggest that while G2 has a gaseous component that is tidally interacting with the central black hole, there is likely a central star providing the self-gravity necessary to sustain the compact nature of this object.

Phifer, K.; Meyer, L.; Ghez, A. M.; Witzel, G.; Yelda, S.; Boehle, A.; Morris, M. R.; Becklin, E. E. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Do, T. [Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H4 (Canada); Lu, J. R. [Institute for Astronomy, University of Hawaii, Hilo, HI 96720 (United States); Matthews, K., E-mail: ghez@astro.ucla.edu [Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA 91125 (United States)

2013-08-10T23:59:59.000Z

42

RADIO DETECTION OF A CANDIDATE NEUTRON STAR ASSOCIATED WITH GALACTIC CENTER SUPERNOVA REMNANT SAGITTARIUS A EAST  

SciTech Connect (OSTI)

We report the Very Large Array (VLA) detection of the radio counterpart of the X-ray object referred to as the 'Cannonball', which has been proposed to be the remnant neutron star resulting from the creation of the Galactic center supernova remnant, Sagittarius A East. The radio object was detected both in our new VLA image from observations in 2012 at 5.5 GHz and in archival VLA images from observations in 1987 at 4.75 GHz and in the period from 1990 to 2002 at 8.31 GHz. The radio morphology of this object is characterized as a compact, partially resolved point source located at the northern tip of a radio 'tongue' similar to the X-ray structure observed by Chandra. Behind the Cannonball, a radio counterpart to the X-ray plume is observed. This object consists of a broad radio plume with a size of 30''15'', followed by a linear tail having a length of 30''. The compact head and broad plume sources appear to have relatively flat spectra (??{sup ?}) with mean values of ? = 0.44 0.08 and 0.10 0.02, respectively, and the linear tail shows a steep spectrum with the mean value of 1.94 0.05. The total radio luminosity integrated from these components is ?8 10{sup 33} erg s{sup 1}, while the emission from the head and tongue amounts for only ?1.5 10{sup 31} erg s{sup 1}. Based on the images obtained from the two epochs' observations at 5 GHz, we infer the proper motion of the object: ?{sub ?} = 0.001 0.003 arcsec yr{sup 1} and ?{sub ?} = 0.013 0.003 arcsec yr{sup 1}. With an implied velocity of 500 km s{sup 1}, a plausible model can be constructed in which a runaway neutron star surrounded by a pulsar wind nebula was created in the event that produced Sgr A East. The inferred age of this object, assuming that its origin coincides with the center of Sgr A East, is approximately 9000 yr.

Zhao, Jun-Hui [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 78, Cambridge, MA 02138 (United States); Morris, Mark R. [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States); Goss, W. M., E-mail: jzhao@cfa.harvard.edu, E-mail: morris@astro.ucla.edu, E-mail: mgoss@aoc.nrao.edu [NRAO, P.O. Box O, Socorro, NM 87801 (United States)

2013-11-10T23:59:59.000Z

43

VVV SURVEY NEAR-INFRARED PHOTOMETRY OF KNOWN BULGE RR LYRAE STARS: THE DISTANCE TO THE GALACTIC CENTER AND ABSENCE OF A BARRED DISTRIBUTION OF THE METAL-POOR POPULATION  

SciTech Connect (OSTI)

We have combined optical and near-infrared data of known RR Lyrae (RRL) stars in the bulge in order to study the spatial distribution of its metal-poor component by measuring precise reddening values and distances of 7663 fundamental-mode RRL stars with high-quality photometry. We obtain a distance to the Galactic center of R {sub 0} = 8.33 0.05 0.14 kpc. We find that the spatial distribution of the RRL stars differs from the structures traced by the predominantly metal-rich red clump (RC) stars. Unlike the RC stars, the RRL stars do not trace a strong bar, but have a more spheroidal, centrally concentrated distribution, showing only a slight elongation in its very center. We find a hint of bimodality in the density distribution at high southern latitudes (b < 5), which needs to be confirmed by extending the areal coverage of the current census. The different spatial distributions of the metal-rich and metal-poor stellar populations suggest that the Milky Way has a composite bulge.

Dkny, I.; Minniti, D.; Catelan, M.; Zoccali, M.; Hempel, M. [Instituto de Astrofsica, Facultad de Fsica, Pontificia Universidad Catlica de Chile, Av. Vicua Mackenna 4860, 782-0436 Macul, Santiago (Chile)] [Instituto de Astrofsica, Facultad de Fsica, Pontificia Universidad Catlica de Chile, Av. Vicua Mackenna 4860, 782-0436 Macul, Santiago (Chile); Saito, R. K. [Departamento de Fsica, Universidade Federal de Sergipe, Av. Marechal Rondon s/n, 49100-000, So Cristvo, SE (Brazil)] [Departamento de Fsica, Universidade Federal de Sergipe, Av. Marechal Rondon s/n, 49100-000, So Cristvo, SE (Brazil); Gonzalez, O. A., E-mail: idekany@astro.puc.cl [European Southern Observatory, Alonso de Crdova 3170, Vitacura, Santiago (Chile)

2013-10-20T23:59:59.000Z

44

Individual differences in gameplay and learning: a narrative-centered learning perspective  

Science Journals Connector (OSTI)

Narrative-centered learning environments are an important class of educational games that situate learning within rich story contexts. The work presented in this paper investigates individual differences in gameplay and learning during student interactions ... Keywords: empirical evaluation, engagement, game-based learning, narrative-centered learning environments

Jonathan P. Rowe; Lucy R. Shores; Bradford W. Mott; James C. Lester

2010-06-01T23:59:59.000Z

45

A seismic approach to testing different formation channels of subdwarf B stars  

E-Print Network [OSTI]

There are many unknowns in the formation of subdwarf B stars. Different formation channels are considered to be possible and to lead to a variety of helium-burning subdwarfs. All seismic models to date, however, assume that a subdwarf B star is a post-helium-flash-core surrounded by a thin inert layer of hydrogen. We examine an alternative formation channel, in which the subdwarf B star originates from a massive (>~2 Msun) red giant with a non-degenerate helium-core. Although these subdwarfs may evolve through the same region of the log g-Teff diagram as the canonical post-flash subdwarfs, their interior structure is rather different. We examine how this difference affects their pulsation modes and whether it can be observed. Using detailed stellar evolution calculations we construct subdwarf B models from both formation channels. The iron accumulation in the driving region due to diffusion, which causes the excitation of the modes, is approximated by a Gaussian function. The pulsation modes and frequencies are calculated with a non-adiabatic pulsation code. A detailed comparison of two subdwarf B models from different channels, but with the same log g and Teff, shows that their mode excitation is different. The excited frequencies are lower for the post-flash than for the post-non-degenerate subdwarf B star. This is mainly due to the differing chemical composition of the stellar envelope. A more general comparison between two grids of models shows that the excited frequencies of most post-non-degenerate subdwarfs cannot be well-matched with the frequencies of post-flash subdwarfs. In the rare event that an acceptable seismic match is found, additional information, such as mode identification and log g and Teff determinations, allows us to distinguish between the two formation channels.

Haili Hu; M. -A. Dupret; C. Aerts; G. Nelemans; S. D. Kawaler; A. Miglio; J. Montalban; R. Scuflaire

2008-08-22T23:59:59.000Z

46

UV and FIR selected star-forming galaxies at z=0: differences and overlaps  

E-Print Network [OSTI]

We study two samples of local galaxies, one is UV (GALEX) selected and the other FIR (IRAS) selected, to address the question whether UV and FIR surveys see the two sides ('bright' and 'dark') of the star formation of the same population of galaxies or two different populations of star forming galaxies. No significant difference between the L$_{tot}$ ($=L_{60}+L_{FUV}$) luminosity functions of the UV and FIR samples is found. Also, after the correction for the `Malmquist bias' (bias for flux limited samples), the FIR-to-UV ratio v.s. L$_{tot}$ relations of the two samples are consistent with each other. In the range of $9 \\la \\log(L_{tot}/L_\\sun) \\la 12$, both can be approximated by a simple linear relation of $\\log (L_{60}/L_{FUV})=\\log(L_{tot}/L_\\sun)-9.66$. These are consistent with the hypothesis that the two samples represent the same population of star forming galaxies, and their well documented differences in L$_{tot}$ and in FIR-to-UV ratio are due only to the selection effect. A comparison between the UV luminosity functions shows marginal evidence for a population of faint UV galaxies missing in the FIR selected sample. The contribution from these 'FIR-quiet' galaxies to the overall UV population is insignificant, given that the K-band luminosity functions (i.e. the stellar mass functions) of the two samples do not show any significant difference.

C. Kevin Xu; Veronique Buat; Jorge Iglesias-Pramo; Tsutomu T. Takeuchi; Tom A. Barlow; Luciana Bianchi; Jose Donas; Karl Forster; Timothy M. Heckman; Patrick N. Jelinsky; Young-Wook Lee; Barry F. Madore; Roger F. Malina; D. Christopher Martin; Bruno Milliard; Patrick Morrissey; R. Michael Rich; Susan G. Neff; David Schiminovich; Oswald H. W. Siegmund; Todd Small; Alex S. Szalay; Barry Y. Welsh; Ted K. Wyder; Sukyoung Yi

2006-04-04T23:59:59.000Z

47

The difference between source and site energy | ENERGY STAR Buildings &  

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

The difference between source and site energy The difference between source and site energy Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit Identify your property type Enter data into Portfolio Manager The data quality checker

48

From blue star-forming to red passive: galaxies in transition in different environments  

E-Print Network [OSTI]

Exploiting a mass complete (M_*>10^(10.25)M_sun) sample at 0.03environment. The incidence of red galaxies increases with increasing mass, and, for M_*environment, and increases monotonically with galaxy mass. We also inspect galaxy structural parameters, star-formation properties, histories and ages and propose an evolutionary scenario for the different subpopulations. Color transformations are due to a reduction and suppression of SFR in bot...

Vulcani, Benedetta; Fritz, Jacopo; Fasano, Giovanni; Moretti, Alessia; Calvi, Rosa; Paccagnella, Angela

2014-01-01T23:59:59.000Z

49

DOE-SR Makes a Difference Through Donation to Educational Center |  

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

DOE-SR Makes a Difference Through Donation to Educational Center DOE-SR Makes a Difference Through Donation to Educational Center DOE-SR Makes a Difference Through Donation to Educational Center February 24, 2011 - 12:00pm Addthis Media Contact Amy Caver, DOE (803) 952-7697 amy.caver@srs.gov Aiken, SC -- The Department of Energy-Savannah River Operations Office (DOE-SR) is making a real impact to increase learning resources for an educational nonprofit organization through its Computers for Learning (CFL) program. Just recently, DOE-SR donated 20 computer systems to the Darden Enlightenment Center located in Farmville, North Carolina. "We at DOE-SR are extremely pleased to be able to make a positive impact in communities where the needs of at-risk youth or senior citizens is great," said DOE-SR Manager Dave Moody. "The donation of these

50

DOE-SR Makes a Difference Through Donation to Educational Center |  

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

DOE-SR Makes a Difference Through Donation to Educational Center DOE-SR Makes a Difference Through Donation to Educational Center DOE-SR Makes a Difference Through Donation to Educational Center February 24, 2011 - 12:00pm Addthis Media Contact Amy Caver, DOE (803) 952-7697 amy.caver@srs.gov Aiken, SC -- The Department of Energy-Savannah River Operations Office (DOE-SR) is making a real impact to increase learning resources for an educational nonprofit organization through its Computers for Learning (CFL) program. Just recently, DOE-SR donated 20 computer systems to the Darden Enlightenment Center located in Farmville, North Carolina. "We at DOE-SR are extremely pleased to be able to make a positive impact in communities where the needs of at-risk youth or senior citizens is great," said DOE-SR Manager Dave Moody. "The donation of these

51

Sitewide Environmental Monitoring Quarterly Progress Report for the Young-Rainey STAR Center, October through December 2002  

Office of Legacy Management (LM)

7500 7500 GJO-2003-409-TAC GJO-PIN 11.6.2 Pinellas Environmental Restoration Project Sitewide Environmental Monitoring Quarterly Progress Report for the Young - Rainey STAR Center October through December 2002 January 2003 Prepared by U.S. Department of Energy Grand Junction Office Grand Junction, Colorado Work Performed Under DOE Contract Number DE-AC13-02GJ79491 Task Order Number ST03-107 Document Number N0057500 Contents DOE/Grand Junction Office Pinellas Environmental Restoration Project January 2003 Page iii Contents Page Acronyms and Abbreviations ..........................................................................................................v 1.0 Introduction ............................................................................................................................1

52

EARLY-STAGE MASSIVE STAR FORMATION NEAR THE GALACTIC CENTER: Sgr C  

SciTech Connect (OSTI)

We present near-infrared spectroscopy and 1 mm line and continuum observations of a recently identified site of high mass star formation likely to be located in the Central Molecular Zone (CMZ) near Sgr C. Located on the outskirts of the massive evolved H II region associated with Sgr C, the area is characterized by an Extended Green Object (EGO) measuring ?10'' in size (0.4 pc), whose observational characteristics suggest the presence of an embedded massive protostar driving an outflow. Our data confirm that early-stage star formation is taking place on the periphery of the Sgr C H II region, with detections of two protostellar cores and several knots of H{sub 2} and Brackett ? emission alongside a previously detected compact radio source. We calculate the cores' joint mass to be ?10{sup 3} M {sub ?}, with column densities of 1-2 10{sup 24} cm{sup 2}. We show the host molecular cloud to hold ?10{sup 5} M {sub ?} of gas and dust with temperatures and column densities favorable for massive star formation to occur, however, there is no evidence of star formation outside of the EGO, indicating that the cloud is predominantly quiescent. Given its mass, density, and temperature, the cloud is comparable to other remarkable non-star-forming clouds such as G0.253 in the eastern CMZ.

Kendrew, S.; Johnston, K.; Beuther, H. [Max-Planck-Institut fr Astronomie, Knigstuhl 17, D-69117 Heidelberg (Germany)] [Max-Planck-Institut fr Astronomie, Knigstuhl 17, D-69117 Heidelberg (Germany); Ginsburg, A.; Bally, J.; Battersby, C. [CASA, University of Colorado at Boulder, UCB 389, Boulder, CO 80309 (United States)] [CASA, University of Colorado at Boulder, UCB 389, Boulder, CO 80309 (United States); Cyganowski, C. J., E-mail: kendrew@mpia.de [Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)

2013-10-01T23:59:59.000Z

53

THE GALACTIC CENTER CLOUD G0.253+0.016: A MASSIVE DENSE CLOUD WITH LOW STAR FORMATION POTENTIAL  

SciTech Connect (OSTI)

We present the first interferometric molecular line and dust emission maps for the Galactic Center (GC) cloud G0.253+0.016, observed using CARMA and the SMA. This cloud is very dense, and concentrates a mass exceeding the Orion Molecular Cloud Complex (2 Multiplication-Sign 10{sup 5} M{sub Sun }) into a radius of only 3 pc, but it is essentially starless. G0.253+0.016 therefore violates ''star formation laws'' presently used to explain trends in galactic and extragalactic star formation by a factor {approx}45. Our observations show a lack of dense cores of significant mass and density, thus explaining the low star formation activity. Instead, cores with low densities and line widths {approx}< 1 km s{sup -1}-probably the narrowest lines reported for the GC region to date-are found. Evolution over several 10{sup 5} yr is needed before more massive cores, and possibly an Arches-like stellar cluster, could form. Given the disruptive dynamics of the GC region, and the potentially unbound nature of G0.253+0.016, it is not clear that this evolution will happen.

Kauffmann, Jens; Pillai, Thushara [Astronomy Department, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125 (United States); Zhang Qizhou, E-mail: jens.kauffmann@astro.caltech.edu [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS78, Cambridge, MA 02138 (United States)

2013-03-10T23:59:59.000Z

54

Mass-loss rates and dust-to-gas ratios for obscured Asymptotic Giant Branch stars of different metallicities  

E-Print Network [OSTI]

The mass-loss rates and dust-to-gas ratios of obscured Asymptotic Giant Branch (AGB) stars are investigated for samples with different initial metallicities: in the Small and Large Magellanic Clouds (SMC & LMC) and in the Milky Way. The properties of their circumstellar envelopes can be explained in a consistent way if, both for obscured M-type AGB stars and for obscured carbon stars, the total (gas+dust) mass-loss rate depends only weakly on initial metallicity whilst the dust-to-gas ratio depends approximately linearly on initial metallicity.

Jacco Th. van Loon

1999-12-02T23:59:59.000Z

55

Abundance Differences Between Exoplanet Binary Host Stars XO-2N and XO-2S -- Dependence on Stellar Parameters  

E-Print Network [OSTI]

The chemical composition of exoplanet host stars is an important factor in understanding the formation and characteristics of their orbiting planets. The best example of this to date is the planet-metallicity correlation. Other proposed correlations are thus far less robust, in part due to uncertainty in the chemical history of stars pre- and post-planet formation. Binary host stars of similar type present an opportunity to isolate the effects of planets on host star abundances. Here we present a differential elemental abundance analysis of the XO-2 stellar binary, in which both G9 stars host giant planets, one of which is transiting. Building on our previous work, we report 16 elemental abundances and compare the $\\Delta$(XO-2N-XO-S) values to elemental condensation temperatures. The $\\Delta$(N-S) values and slopes with condensation temperature resulting from four different pairs of stellar parameters are compared to explore the effects of changing the relative temperature and gravity of the stars. We find t...

Teske, Johanna K; Cunha, Katia; Smith, Verne V; Schuler, Simon C; Bergemann, Maria

2015-01-01T23:59:59.000Z

56

Mass ejection from neutron star mergers: different components and expected radio signals  

E-Print Network [OSTI]

In addition to producing a strong gravitational signal, a short gamma-ray burst (GRB), and a compact remnant, neutron star mergers eject significant masses at significant kinetic energies. This mass ejection takes place via dynamical mass ejection and a GRB jet but other processes have also been suggested: a shock-breakout material, a cocoon resulting from the interaction of the jet with other ejecta, and viscous and neutrino driven winds from the central remnant or the accretion disk. The different components of the ejected masses include up to a few percent of a solar mass, some of which is ejected at relativistic velocities. The interaction of these ejecta with the surrounding interstellar medium will produce a long lasting radio flare, in a similar way to GRB afterglows or to radio supernovae. The relative strength of the different signals depends strongly on the viewing angle. An observer along the jet axis or close to it will detect a strong signal at a few dozen days from the radio afterglow (or the or...

Hotokezaka, Kenta

2015-01-01T23:59:59.000Z

57

Do Healthcare Process and Outcomes Differ for Acute Ischemic Stroke Patients Admitted to Designated Stroke Centers?.  

E-Print Network [OSTI]

??Stroke is the third leading cause of mortality and the leading cause of serious long-term disability in the Unites States. Establishment of designated stroke centers (more)

Xian, Ying

2011-01-01T23:59:59.000Z

58

Oxygen abundances in planet-harbouring stars. Comparison of different abundance indicators  

E-Print Network [OSTI]

We present a detailed and uniform study of oxygen abundances in 155 solar type stars, 96 of which are planet hosts and 59 of which form part of a volume-limited comparison sample with no known planets. EW measurements were carried out for the [O I] 6300 \\AA line and the O I triplet, and spectral synthesis was performed for several OH lines. NLTE corrections were calculated and applied to the LTE abundance results derived from the O I 7771-5 \\AA\\ triplet. Abundances from [O I], the O I triplet and near-UV OH were obtained in 103, 87 and 77 dwarfs, respectively. We present the first detailed and uniform comparison of these three oxygen indicators in a large sample of solar-type stars. There is good agreement between the [O/H] ratios from forbidden and OH lines, while the NLTE triplet shows a systematically lower abundance. We found that discrepancies between OH, [O I] and the O I triplet do not exceed 0.2 dex in most cases. We have studied abundance trends in planet host and comparison sample stars, and no obvious anomalies related to the presence of planets have been detected. All three indicators show that, on average, [O/Fe] decreases with [Fe/H] in the metallicity range -0.8oxygen overabundance of 0.1-0.2dex with respect to the comparison sample.

A. Ecuvillon; G. Israelian; N. C. Santos; N. G. Shchukina; M. Mayor; R. Rebolo

2005-09-13T23:59:59.000Z

59

Carbon monoxide line emission as a CMB foreground: tomography of the star-forming universe with different spectral resolutions  

E-Print Network [OSTI]

The rotational lines of carbon monoxide and the fine structure lines of CII and of the most abundant metals, emitted during the epoch of enhanced star formation in the universe, are redshifted in the frequency channels where the present-day and future CMB experiments are sensitive. We estimate the contribution to the CMB angular power spectrum by the emission in such lines in merging star-forming galaxies. We used the Lacey-Cole approach to characterize the distribution of the merging halos, together with a parametrization for the star formation rate in each of them. Using observational data from a sample of local, low-redshift, and high-redshift objects, we calibrated the luminosity in each line as a function of the star formation rate. We show that the correlation term arising from CO line emission is a significant source of foreground for CMB in a broad range of frequencies (in particular in the 20-60 GHz band) and for 1000different spectral resolutions will give the possibility of increasing the amplitude of the signal up to two orders of magnitude in C_l and will help separate the line contribution from practically all other foreground sources and from the primary fluctuations themselves, since these show no significant dependence on the spectral resolution. We propose to perform observations with varying spectral bandwidths as a new tool to construct a tomography of the universe, by probing different redshift slices with varying thickness. (abridged)

Mattia Righi; Carlos Hernandez-Monteagudo; Rashid Sunyaev

2008-07-24T23:59:59.000Z

60

Two-Dimensional Hydrodynamic Core-Collapse Supernova Simulations with Spectral Neutrino Transport II. Models for Different Progenitor Stars  

E-Print Network [OSTI]

1D and 2D supernova simulations for stars between 11 and 25 solar masses are presented, making use of the Prometheus/Vertex neutrino-hydrodynamics code, which employs a full spectral treatment of the neutrino transport. Multi-dimensional transport aspects are treated by the ``ray-by-ray plus'' approximation described in Paper I. Our set of models includes a 2D calculation for a 15 solar mass star whose iron core is assumed to rotate rigidly with an angular frequency of 0.5 rad/s before collapse. No important differences were found depending on whether random seed perturbations for triggering convection are included already during core collapse, or whether they are imposed on a 1D collapse model shortly after bounce. Convection below the neutrinosphere sets in about 40 ms p.b. at a density above 10**12 g/cm^3 in all 2D models, and encompasses a layer of growing mass as time goes on. It leads to a more extended proto-neutron star structure with accelerated lepton number and energy loss and significantly higher muon and tau neutrino luminosities, but reduced mean energies of the radiated neutrinos, at times later than ~100 ms p.b. In case of an 11.2 solar mass star we find that low (l = 1,2) convective modes cause a probably rather weak explosion by the convectively supported neutrino-heating mechanism after ~150 ms p.b. when the 2D simulation is performed with a full 180 degree grid, whereas the same simulation with 90 degree wedge fails to explode like all other models. This sensitivity demonstrates the proximity of our 2D models to the borderline between success and failure, and stresses the need of simulations in 3D, ultimately without the axis singularity of a polar grid. (abridged)

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

2005-12-07T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

A STAR DISRUPTED BY A STELLAR BLACK HOLE AS THE ORIGIN OF THE CLOUD FALLING TOWARD THE GALACTIC CENTER  

SciTech Connect (OSTI)

We propose that the cloud moving on a highly eccentric orbit near the central black hole in our Galaxy, reported by Gillessen et al., is formed by a photoevaporation wind originating in a disk around a star that is tidally perturbed and shocked at every peribothron passage. The disk is proposed to have formed when a stellar black hole flew by the star, tidally disrupted its envelope, and placed the star on its present orbit with some of the tidal debris forming a disk. A disrupting encounter at the location of the observed cloud is most likely to be caused by a stellar black hole because of the expected dynamical mass segregation; the rate of these disk-forming encounters may be as high as {approx}10{sup -6} per year. The star should also be spun up by the encounter, so the disk may subsequently expand by absorbing angular momentum from the star. Once the disk expands up to the tidal truncation radius, the tidal perturbation of the outer disk edge at every peribothron may place gas streams on larger orbits, which can give rise to a photoevaporation wind that forms the cloud at every orbit. This model predicts that, after the cloud is disrupted at the next peribothron passage in 2013, a smaller unresolved cloud will gradually grow around the star on the same present orbit. An increased infrared luminosity from the disk may also be detectable when the peribothron is reached. We also note that this model revives the encounter theory for planet formation.

Miralda-Escude, Jordi [Institucio Catalana de Recerca i Estudis Avancats, Barcelona, Catalonia (Spain)

2012-09-01T23:59:59.000Z

62

Absolute Measurements of the Magnetic Field Generated by Different Coils in the Center of EGYPTOR Tokamak  

Science Journals Connector (OSTI)

The present work is devoted to measure the absolute magnetic field produced by different coils in the EGYPTOR tokamak using a calibrated pickup coil. Scaling these...

H. Hegazy; F. Zacek

2006-06-01T23:59:59.000Z

63

WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z {approx} 2 FROM CANDELS  

SciTech Connect (OSTI)

We use HST/WFC3 imaging from the CANDELS Multi-Cycle Treasury Survey, in conjunction with the Sloan Digital Sky Survey, to explore the evolution of galactic structure for galaxies with stellar masses >3 Multiplication-Sign 10{sup 10} M{sub Sun} from z = 2.2 to the present epoch, a time span of 10 Gyr. We explore the relationship between rest-frame optical color, stellar mass, star formation activity, and galaxy structure. We confirm the dramatic increase from z = 2.2 to the present day in the number density of non-star-forming galaxies above 3 Multiplication-Sign 10{sup 10} M{sub Sun} reported by others. We further find that the vast majority of these quiescent systems have concentrated light profiles, as parameterized by the Sersic index, and the population of concentrated galaxies grows similarly rapidly. We examine the joint distribution of star formation activity, Sersic index, stellar mass, inferred velocity dispersion, and stellar surface density. Quiescence correlates poorly with stellar mass at all z < 2.2. Quiescence correlates well with Sersic index at all redshifts. Quiescence correlates well with 'velocity dispersion' and stellar surface density at z > 1.3, and somewhat less well at lower redshifts. Yet, there is significant scatter between quiescence and galaxy structure: while the vast majority of quiescent galaxies have prominent bulges, many of them have significant disks, and a number of bulge-dominated galaxies have significant star formation. Noting the rarity of quiescent galaxies without prominent bulges, we argue that a prominent bulge (and perhaps, by association, a supermassive black hole) is an important condition for quenching star formation on galactic scales over the last 10 Gyr, in qualitative agreement with the active galactic nucleus feedback paradigm.

Bell, Eric F.; Herrington, Jessica [Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States); Van der Wel, Arjen [Max-Planck Institut fuer Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Papovich, Casey [George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A and M University, College Station, TX 77843-4242 (United States); Kocevski, Dale; Faber, S. M.; Cheung, Edmond; Koo, David C.; McGrath, Elizabeth J. [UCO/Lick Observatory, Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States); Lotz, Jennifer; Ferguson, Harry; Koekemoer, Anton; Grogin, Norman [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); McIntosh, Daniel H. [Department of Physics, University of Missouri-Kansas City, Kansas City, MO 64110 (United States); Kartaltepe, Jeyhan [NOAO-Tucson, 950 North Cherry Avenue, Tucson, AZ 85719 (United States); Wuyts, Stijn [Max-Planck-Institut fuer Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching (Germany); Conselice, Christopher J. [University of Nottingham, School of Physics and Astronomy, Nottingham NG7 2RD (United Kingdom); Dekel, Avishai [Racah Institute of Physics, The Hebrew University, Jerusalem 91904 (Israel); Dunlop, James S. [Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ (United Kingdom); Giavalisco, Mauro, E-mail: ericbell@umich.edu [Department of Astronomy, University of Massachusetts, Amherst, MA 01003 (United States); and others

2012-07-10T23:59:59.000Z

64

Leading organizations choose ENERGY STAR | ENERGY STAR Buildings & Plants  

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

Leading organizations choose ENERGY STAR Leading organizations choose ENERGY STAR Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Why design to earn ENERGY STAR Leading organizations choose ENERGY STAR Sell others on the idea of ENERGY STAR An overview of the ENERGY STAR lifecycle Design to earn ENERGY STAR Leading organizations choose ENERGY STAR Facebook's data center achieved Designed to Earn the ENERGY STAR More than

65

STAR Test Environment  

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

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

66

The role of magnetic fields in hyperon stars  

SciTech Connect (OSTI)

We investigate the effects of strong magnetic fields (SMF) on the properties of neutron stars that have hyperons in their composition. The matter is described by a hadronic model in which a parameterized and derivative coupling between hadrons and mesons is considered. We study the magnetic effects on the equation of state (EoS) from Landau quantization, assuming a density dependent static magnetic field that reaches 10{sup 19} G in the center of the star. The Tolman- Oppenheimer-Volkoff (TOV) equations are solved in order to show the dependence of the massradius relation and population of hyperon stars on the central magnetic field and on different hyperon coupling schemes.

Gomes, R. O.; Vasconcellos, C. A. Z. [Instituto de Fsica - Universidade Federal do Rio Grande do Sul, Porto Alegre, RS 91501-970 (Brazil); Dexheimer, V. [Department of Physics - Kent State University, Kent, OH 44242 (United States)

2014-05-09T23:59:59.000Z

67

Covered Product Category: Data Center Storage  

Broader source: Energy.gov [DOE]

The Federal Energy Management Program (FEMP) provides acquisition guidance for data center storage, which is a product category covered by the ENERGY STAR program. Federal laws and requirements...

68

Leading firms choose ENERGY STAR | ENERGY STAR Buildings & Plants  

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

Leading firms choose ENERGY STAR Leading firms choose ENERGY STAR Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Why you should design to earn the ENERGY STAR Leading firms choose ENERGY STAR Why new doesn't always mean efficient Follow EPA's step-by-step process ENERGY STAR Challenge for Architects Leading firms choose ENERGY STAR Facebook data center Hundreds of leading A/E firms have already partnered

69

ADVANCED BURNING STAGES AND FATE OF 8-10 M{sub Sun} STARS  

SciTech Connect (OSTI)

The stellar mass range 8 {approx}< M/M{sub Sun} {approx}< 12 corresponds to the most massive asymptotic giant branch (AGB) stars and the most numerous massive stars. It is host to a variety of supernova (SN) progenitors and is therefore very important for galactic chemical evolution and stellar population studies. In this paper, we study the transition from super-AGB (SAGB) star to massive star and find that a propagating neon-oxygen-burning shell is common to both the most massive electron capture supernova (EC-SN) progenitors and the lowest mass iron-core-collapse supernova (FeCCSN) progenitors. Of the models that ignite neon-burning off-center, the 9.5 M{sub Sun} star would evolve to an FeCCSN after the neon-burning shell propagates to the center, as in previous studies. The neon-burning shell in the 8.8 M{sub Sun} model, however, fails to reach the center as the URCA process and an extended (0.6 M{sub Sun }) region of low Y{sub e} (0.48) in the outer part of the core begin to dominate the late evolution; the model evolves to an EC-SN. This is the first study to follow the most massive EC-SN progenitors to collapse, representing an evolutionary path to EC-SN in addition to that from SAGB stars undergoing thermal pulses (TPs). We also present models of an 8.75 M{sub Sun} SAGB star through its entire TP phase until electron captures on {sup 20}Ne begin at its center and of a 12 M{sub Sun} star up to the iron core collapse. We discuss key uncertainties and how the different pathways to collapse affect the pre-SN structure. Finally, we compare our results to the observed neutron star mass distribution.

Jones, S.; Hirschi, R. [Astrophysics Group, Lennard Jones Building, Keele University, Staffordshire ST5 5BG (United Kingdom); Nomoto, K. [Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa, Chiba 277-8583 (Japan); Fischer, T.; Martinez-Pinedo, G. [GSI Helmholtzzentrum fuer Schwerionenforschung GmbH, Planckstrasse 1, D-64291 Darmstadt (Germany); Timmes, F. X. [School of Earth and Space Exploration, University of Arizona, Tempe, AZ 85287 (United States); Herwig, F. [Joint Institute for Nuclear Astrophysics, University of Notre Dame, IN 46556 (United States); Paxton, B. [KITP and Department of Physics, University of California, Santa Barbara, CA 93106 (United States); Toki, H. [Research Center for Nuclear Physics (RCNP), Osaka University, Osaka 567-0047 (Japan); Suzuki, T. [Department of Physics, College of Humanities and Sciences, Nihon University Sakurajosui 3-25-40, Setagaya-ku, Tokyo 156-8550 (Japan); Lam, Y. H. [Institut fuer Kernphysik, Technische Universitaet Darmstadt, Schlossgartenstrasse 2, D-64289 Darmstadt (Germany); Bertolli, M. G., E-mail: s.w.jones@keele.ac.uk [Theoretical Division, Los Alamos National Laboratory, Los Alamos, NM 87545 (United States)

2013-08-01T23:59:59.000Z

70

Dark Stars: A Review  

E-Print Network [OSTI]

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

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

2015-01-10T23:59:59.000Z

71

Nuclear Reactions in Stars  

Science Journals Connector (OSTI)

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

1961-01-01T23:59:59.000Z

72

STAR METRICS  

Broader source: Energy.gov [DOE]

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

73

X-ray Emission from Massive Stars  

E-Print Network [OSTI]

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

Cohen, David

74

Star Formation in the Local Universe  

E-Print Network [OSTI]

We present preliminary results of a long-term study aimed at answering a number of open questions on the evolution of starbursts in local galaxies. The project employes mainly HST data from the ultraviolet to the red of the stellar continuum and of the nebular emission from the galaxies. Here we concentrate on NGC5253 and NGC5236 (M83), that form a dwarf--massive galaxy pair at about 4 Mpc distance. The recent star formation history of the centers of the two galaxies is investigated in order to identify similarities and differences in the evolution of their central starbursts.

Daniela Calzetti; Jason Harris

2001-11-28T23:59:59.000Z

75

Discovery of new Milky Way star cluster candidates in the 2MASS point source catalog III. Follow-up observations of cluster candidates in the Galactic Center region  

E-Print Network [OSTI]

This paper is part of a project to search the inner Milky Way for hidden massive clusters and to address the question of whether our Galaxy still forms clusters similar to the progenitors of the present-day globular clusters. We report high angular resolution deep near-infrared imaging of 21 cluster candidates selected from the catalogues of Bica et al. (2003) and Dutra et al.(2003) in a region around the Galactic Center. These catalogues were created from visual inspection of the 2MASS images. Seven objects appear to be genuine clusters, and for these objects we present estimates of extinction, distance and in some cases age and mass. Our estimated masses range from 1200 to 5500 solar masses. These clusters are thus significantly smaller than any Galactic globular cluster, and indicate that the formation of massive young clusters such as Arches and Quintuplet is not common in the present-day Milky Way. The remaining 14 objects are either not clusters or cannot be classified based on our data.

J. Borissova; V. D. Ivanov; D. Minniti; D. Geisler; A. W. Stephens

2005-02-01T23:59:59.000Z

76

Dark Stars: A Review  

E-Print Network [OSTI]

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

Freese, Katherine; Spolyar, Douglas; Valluri, Monica

2015-01-01T23:59:59.000Z

77

ENERGY STAR  

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

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

78

Anisotropic charged dark energy star  

E-Print Network [OSTI]

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

Kanika Das; Nawsad Ali

2014-02-02T23:59:59.000Z

79

Supermassive black holes from supermassive stars  

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

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

80

Physics of Neutron Star Crusts  

E-Print Network [OSTI]

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

N. Chamel; P. Haensel

2008-12-20T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

Hypervelocity binary stars: smoking gun of massive binary black holes  

E-Print Network [OSTI]

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

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

2007-07-12T23:59:59.000Z

82

Establishing Regional Resource Centers  

Wind Powering America (EERE)

Establishing Regional Resource Centers Establishing Regional Resource Centers July 25, 2013 Coordinator: Welcome and thank you for standing by. At this time all participants are in a listen only mode. To ask a question later during the question and answer session please press star then 1 on your touchtone phone. Today's conference is being recorded. If you have any objections you may disconnect. And I would like to turn it over to Mr. Jonathan Bartlett. Sir, you may begin. Jonathan Bartlett: Thank you very much. This is Jonathan Bartlett from the Department of Energy's Wind and Water Power Technologies Office. Today's WPA Webinar will be on the subject of establishing regional resource centers. I will be joined by Ian Baring-Gould at the National Renewable Energy Laboratory and the

83

Neutron star interiors and topology change  

E-Print Network [OSTI]

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

Peter K. F. Kuhfittig

2012-07-27T23:59:59.000Z

84

The nuclear physics of neutron stars  

SciTech Connect (OSTI)

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

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

2014-05-09T23:59:59.000Z

85

Coalescing Neutron Stars -- a Step Towards Physical Models. I. Hydrodynamic Evolution and Gravitational-Wave Emission  

E-Print Network [OSTI]

We investigate the dynamics and evolution of coalescing neutron stars. Although the code (Piecewise Parabolic Method) is purely Newtonian, we do include the emission of gravitational waves and their backreaction on the hydrodynamic flow. The properties of neutron star matter are described by the physical equation of state of Lattimer \\& Swesty (1991). Energy loss by all types of neutrinos and changes of the electron fraction due to the emission of electron neutrinos and antineutrinos are taken into account by an elaborate ``neutrino leakage scheme''. We simulate the coalescence of two identical, cool neutron stars with a baryonic mass of $\\approx\\!1.6\\,M_\\odot$ and a radius of $\\approx\\!15$~km and with an initial center-to-center distance of 42~km. The initial distributions of density and electron concentration are given from a model of a cold neutron star in hydrostatic equilibrium (central temperature about $8\\,{\\rm MeV}$). We investigate three cases which differ by the initial velocity distribution in the neutron stars, representing different cases of the neutron star spins relative to the direction of the orbital angular momentum vector. Within about 1~ms the neutron stars merge into a rapidly spinning ($P_{\\rm spin}\\approx 1$~ms), high-density body ($\\rho\\approx 10^{14}$~g/cm$^3$) with a surrounding thick disk of material with densities $\\rho\\approx 10^{10}-10^{12}$~g/cm$^3$ and orbital velocities of~0.3--0.5~c. In this work we evaluate the models in detail with respect to the gravitational wave emission using the quadrupole approximation. In a forthcoming paper we will concentrate on the neutrino emission and implications for gamma-ray bursters. A maximum luminosity in excess of $10^{55}$~erg/s is reached for about 1~ms.

M. Ruffert; H. -Th. Janka; G. Schaefer

1995-09-01T23:59:59.000Z

86

ENERGY STAR  

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

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

87

The Star Formation History of NGC 6822  

E-Print Network [OSTI]

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

Ted K. Wyder

2001-07-31T23:59:59.000Z

88

Star Power  

SciTech Connect (OSTI)

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

None

2014-10-17T23:59:59.000Z

89

Star Power  

ScienceCinema (OSTI)

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

None

2014-11-18T23:59:59.000Z

90

Geothermal Academy: Focus Center | Department of Energy  

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

Academy: Focus Center Geothermal Academy: Focus Center Project objective: to develop a sufficiently robust data collection and analysis framework to: Accommodate many different...

91

Massive Stars: Their Birth Sites and Distribution  

E-Print Network [OSTI]

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

Pavel Kroupa

2003-09-22T23:59:59.000Z

92

ENERGY STAR  

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

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

93

Massive Star Outflows  

E-Print Network [OSTI]

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

D. S. Shepherd

2005-06-01T23:59:59.000Z

94

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

E-Print Network [OSTI]

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

Swanzy, Michael John

2007-04-25T23:59:59.000Z

95

operations center  

National Nuclear Security Administration (NNSA)

1%2A en Operations Center http:nnsa.energy.govaboutusourprogramsemergencyoperationscounterterrorismoperationscenter

...

96

Nuclear and gravitational energies in stars  

E-Print Network [OSTI]

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

Meynet, Georges; Ekstrm, Sylvia

2013-01-01T23:59:59.000Z

97

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

98

Voluntary Protection Program Onsite Review, Volpentest HAMMER Training Center January 2011  

Broader source: Energy.gov [DOE]

Evaluation to determine whether Volpentest Hazardous Materials Management and Emergency Response Training Center is continuing to perform at a level deserving DOE-VPP Star recognition.

99

Voluntary Protection Program Onsite Review, Transuranic Waste Processing Center- September 2012  

Broader source: Energy.gov [DOE]

Evaluation to determine whether Transuranic Waste Processing Center is continuing to perform at a level deserving DOE-VPP Star recognition.

100

Data Centers: Looking for Energy Solutions  

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

operating costs, benchmark energy performance, and demonstrate environmental stewardship. Turn to an ENERGY STAR ® Service and Product Provider Partner ENERGY STAR Service and Product Providers (SPPs) have the experience and tools to implement energy-efficient strategies that are right for you. Following the U.S. Environmental Protection Agency's (EPA) Guidelines for Energy Management, a proven strategy developed from ENERGY STAR partner successes, SPPs can help your organization gain control of energy consumption and costs. ENERGY STAR SPPs can help data center owners and operators reap the financial and environmental benefits of superior energy efficiency. In its 2007 Report to Congress on Server and Data Center Energy Efficiency Opportunities, EPA estimated that the nation's servers and data

Note: This page contains sample records for the topic "difference star center" 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

Energy Star  

E-Print Network [OSTI]

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

Reihl, K.; Tullos, A.

2012-01-01T23:59:59.000Z

102

Generalized equation of state for cold superfluid neutron stars  

SciTech Connect (OSTI)

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

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

2011-09-21T23:59:59.000Z

103

New subdwarf B star periods  

E-Print Network [OSTI]

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

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

2002-09-26T23:59:59.000Z

104

On Magnetized Neutron Stars  

E-Print Network [OSTI]

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

Lopes, Luiz L

2014-01-01T23:59:59.000Z

105

Help Center  

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

Los Alamos National Laboratory Advanced Simulation and Computing Los Alamos National Laboratory Advanced Simulation and Computing Menu Events Partnerships Help Center Events Partnerships Help Center Videos Advanced Simulation and Computing Program » Help Center Computing Help Center Help hotlines, hours of operation, training, technical assistance, general information Los Alamos National Laboratory Hours: Monday through Friday, 8:00 a.m. - noon, 1:00-5:00 p.m. Mountain time Telephone: (505) 665-4444 option 3 Fax: (505) 665-6333 E-mail: consult@lanl.gov 24 hours a day, 7 days a week Operations (to report a system or network problem: (505) 667-2919 Lawrence Livermore National Laboratory Hours: Monday through Friday, 8:00 a.m. - noon, 1:00-4:45 p.m. Pacific time High Performance Hotline (technical consulting) Telephone: (925) 422-4532

106

ENERGY STAR  

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

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

107

ENERGY STAR  

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

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

108

Directed search for continuous gravitational waves from the Galactic center  

E-Print Network [OSTI]

We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic center region, performed on two years of data from LIGOs fifth science run from two LIGO ...

Aggarwal, Nancy

109

2014 ENERGY STAR Awards : ENERGY STAR  

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

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

110

Reliability-Centered Maintenance | Department of Energy  

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

Reliability-Centered Maintenance Reliability-Centered Maintenance Reliability-Centered Maintenance October 7, 2013 - 9:48am Addthis Reliability-centered maintenance leverages the same practices and technologies of predictive maintenance. The difference is that reliability-centered maintenance recognizes that: Equipment design and operations differ Different equipment has different probabilities of failure All equipment is not of equal importance to facility operations Facilities have limited financial and personnel resources. While reliability-centered maintenance relies on predictive maintenance practices and technologies, it also recognizes that maintenance on inexpensive and/or unimportant equipment may be better served by a reactive or predictive maintenance approach. Each of the aforementioned factors are

111

ASU EFRC - Center researchers  

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

Principal Investigators Postdoctoral Fellows Center researchers Graduate Students Undergraduate Students All Bisfuel Center Personnel Center researchers Chad Simmons Academic...

112

Centers | U.S. DOE Office of Science (SC)  

Office of Science (SC) Website

Centers Centers Energy Frontier Research Centers (EFRCs) EFRCs Home Centers Research Science Highlights News & Events Publications Contact BES Home Centers Print Text Size: A A A RSS Feeds FeedbackShare Page Energy Frontier Research Centers To learn more about each of the 46 EFRC centers, click on the stars in the map or the html links below. Interactive Map of Energy Frontier Research Centers CETM PHaSE CES RPEMSC NECCES CEFRC EMC2 CCEI CLSF Efree NEES CCHF UNC HeteroFoaM CSTEC RMSSEC MSA C3Bio CABS PARC CALCD SSLS CISSEM BISfuel LMI CEN MEEM CEEM CNEEC CGS NCGC CID CMSNF CME CE S3TEC FIRST CDP CEES IACT ANSER NERC CST CFSES CMIME CASP Centers ordered alphabetically by state and then by center name Arizona Center for Bio-Inspired Solar Fuel Production (BISfuel) Devens Gust, Arizona State University

113

Center Resources  

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

Resources for Planning Center Activities Resources for Planning Center Activities       QuarkNet at Work - Resources Home QuarkNet is a teacher professional development effort funded by the National Science Foundation and the US Department of Energy. Teachers work on particle physics experiments during a summer and join a cadre of scientists and teachers working to introduce some aspects of their research into their classrooms. This allows tomorrow's particle physicists to peek over the shoulder of today's experimenters. These resources are available for lead teachers and mentors at Quartnet Centers as they design activities for associate teacher workshops and follow-on activities. Important Findings from Previous Years Mentor Tips Associate Teacher Institute Toolkit

114

Preparing the COROT space mission: new variable stars in the galactic Anticenter direction  

E-Print Network [OSTI]

The activities related to the preparation of the asteroseismic, photometric space mission COROT are described. Photoelectric observations, wide--field CCD photometry, uvbyB calibrations and further time--series have been obtained at different observatories and telescopes. They have been planned to complete the COROT programme in the direction of the galactic Anticenter. In addition to suitable asteroseismic targets covering the different evolutionary stages between ZAMS and TAMS, we discovered several other variable stars, both pulsating and geometrical. We compared results on the incidence of variability in the galactic Center and Anticenter directions. Physical parameters have been obtained and evolutionary tracks fitting them have been calculated. The peculiarities of some individual stars alre pointed out. Paper based on observations collected at the San Pedro Martir, Sierra Nevada, Teide, La Silla, Haute-Provence and Roque de Los Muchachos (Telescopio Nazionale Galileo and Mercator telescopes) observator...

Poretti, E; Amado, P J; Belmonte, J A; Garrido, R; Martin-Ruiz, S; Uytterhoeven, K; Catala, C; Lebreton, Y; Michel, E; Surez, J C; Aerts, C; Creevey, O; Goupil, M J; Mantegazza, L; Mathias, P; Rainer, M; Weiss, W W

2005-01-01T23:59:59.000Z

115

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

E-Print Network [OSTI]

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

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

2013-01-01T23:59:59.000Z

116

JGI - DOE Bioenergy Research Centers  

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

DOE Bioenergy Research Centers DOE Bioenergy Research Centers DOE JGI performs sequencing on behalf of the U.S. Department of Energy Bioenergy Research Centers. The Centers are intended to accelerate basic research in the development of cellulosic ethanol and other biofuels, advancing the federal initiative that seeks to reduce U.S. gasoline consumption by 20% within 10 years through increased efficiency and diversification of clean energy sources. The three Centers are located in geographically distinct areas and use different plants both for laboratory research and for improving feedstock crops. DOE BioEnergy Science Center led by DOE's Oak Ridge National Laboratory in Oak Ridge, Tennessee. This center will focus on the resistance of plant fiber to breakdown into sugars and is studying the potential energy crops

117

Neutron stars and the equation of state  

Science Journals Connector (OSTI)

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

J. Cooperstein

1988-02-01T23:59:59.000Z

118

Neutron stars, {beta}-stable ring-diagram equation of state, and Brown-Rho scaling  

SciTech Connect (OSTI)

Neutron star properties, such as mass, radius, and moment of inertia, are calculated by solving the Tolman-Oppenheimer-Volkov (TOV) equations using the ring-diagram equation of state (EOS) obtained from realistic low-momentum NN interactions V{sub low-k}. Several NN potentials (CDBonn, Nijmegen, Argonne V18, and BonnA) have been employed to calculate the ring-diagram EOS where the particle-particle hole-hole ring diagrams are summed to all orders. The proton fractions for different radial regions of a {beta}-stable neutron star are determined from the chemical potential conditions {mu}{sub n}-{mu}{sub p}={mu}{sub e}={mu}{sub {mu}}. The neutron star masses, radii, and moments of inertia given by the aforementioned potentials all tend to be too small compared with the accepted values. Our results are largely improved with the inclusion of a Skyrme-type three-body force based on Brown-Rho scalings where the in-medium meson masses, particularly those of {omega}, {rho}, and {sigma}, are slightly decreased compared with their in-vacuum values. Representative results using such medium-corrected interactions are maximum neutron-star mass M{approx}1.8M{sub {center_dot}} with radius R{approx}9 km and moment of inertia {approx}60M{sub {center_dot}} km{sup 2}, values given by the four NN potentials being nearly the same. The effects of nuclei-crust EOSs on the properties of neutron stars are discussed.

Dong, Huan; Kuo, T. T. S.; Machleidt, R. [Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794-3800 (United States); Department of Physics, University of Idaho, Moscow, Idaho 83844 (United States)

2009-12-15T23:59:59.000Z

119

Better Buildings Residential Program Solution Center Demonstration Webinar Transcript  

Broader source: Energy.gov [DOE]

The Better Buildings Residential Program Solution Center is a robust online collection of nearly 1,000 examples, strategies, and resources from Better Buildings Neighborhood Program partners, Home Performance with ENERGY STAR Sponsors, and others. This webinar presented on November 19, 2014 gives more information on the Solution Center.

120

Supermassive Stars: Fact or Fiction?  

E-Print Network [OSTI]

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

H. -Th. Janka

2002-02-01T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

ENERGY STAR Challenge  

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

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

122

Upsilon Productions at STAR  

E-Print Network [OSTI]

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

A. M. Hamed

2010-05-22T23:59:59.000Z

123

Multiple glass transitions in star polymer mixtures: Insights from theory and simulations  

E-Print Network [OSTI]

The glass transition in binary mixtures of star polymers is studied by mode coupling theory and extensive molecular dynamics computer simulations. In particular, we have explored vitrification in the parameter space of size asymmetry $\\delta$ and concentration $\\rho_2$ of the small star polymers at fixed concentration of the large ones. Depending on the choice of parameters, three different glassy states are identified: a single glass of big polymers at low $\\delta$ and low $\\rho_2$, a double glass at high $\\delta$ and low $\\rho_2$, and a novel double glass at high $\\rho_2$ and high $\\delta$ which is characterized by a strong localization of the small particles. At low $\\delta$ and high $\\rho_2$ there is a competition between vitrification and phase separation. Centered in the $(\\delta, \\rho_2)$-plane, a liquid lake shows up revealing reentrant glass formation. We compare the behavior of the dynamical density correlators with the predictions of the theory and find remarkable agreement between the two.

Christian Mayer; Francesco Sciortino; Christos N. Likos; Piero Tartaglia; Hartmut Loewen; Emanuela Zaccarelli

2008-11-10T23:59:59.000Z

124

Nuclear and gravitational energies in stars  

SciTech Connect (OSTI)

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

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

2014-05-09T23:59:59.000Z

125

APS Conference Center  

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

Advanced Photon Source Conference Center The APS Conference Center at Argonne National Laboratory is the ideal location for scientific and professional meetings. The Center can...

126

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Fuels Promotion and Information The Center for Alternative Fuels (Center) promotes alternative fuels as viable energy sources in the state. The Center must assess the...

127

Center Research  

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

5 5 Center Research ... Supports Electric Utility Restructuring Winds of change in the U.S. power sector: factors listed in the left column have created a gap between the prices utilities must charge to recover their embedded costs and the lower rates they would have to charge in a competitive environment. Possible responses to these pressures are listed to the right. The electricity industry in the U.S. is being dramatically restructured by state regulatory commissions and the Federal Energy Regulatory Commission. Efforts are underway to create a wholesale market for electricity, with wholesale prices to distributing utility companies no longer being regulated. Discussions in several states and at the FERC are aimed at revising the regulation of the structure, operation, and pricing of the

128

KILLGORE CENTER  

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

LEASE AGREEMENT NO. DE-AC04-89-AL42 1 10 LEASE AGREEMENT NO. DE-AC04-89-AL42 1 10 KILLGORE CENTER AMENDMENT NO. 6 Lease Agreement No. DE-AC04-89-AL-42110, between the U.S. Department of Energy and Texas Tech University, dated October 1, 1989, as amended (amendments one, two, three, four, and five), is hereby further amended as follows: Article I1 of the base lease entitled, "TERM AND RENT," paragraph A., is hereby deleted and revised to read: A. The term of this Lease is extended for five years beginning October 1, 2009, and ending September 30, 2014. The annual rental for this term shall be as indicated in the following rate schedule determined as follows: 1. Approximately 6,680 square feet of office space. $ 58,280.00 2. Approximately 380 square feet of space in the foyer. $ 3,314.00

129

ENERGY STAR Success Story: Staples, Inc.  

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

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

130

TRAN-STAR EXECUTIVE LIMOUSINE COMPANY  

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

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

131

COMMITTEE OF CENTERS AND  

E-Print Network [OSTI]

...................................................................................................... 75 9. CENTER FOR ELECTRIC CAR AND ENERGY CONVERSION............................................... 89

Massachusetts at Lowell, University of

132

2013 Bisfuel Center Retreat at Camp Tontozona | Center for Bio...  

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

Center News Research Highlights Center Research News Media about Center Center Video Library Bisfuel Picture Gallery 2013 Bisfuel Center Retreat at Camp Tontozona 28 Oct 2013 The...

133

BPS Skyrmions as neutron stars  

E-Print Network [OSTI]

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

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

2014-07-14T23:59:59.000Z

134

BPS Skyrmions as neutron stars  

E-Print Network [OSTI]

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

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

2014-07-14T23:59:59.000Z

135

Alternative Fuels Data Center: Biodiesel Blends  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Blends to Blends to someone by E-mail Share Alternative Fuels Data Center: Biodiesel Blends on Facebook Tweet about Alternative Fuels Data Center: Biodiesel Blends on Twitter Bookmark Alternative Fuels Data Center: Biodiesel Blends on Google Bookmark Alternative Fuels Data Center: Biodiesel Blends on Delicious Rank Alternative Fuels Data Center: Biodiesel Blends on Digg Find More places to share Alternative Fuels Data Center: Biodiesel Blends on AddThis.com... More in this section... Biodiesel Basics Blends Production & Distribution Specifications Related Links Benefits & Considerations Stations Vehicles Laws & Incentives Biodiesel Blends Biodiesel can be blended and used in many different concentrations, including B100 (pure biodiesel), B20 (20% biodiesel, 80% petroleum diesel),

136

STAR Teaching Program Application Period | Department of Energy  

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

STAR Teaching Program Application Period STAR Teaching Program Application Period STAR Teaching Program Application Period December 28, 2012 2:30PM EST to January 31, 2013 5:30PM EST Cal Poly The Science Teacher and Researcher (STAR) Researcher program, a collaborative project of California State University, provides pre-service and early career science teachers with eight week long paid mentor and research opportunities at a national research center. Applicants must have the following: A demonstrated interest in becoming a science or mathematics teacher at the secondary level (grades 6-12) Either a California State University (CSU) student OR NSF Noyce Scholar in the United States OR a STAR Alum with two or fewer years of participation AND two or fewer years of teaching experience (first time participants must be pre-service teachers, i.e., not yet teaching full-time

137

Data Center Report to Congress -FINAL 7-25-07.doc  

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

Server and Data Center Energy Efficiency Server and Data Center Energy Efficiency Public Law 109-431 U.S. Environmental Protection Agency ENERGY STAR Program August 2, 2007 Table of Contents Table of Contents............................................................................................................................. i Executive Summary ........................................................................................................................ 4 Background ................................................................................................................................. 4 Energy Use in Data Centers Through 2011 ................................................................................ 7 Incentives and Voluntary Programs to Promote Energy Efficiency ......................................... 11

138

Stars and statistical physics: A teaching experience  

Science Journals Connector (OSTI)

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

Roger Balian; Jean-Paul Blaizot

1999-01-01T23:59:59.000Z

139

Maintaining STAR - Hanford Site  

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

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

140

Star-ND (Multi-Dimensional Star-Identification)  

E-Print Network [OSTI]

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

Spratling, Benjamin

2012-07-16T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

ATOMIC HYDROGEN IN A GALACTIC CENTER OUTFLOW  

SciTech Connect (OSTI)

We describe a population of small, high-velocity, atomic hydrogen clouds, loops, and filaments found above and below the disk near the Galactic center. The objects have a mean radius of 15 pc, velocity widths of {approx}14 km s{sup -1}, and are observed at |z| heights up to 700 pc. The velocity distribution of the clouds shows no signature of Galactic rotation. We propose a scenario where the clouds are associated with an outflow from a central star-forming region at the Galactic center. We discuss the clouds as entrained material traveling at {approx}200 km s{sup -1} in a Galactic wind.

McClure-Griffiths, N. M.; Green, J. A.; Hill, A. S. [Australia Telescope National Facility, CSIRO Astronomy and Space Science, Marsfield, NSW 2122 (Australia); Lockman, F. J. [National Radio Astronomy Observatory, Green Bank, WV 24944 (United States); Dickey, J. M. [School of Physics and Mathematics, University of Tasmania, TAS 7001 (Australia); Gaensler, B. M.; Green, A. J., E-mail: naomi.mcclure-griffiths@csiro.au [Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006 (Australia)

2013-06-10T23:59:59.000Z

142

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

E-Print Network [OSTI]

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

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

2008-01-01T23:59:59.000Z

143

ENERGY STAR certification | ENERGY STAR Buildings & Plants  

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

ENERGY STAR certification ENERGY STAR certification Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Facts and stats Climate change and buildings ENERGY STAR certification

144

Hadronic matter and rapidly rotating compact stars  

SciTech Connect (OSTI)

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

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

1994-03-01T23:59:59.000Z

145

Condensation temperature trends among stars with planets  

E-Print Network [OSTI]

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

Guillermo Gonzalez

2005-12-08T23:59:59.000Z

146

Video Center Administrator Guide  

E-Print Network [OSTI]

LifeSize® Video Center Administrator Guide March 2011 LifeSize Video Center 2200 #12;LifeSize Video Center Adminstrator Guide 2 Administering LifeSize Video Center LifeSize Video Center is a network server that stores and streams video sent by LifeSize video communications systems enabled for recording. It can also

Eisen, Michael

147

Neutron Stars and Fractal Dimensionality  

E-Print Network [OSTI]

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

Burra G. Sidharth

2008-05-06T23:59:59.000Z

148

Carbon Stars | Open Energy Information  

Open Energy Info (EERE)

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

149

Energy Center Center for Coal Technology Research  

E-Print Network [OSTI]

Energy Center Center for Coal Technology Research http://www.purdue.edu/dp/energy/CCTR/ Consumption Production Gasification Power Plants Coking Liquid Fuels Environment Oxyfuels Byproducts Legislation, 500 Central Drive West Lafayette, IN 47907-2022 #12;INDIANA COAL REPORT 2009 Center for Coal

Fernández-Juricic, Esteban

150

Chemical Hydrogen Storage Center Center of Excellence  

E-Print Network [OSTI]

alternatives and assess economics and life cycle analysis of borohydride/water to hydrogen · Millennium CellChemical Hydrogen Storage Center Center of Excellence for Chemical Hydrogen Storage William Tumas proprietary or confidential information #12;2 Chemical Hydrogen Storage Center Overview Project Start Date: FY

Carver, Jeffrey C.

151

Home : ENERGY STAR  

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

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

152

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

E-Print Network [OSTI]

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

Ignazio Bombaci; Bhaskar Datta

2000-01-27T23:59:59.000Z

153

PNNL: News Center - Search  

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

Newsroom Search the News Center Keywords Search News Center News Center Home News Releases Social Media Directory PNNL Leadership Our Experts Subscribe to E-Mail News Service RSS...

154

Centers | ornl.gov  

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

Centers Centers SHARE Centers BioEnergy Science Center (BESC) The BioEnergy Science Center (BESC) is a multi-institutional (17 partners), multidisciplinary research (biological, chemical, physical and computational sciences, mathematics and engineering) organization focused on the fundamental understanding and elimination of biomass recalcitrance. DOE Energy Frontier Research Centers The Energy Frontier Research Centers program aims to accelerate such transformative discovery, combining the talents and creativity of our national scientific workforce with a powerful new generation of tools for penetrating, understanding, and manipulating matter on the atomic and molecular scales. ORNL is also home to two DOE Energy Frontier Research Centers, the Fluid Interface, Reactions, Structures and Transport (FIRST)

155

Benchmarking Help Center Guide  

Broader source: Energy.gov [DOE]

Benchmarking Help Center Guide provides recommendations for establishing a benchmarking help center based on experiences and lessons learned in New York City and Seattle.

156

Energy Efficient Data Centers  

Broader source: Energy.gov [DOE]

Presentationgiven at the Federal Utility Partnership Working Group (FUPWG) Fall 2008 meetingcovers energy efficiency improvement opportunities for data centers, including data center design.

157

Multiwavelength Phenomenology of Isolated Neutron Stars  

E-Print Network [OSTI]

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

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

1995-02-07T23:59:59.000Z

158

Magnetic fields in Neutron Stars  

E-Print Network [OSTI]

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

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

2015-01-01T23:59:59.000Z

159

Observational Cosmology With Semi-Relativistic Stars  

E-Print Network [OSTI]

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

Loeb, Abraham

2014-01-01T23:59:59.000Z

160

Statistical theory of thermal evolution of neutron stars  

E-Print Network [OSTI]

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

Beznogov, M V

2014-01-01T23:59:59.000Z

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


161

S M Stoller Star Center-B100  

Office of Legacy Management (LM)

B100 B100 7030-226/Monthly Accutest Job Number: F27169 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director

162

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

7170 7170 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director e-Hardcopy 2.0 Automated Report 12 1 of 12

163

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

227 227 Sampling Dates: 03/31/04 - 04/01/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director e-Hardcopy 2.0 Automated Report

164

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

WWNA Monthly; Largo, FL WWNA Monthly; Largo, FL 7031-226 Accutest Job Number: F36361 Sampling Date: 11/03/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

165

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

124 124 Sampling Date: 01/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director e-Hardcopy 2.0 Automated Report 18 1 of 18

166

S M Stoller Quarterly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

531 531 Sampling Date: 04/16/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director e-Hardcopy 2.0 Automated Report 21 1 of 21

167

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

8014 8014 Sampling Date: 11/09/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director e-Hardcopy 2.0 Automated Report 12 1 of 12

168

S M Stoller Star Center-B100  

Office of Legacy Management (LM)

B100 B100 110406202 Accutest Job Number: F33040 Sampling Date: 07/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D. Laboratory Director

169

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

WWNA Monthly; Largo, FL WWNA Monthly; Largo, FL 110406202 Accutest Job Number: F25982 Sampling Date: 08/10/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

170

S M Stoller Star Center-B100  

Office of Legacy Management (LM)

B100 B100 Monthly Sampling, 110406202 Accutest Job Number: F25245 Sampling Date: 07/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

171

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

WWNA Monthly; Largo, FL WWNA Monthly; Largo, FL 7030-226 Accutest Job Number: F33038 Sampling Date: 07/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results contained within this data package meet the requirements of the National Environmental Laboratory Accreditation Conference and/or state specific certification programs as applicable. Harry Behzadi, Ph.D.

172

S M Stoller Monthly Sampling (Pinellas Co), STAR Center, Largo...  

Office of Legacy Management (LM)

* Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http:www.accutest.com Test results contained within this data package meet the requirements of the National...

173

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

623 Sampling Date: 020205 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ...

174

S M Stoller Star Center-WWNA Monthly; Largo, FL  

Office of Legacy Management (LM)

Chloroform ND 1.0 0.50 ugl 110-75-8 2-Chloroethyl vinyl ether ND 5.0 2.5 ugl 56-23-5 Carbon tetrachloride ND 1.0 0.50 ugl 75-34-3 1,1-Dichloroethane ND 1.0 0.50 ugl 75-35-4...

175

S M Stoller Monthly Sampling, STAR Center, Largo, FL  

Office of Legacy Management (LM)

Chloroform ND 1.0 0.50 ugl 110-75-8 2-Chloroethyl vinyl ether ND 5.0 2.5 ugl 56-23-5 Carbon tetrachloride ND 1.0 0.50 ugl 75-34-3 1,1-Dichloroethane ND 1.0 0.50 ugl 75-35-4...

176

Neutron stars in f(R) gravity with perturbative constraints  

SciTech Connect (OSTI)

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

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

2010-09-15T23:59:59.000Z

177

Hyperons in neutron stars  

E-Print Network [OSTI]

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

Katayama, Tetsuya

2015-01-01T23:59:59.000Z

178

On the conversion of neutron stars into quark stars  

E-Print Network [OSTI]

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

Giuseppe Pagliara

2013-12-04T23:59:59.000Z

179

Designing for Sustainability: Houston DOW Center LEED Gold  

E-Print Network [OSTI]

materials ? Plastic moving crates in place of cardboard boxes ? Energy Star rated appliances ? Secondary Goals ? Building operating cost savings ? Community outreach Driving Energy Efficiency at Dow Designing for Sustainability Houston Dow Center... capable of housing 1,200 employees ? Energy efficient ? Sustainable ? Good location close to employees ? Cost effective ? Project to be started in 2007 and completed by November 2008 Designing for Sustainability Houston Dow Center Search for a LEED...

McCall, H.; McVey, K.; Rash, A.

180

Reliability-Centered Maintenance  

Broader source: Energy.gov [DOE]

Reliability-centered maintenance leverages the same practices and technologies of predictive maintenance.

Note: This page contains sample records for the topic "difference star center" 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

Neutron stars - thermal emitters  

E-Print Network [OSTI]

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

Potekhin, A Y; Pons, J A

2014-01-01T23:59:59.000Z

182

Masers and star formation  

E-Print Network [OSTI]

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

Vincent L. Fish

2007-04-02T23:59:59.000Z

183

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

AFDC AFDC Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Alternative Fuels Data Center: Page Not Found Skip to Content Eere_header_logo U.S. Department of Energy Energy Efficiency and Renewable Energy EERE Home | Programs & Offices | Consumer Information Alternative Fuels Data Center Search Search Help Alternative Fuels Data Center Fuels & Vehicles Biodiesel | Diesel Vehicles

184

Holographic Neutron Stars  

E-Print Network [OSTI]

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

Jan de Boer; Kyriakos Papadodimas; Erik Verlinde

2009-07-16T23:59:59.000Z

185

Guidance for Preparing ENERGY STAR Challenge for Industry Plant Profile  

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

Long Beach Douglas Center Long Beach Douglas Center The Boeing Company 4000 Lakewood Blvd. Long Beach, CA 90808 The Boeing Long Beach Douglas Center campus hosts a wide array of activities supporting the development of commercial airplanes including: Airplane Programs Engineering, Product Support Engineering, Modification Services, Spares, and Continental Data Graphics. This site achieved the Challenge for Industry in 2010, 2011 and 2012. Achieving the ENERGY STAR Challenge for Industry has been a key factor in Boeing's 'four walls' strategy to reduce energy usage and waste along with reducing the environmental footprint of its operations. The energy savings was achieved by upgrading air-conditioning, lighting and energy-management systems,

186

A star cluster at the edge of the Galaxy  

E-Print Network [OSTI]

We study stars and molecular gas in the direction of IRAS06145+1455 (WB89-789) through NIR (JHK), molecular line-, and dust continuum observations. The kinematic distance of the associated molecular cloud is 11.9 kpc. With a galactocentric distance of about 20.2 kpc, this object is at the edge of the (molecular) disk of the Galaxy. The near-IR data show the presence of an (embedded) cluster of about 60 stars, with a radius ca. 1.3 pc and an average stellar surface density of ca. 12 pc^{-2}. We find at least 14 stars with NIR-excess, 3 of which are possibly Class I objects. The cluster is embedded in a 1000 Mo molecular/dust core, from which a molecular outflow originates. The temperature of most of the outflowing gas is < 40 K, and the total mass of the swept-up material is < 10 Mo. Near the center of the flow, indications of much higher temperatures are found, probably due to shocks. A spectrum of one of the probable cluster members shows a tentative likeness to that of a K3III-star (with an age of at least 20 Myr). If correct, this would confirm the kinematic distance. This cluster is the furthest one from the Galactic center yet detected. The combination of old and recent activity implies that star formation has been going on for at least 20 Myr, which is difficult to understand considering the location of this object, where external triggers are either absent or weak, compared to the inner Galaxy. This suggests that once star formation is occurring, later generations of stars may form through the effect of the first generation of stars on the (remnants of) the original molecular cloud.

J. Brand; J. G. A. Wouterloot

2007-02-20T23:59:59.000Z

187

The Era of Star Formation in Galaxy Clusters  

E-Print Network [OSTI]

We analyze the star formation properties of 16 infrared-selected, spectroscopically confirmed galaxy clusters at $1 1.35$. Using infrared luminosities measured with deep Spitzer/MIPS observations at 24 $\\mu$m, along with robust optical+IRAC photometric redshifts and SED-fitted stellar masses, we present the dust-obscured star-forming fractions, star formation rates and specific star formation rates in these clusters as functions of redshift and projected clustercentric radius. We find that $z\\sim 1.4$ represents a transition redshift for the ISCS sample, with clear evidence of an unquenched era of cluster star formation at earlier times. Beyond this redshift the fraction of star-forming cluster members increases monotonically toward the cluster centers. Indeed, the specific star formation rate in the cores of these distant clusters is consistent with field values at similar redshifts, indicating that at $z>1.4$ environment-dependent quenching had not yet been established in ISCS clusters. Combining these obse...

Brodwin, M; Gonzalez, Anthony H; Zeimann, G R; Snyder, G F; Mancone, C L; Pope, A; Eisenhardt, P R; Stern, D; Alberts, S; Ashby, M L N; Brown, M J I; Chary, R -R; Dey, Arjun; Galametz, A; Gettings, D P; Jannuzi, B T; Miller, E D; Moustakas, J; Moustakas, L A

2013-01-01T23:59:59.000Z

188

Our Knowledge of High-Mass Star Formation at the Dawn of Herschel  

E-Print Network [OSTI]

We review the theories and observations of high-mass star formation emphasizing the differences with those of low-mass star formation. We hereafter describe the progress expected to be achieved with Herschel, thanks notably to Key Programmes dedicated to the earliest phases of high-mass star formation.

Frdrique Motte; Patrick Hennebelle

2008-06-04T23:59:59.000Z

189

SHOCKED SUPERWINDS FROM THE z {approx} 2 CLUMPY STAR-FORMING GALAXY, ZC406690  

SciTech Connect (OSTI)

We have obtained high-resolution data of the z {approx} 2 ring-like, clumpy star-forming galaxy (SFG) ZC406690 using the VLT/SINFONI with adaptive optics (in K band) and in seeing-limited mode (in H and J bands). Our data include all of the main strong optical emission lines: [O II], [O III], H{alpha}, H{beta}, [N II], and [S II]. We find broad, blueshifted H{alpha} and [O III] emission line wings in the spectra of the galaxy's massive, star-forming clumps ({sigma} {approx} 85 km s{sup -1}) and even broader wings (up to 70% of the total H{alpha} flux, with {sigma} {approx} 290 km s{sup -1}) in regions spatially offset from the clumps by {approx}2 kpc. The broad emission likely originates from large-scale outflows with mass outflow rates from individual clumps that are 1-8 Multiplication-Sign the star formation rate (SFR) of the clumps. Based on emission line ratio diagnostics ([N II]/H{alpha} and [S II]/H{alpha}) and photoionization and shock models, we find that the emission from the clumps is due to a combination of photoionization from the star-forming regions and shocks generated in the outflowing component, with 5%-30% of the emission deriving from shocks. In terms of the ionization parameter (6 Multiplication-Sign 10{sup 7} to 10{sup 8} cm s{sup -1}, based on both the SFR and the O{sub 32} ratio), density (local electron densities of 300-1800 cm{sup -3} in and around the clumps, and ionized gas column densities of 1200-8000 M{sub Sun }pc{sup -2}), and SFR (10-40 M{sub Sun} yr{sup -1}), these clumps more closely resemble nuclear starburst regions of local ultraluminous infrared galaxies and dwarf irregulars than H II regions in local galaxies. However, the star-forming clumps are not located in the nucleus as in local starburst galaxies but instead are situated in a ring several kpc from the center of their high-redshift host galaxy, and have an overall disk-like morphology. The two brightest clumps are quite different in terms of their internal properties, energetics, and relative ages, and thus we are given a glimpse at two different stages in the formation and evolution of rapidly star-forming giant clumps at high-z.

Newman, Sarah F.; Genzel, Reinhard [Department of Astronomy, Campbell Hall, University of California, Berkeley, CA 94720 (United States); Shapiro Griffin, Kristen [Aerospace Research Laboratories, Northrop Grumman Aerospace Systems, Redondo Beach, CA 90278 (United States); Davies, Ric; Foerster-Schreiber, Natascha M.; Tacconi, Linda J.; Kurk, Jaron; Wuyts, Stijn; Genel, Shy; Buschkamp, Peter; Eisenhauer, Frank; Lutz, Dieter [Max-Planck-Institut fuer extraterrestrische Physik (MPE), Giessenbachstr.1, D-85748 Garching (Germany); Lilly, Simon J.; Carollo, C. Marcella [Institute of Astronomy, Department of Physics, Eidgenoessische Technische Hochschule, ETH Zuerich CH-8093 (Switzerland); Renzini, Alvio; Mancini, Chiara [Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, Padova I-35122 (Italy); Bouche, Nicolas [Department of Physics and Astronomy, University of California, Santa Barbara, Santa Barbara, CA 93106 (United States); Burkert, Andreas [Department fuer Physik, Universitaets-Sternwarte Ludwig-Maximilians-Universitaet (USM), Scheinerstr. 1, Muenchen, D-81679 (Germany); Cresci, Giovanni [Istituto Nazionale di AstrofisicaOsservatorio Astronomico di Arcetri, Largo Enrico Fermi 5, I 50125 Firenze (Italy); Hicks, Erin, E-mail: sfnewman@berkeley.edu [Department of Astronomy, University of Washington, Box 351580, U.W., Seattle, WA 98195-1580 (United States); and others

2012-06-20T23:59:59.000Z

190

The Kepler characterization of the variability amongst A- and F-type stars. I. General overview  

E-Print Network [OSTI]

The Kepler spacecraft is providing time series of photometric data with micromagnitude precision for hundreds of A-F type stars. We present a first general characterization of the pulsational behaviour of A-F type stars as observed in the Kepler light curves of a sample of 750 candidate A-F type stars. We propose three main groups to describe the observed variety in pulsating A-F type stars: gamma Dor, delta Sct, and hybrid stars. We assign 63% of our sample to one of the three groups, and identify the remaining part as rotationally modulated/active stars, binaries, stars of different spectral type, or stars that show no clear periodic variability. 23% of the stars (171 stars) are hybrid stars, which is a much larger fraction than what has been observed before. We characterize for the first time a large number of A-F type stars (475 stars) in terms of number of detected frequencies, frequency range, and typical pulsation amplitudes. The majority of hybrid stars show frequencies with all kinds of periodicities...

Uytterhoeven, K; Grigahcene, A; Guzik, J A; Gutierrez-Soto, J; Smalley, B; Handler, G; Balona, L A; Niemczura, E; Machado, L Fox; Benatti, S; Chapellier, E; Tkachenko, A; Szabo, R; Suarez, J C; Ripepi, V; Pascual, J; Mathias, P; Martin-Ruiz, S; Lehmann, H; Jackiewicz, J; Hekker, S; Gruberbauer, M; Garcia, R A; Dumusque, X; Diaz-Fraile, D; Bradley, P; Antoci, V; Roth, M; Leroy, B; Murphy, S J; De Cat, P; Cuypers, J; Kjeldsen, H; Christensen-Dalsgaard, J; Breger, M; Pigulski, A; Kiss, L L; Still, M; Thompson, S E; Van Cleve, J

2011-01-01T23:59:59.000Z

191

ENERGY STAR industrial partnership | ENERGY STAR Buildings & Plants  

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

ENERGY STAR industrial partnership ENERGY STAR industrial partnership Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance ENERGY STAR industrial partnership New ENERGY STAR industrial partners Energy guides Energy efficiency and air regulation

192

Use ENERGY STAR benchmarking tools | ENERGY STAR Buildings & Plants  

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

Use ENERGY STAR benchmarking tools Use ENERGY STAR benchmarking tools Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use Learn about benchmarking Use ENERGY STAR benchmarking tools ENERGY STAR in action Communicate and educate

193

Star Power | Princeton Plasma Physics Lab  

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

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

194

ENERGY STAR | Open Energy Information  

Open Energy Info (EERE)

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

195

Compact boson stars in K field theories  

E-Print Network [OSTI]

We study a scalar field theory with a non-standard kinetic term minimally coupled to gravity. We establish the existence of compact boson stars, that is, static solutions with compact support of the full system with self-gravitation taken into account. Concretely, there exist two types of solutions, namely compact balls on the one hand, and compact shells on the other hand. The compact balls have a naked singularity at the center. The inner boundary of the compact shells is singular, as well, but it is, at the same time, a Killing horizon. These singular, compact shells therefore resemble black holes.

C. Adam; N. Grandi; P. Klimas; J. Sanchez-Guillen; A. Wereszczynski

2009-09-16T23:59:59.000Z

196

Compact boson stars in K field theories  

E-Print Network [OSTI]

We study a scalar field theory with a non-standard kinetic term minimally coupled to gravity. We establish the existence of compact boson stars, that is, static solutions with compact support of the full system with self-gravitation taken into account. Concretely, there exist two types of solutions, namely compact balls on the one hand, and compact shells on the other hand. The compact balls have a naked singularity at the center. The inner boundary of the compact shells is singular, as well, but it is, at the same time, a Killing horizon. These singular, compact shells therefore resemble black holes.

Adam, C; Klimas, P; Snchez-Guilln, J; Wereszczynski, A

2009-01-01T23:59:59.000Z

197

On Star Formation Rates in Dwarf Galaxies  

E-Print Network [OSTI]

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

Peter M. Weilbacher; Uta Fritze-v. Alvensleben

2001-05-16T23:59:59.000Z

198

SPECTROSCOPIC METALLICITY DETERMINATIONS FOR W UMa-TYPE BINARY STARS  

SciTech Connect (OSTI)

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

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

2013-09-15T23:59:59.000Z

199

Tracking Elevated Pollution Layers with a Newly Developed Hyperspectral Sun/Sky Spectrometer (4STAR): Results from the TCAP 2012 and 2013 Campaigns  

SciTech Connect (OSTI)

Total columnar amounts of water vapor, nitrogen dioxide (NO2) and ozone (O3) are derived from a newly developed, hyperspectral airborne sun-sky spectrometer (4STAR) for the first time during the two intensive phases of the Two Column Aerosol Project (TCAP) in summer 2012 and winter 2013 aboard the DOE G-1 aircraft. We compare results with coincident measurements. We find 0.045 g/cm2 (4.2%) negative bias and 0.28 g/cm2 (26.3%) root-mean-square (RMS) difference in water vapor layer comparison with in-situ hygrometer, and an overall RMS difference of 1.28 g/m3 (38%) water vapor amount in profile by profile comparisons, with differences distributed evenly around zero in most cases. The RMS differences for O3 values average to 3%, with a 1% negative bias for 4STAR compared with the spaceborne Ozone Measuring Instrument (OMI) along the aircraft flight-track for 14 flights during both TCAP phases. Ground-based comparisons with the Pandora spectrometer system at the Goddard Space Flight Center (GSFC), Greenbelt, Maryland showed excellent agreement between the instruments for both O3 and NO2, further emphasizing 4STARs new capabilities. During the summer phase, we have succeeded in identifying variations in elevated pollution layers corresponding to urban pollution outflow and transported biomass burning. This was done using clustering analysis of the retrieved products (e.g. ngstrom exponent, NO2 and columnar water vapor), and was confirmed by aerosol type identification by HSRL2 aboard the NASA B-200 aircraft. These newly demonstrated 4STAR capabilities are expected to be instrumental in improving our understanding of atmospheric composition variability and aerosol-trace-gas interactions; they open new horizons and opportunities in airborne sunphotometry.

Segal Rozenhaimer, Michal; Russell, P. B.; Schmid, Beat; Redemann, Jens; Livingston, J. M.; Flynn, Connor J.; Johnson, Roy R.; Dunagan, Stephen; Shinozuka, Yohei; Herman, J. R.; Cede, A.; Abuhassan, N.; Comstock, Jennifer M.; Hubbe, John M.; Zelenyuk, Alla; Wilson, Jacqueline M.

2014-03-16T23:59:59.000Z

200

Tidal Love Numbers of Neutron Stars  

SciTech Connect (OSTI)

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

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

2008-04-20T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

Lujan Center User Guide  

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

1 1 The Surface Profile Analysis Reflectometer (SPEAR), located on Flight Path 9 in the Lujan Center, is ideally suited to study thin (from 5 - 3000 Å) organic and inorganic layers in a variety of different environments. The instrument uses an unpolarized neutron beam to study a broad range of materials including polymers, nano-engineered films, and biological systems. SPEAR is a time-of-flight (TOF) reflectometer using 2 choppers to define a typical wavelength range of 4.5 Å - 16 Å. With this polychromatic beam, a range of momentum transfer vectors (Q z ) can be measured without altering the angle of the incident beam. An important feature of SPEAR's design is that the beam is inclined to the horizon at 1.0°±0.0.25 This inclination allows for reflectivity

202

Predictions from star formation in the multiverse  

SciTech Connect (OSTI)

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

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

2010-03-15T23:59:59.000Z

203

Variable Star Network: World Center for Transient Object Astronomy and Variable Stars  

Science Journals Connector (OSTI)

......from the Ministry of Education, Culture, Sports, Science and Technology. Part...for the Promotion of Science for Young Scientists...GCVS. Appendix 1. Poster Presented at the 23rd...for the Promotion of Science for Young Scientists......

Taichi Kato; Makoto Uemura; Ryoko Ishioka; Daisaku Nogami; Chatief Kunjaya; Hajime Baba; Hitoshi Yamaoka

2004-03-25T23:59:59.000Z

204

Variable Star Network: World Center for Transient Object Astronomy and Variable Stars  

Science Journals Connector (OSTI)

......2001; Duerbeck 2002; Clayton 2002; Jeffery, Pollacco 2002; Kamath, Ashok 2002...Frank J. 1982b, Nature, 300, 152. Jeffery C. S. , Pollacco D. 2002, ApSS, 279...7253. Swartz D. A. , Clocchiatti A., Benjamin R., Lester D. F., Wheeler J. C......

Taichi Kato; Makoto Uemura; Ryoko Ishioka; Daisaku Nogami; Chatief Kunjaya; Hajime Baba; Hitoshi Yamaoka

2004-03-25T23:59:59.000Z

205

Improving the Energy Performance of Data Centers  

E-Print Network [OSTI]

to most data centers. The second uses air-side economizers (air-side economizer scenario (ASE) requires a different type of air delivery than typically found in a data centerdata centers. The performance ratios for the ASE and WSE scenarios show that air-side economizers

Horvath, A; Shehabi, Arman

2008-01-01T23:59:59.000Z

206

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Center to someone by E-mail Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Federal State Advanced Search All Laws & Incentives Sorted by Type Local Laws and Incentives There are a variety of local laws and incentives that support reducing U.S. petroleum consumption by encouraging or requiring individuals and/or public and private organizations to use alternative fuels, advanced vehicles, and strategies to decrease fuel use or increase fuel economy. Local city and county governments create such laws and incentives to ensure people use

207

About Cost Center  

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

from the university, fee-for-service contracts, as well as establishing CAMD as a cost center. We know that our users are reluctant to see CAMD become a cost center, however...

208

NREL: Education Center - Events  

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

phone number is 303-384-6565. November 2014 Education Center Holiday Hours November 26 - December 1, 2014 Golden, CO Contact: NREL Education Center 303-384-6565 The NREL...

209

ARM - News Center Archive  

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

3 1 BAECC 1 BBOP 4 ENA 1 GOAMAZON 6 MAGIC 15 MC3E 17 SGP 3 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center...

210

LANSCE | Lujan Center | Publications  

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

use of add here name of specific Lujan instruments at the Lujan Center at Los Alamos Neutron Science Center. Los Alamos National Laboratory is operated by Los Alamos National...

211

ENERGY CENTER OF WISCONSIN  

E-Print Network [OSTI]

ENERGY CENTER OF WISCONSIN report report report report report report report report report report energy center Report 193-1 Fuel Cells for Distributed Generation A Technology and Marketing Summary March

Wisconsin at Madison, University of

212

INTERNATIONAL PACIFIC RESEARCH CENTER  

E-Print Network [OSTI]

INTERNATIONAL PACIFIC RESEARCH CENTER APRIL 2004­MARCH 2005 REPORT SCHOOL OF OCEAN AND EARTH RESEARCH HIGHLIGHTS Indo-Pacific Ocean Climate Pacific Research Center Design by: Susan Yamamoto Printed by: Hagadone Printing Company Photo: Waikiki

Wang, Yuqing

213

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Center to someone by E-mail Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Federal State Advanced Search All Laws & Incentives Sorted by Type Recent Federal Actions This list includes recent federal actions, such as Federal Register notices and rulemaking actions, agency directives or agency communications, that are all publicly available. These actions relate to alternative fuels and vehicles, fuel blends, hybrid vehicles, and idle reduction and fuel economy measures. When rulemakings are finalized, they will move to the list of

214

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Center to someone by E-mail Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Federal State Advanced Search All Laws & Incentives Sorted by Type Expired, Repealed, and Archived Federal Incentives and Laws The following is a list of expired, repealed, and archived incentives, laws, regulations, funding opportunities, or other initiatives related to alternative fuels and vehicles, advanced technologies, or air quality. Value-Added Producer Grants (VAPG) Archived: 12/31/2012

215

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Tools Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Truckstop Electrification Truck Stop Electrification Locator Locate truck stops with electrification sites. Click on a location on the map for site details. A U.S. Department of Energy Energy Efficiency and Renewable Energy Source: Alternative Fuels Data Center dditional Resources View list of electrification sites in the U.S. by state. Learn more about idle reduction techniques.

216

Cooling of neutron stars  

Science Journals Connector (OSTI)

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

C. J. Pethick

1992-10-01T23:59:59.000Z

217

On the efficiency of field star capture by star clusters  

E-Print Network [OSTI]

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

Steffen Mieske; Holger Baumgardt

2007-09-10T23:59:59.000Z

218

Energy Technology Engineering Center  

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

Technology Engineering Center Technology Engineering Center 41 00 Guardian Street, Suite # 160 Simi Valley, CA 93063 Memorandum for: Gregory H. Woods General Council January 30, 2013 FROM: John Jones EL\= Federal Proje� irector Energy Technology Engineering Center (ETEC) Project Office SUBJECT: Annual National Environmental Policy Act {NEPA) Planning Summary Attached is the 2013 Annual NEPA Planning Summary for the ETEC Project Office.

219

Louisiana Transportation Research Center  

E-Print Network [OSTI]

Louisiana Transportation Research Center LTRC www.ltrc.lsu.edu 2012-13 ANNUALREPORT #12;The Louisiana Transportation Research Center (LTRC) is a research, technology transfer, and training center administered jointly by the Louisiana Department of Transportation and Development (DOTD) and Louisiana State

Harms, Kyle E.

220

A Star on Earth  

ScienceCinema (OSTI)

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

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

2014-06-06T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

A Star on Earth  

SciTech Connect (OSTI)

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

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

2014-03-05T23:59:59.000Z

222

Aircraft Integration and Flight Testing of 4STAR  

SciTech Connect (OSTI)

Under funding from the U.S. Dept. of Energy, in conjunction with a funded NASA 2008 ROSES proposal, with internal support from Battelle Pacific Northwest Division (PNWD), and in collaboration with NASA Ames Research Center, we successfully integrated the Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research (4STAR-Air) instrument for flight operation aboard Battelles G-1 aircraft and conducted a series of airborne and ground-based intensive measurement campaigns (hereafter referred to as intensives) for the purpose of maturing the initial 4STAR-Ground prototype to a flight-ready science-ready configuration.

Flynn, CJ; Kassianov, E; Russell, P; Redemann, J; Dunagan, S; Holben, B

2012-10-12T23:59:59.000Z

223

Star Biomass | Open Energy Information  

Open Energy Info (EERE)

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

224

Center for Bio-inspired Solar Fuel Production Personnel | Center...  

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

Center for Bio-inspired Solar Fuel Production Personnel Principal Investigators Postdoctoral Fellows Center researchers Graduate Students Undergraduate Students All Bisfuel Center...

225

Star clusters as diaries of galaxies  

E-Print Network [OSTI]

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

Th. Maschberger; P. Kroupa

2007-06-11T23:59:59.000Z

226

Alternative Fuels Data Center: Vehicle Conversion Basics  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Vehicle Conversion Vehicle Conversion Basics to someone by E-mail Share Alternative Fuels Data Center: Vehicle Conversion Basics on Facebook Tweet about Alternative Fuels Data Center: Vehicle Conversion Basics on Twitter Bookmark Alternative Fuels Data Center: Vehicle Conversion Basics on Google Bookmark Alternative Fuels Data Center: Vehicle Conversion Basics on Delicious Rank Alternative Fuels Data Center: Vehicle Conversion Basics on Digg Find More places to share Alternative Fuels Data Center: Vehicle Conversion Basics on AddThis.com... Vehicle Conversion Basics Photo of a Ford Transit Connect converted to run on compressed natural gas. A Ford Transit Connect converted to run on compressed natural gas. A converted vehicle or engine is one modified to use a different fuel or

227

ENERGY STAR plant certification | ENERGY STAR Buildings & Plants  

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

» ENERGY STAR plant certification » ENERGY STAR plant certification Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Improve energy performance Industrial service and product providers Earn recognition ENERGY STAR Partner of the Year Award

228

Campaigns and incentive programs that incorporate ENERGY STAR | ENERGY STAR  

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

Campaigns and incentive programs that incorporate ENERGY STAR Campaigns and incentive programs that incorporate ENERGY STAR Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Policies that specify the use of ENERGY STAR tools Campaigns and incentive programs that incorporate ENERGY STAR Lead by example Gather support Develop programs and policies Host a competition Use financing vehicles

229

ENERGY STAR service and product provider training series | ENERGY STAR  

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

service and product provider training series service and product provider training series Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner ENERGY STAR service & product provider training series Service and product provider's marketing toolkit ENERGY STAR sales tools for service and product providers

230

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Tools Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Fuel Properties Search Fuel Properties Comparison Create a custom chart comparing fuel properties and characteristics for multiple fuels. Select the fuel and properties of interest. Select Fuels Clear all All Fuels Gasoline Diesel (No. 2) Biodiesel Compressed Natural Gas (CNG) Electricity Ethanol Hydrogen Liquefied Natural Gas (LNG) Propane (LPG)

231

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Electricity » Laws & Incentives Electricity » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Electricity Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for EVs The list below contains summaries of all Federal laws and incentives related to EVs. Incentives Alternative Fuel Infrastructure Tax Credit Fueling equipment for natural gas, liquefied petroleum gas (propane),

232

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Propane » Laws & Incentives Propane » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Propane Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for Propane (LPG) The list below contains summaries of all Federal laws and incentives related to Propane (LPG). Incentives Alternative Fuel Infrastructure Tax Credit Fueling equipment for natural gas, liquefied petroleum gas (propane),

233

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Biodiesel » Laws & Incentives Biodiesel » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Biodiesel Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for Biodiesel The list below contains summaries of all Federal laws and incentives related to Biodiesel. Incentives Alternative Fuel Infrastructure Tax Credit Fueling equipment for natural gas, liquefied petroleum gas (propane),

234

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Ethanol » Laws & Incentives Ethanol » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Ethanol Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for Ethanol The list below contains summaries of all Federal laws and incentives related to Ethanol. Incentives Alternative Fuel Infrastructure Tax Credit Fueling equipment for natural gas, liquefied petroleum gas (propane),

235

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Hydrogen » Laws & Incentives Hydrogen » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Hydrogen Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for Hydrogen Fuel Cells The list below contains summaries of all Federal laws and incentives related to Hydrogen Fuel Cells. Incentives Alternative Fuel Tax Exemption Alternative fuels used in a manner that the Internal Revenue Service (IRS)

236

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Tools Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Data Included in the Alternative Fuel Stations Download The following data fields are provided in the downloadable files for alternative fuel stations. Field Value Description fuel_type_code Type: string The type of alternative fuel the station provides. Fuel types are given as code values as described below: Value Description BD Biodiesel (B20 and above)

237

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Conserve Fuel » Laws & Incentives Conserve Fuel » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Biodiesel Electricity Ethanol Hydrogen Natural Gas Propane Emerging Fuels Fuel Prices Federal Laws and Incentives for Idle Reduction The list below contains summaries of all Federal laws and incentives related to Idle Reduction. Incentives Idle Reduction Technology Excise Tax Exemption Qualified on-board idle reduction devices and advanced insulation are

238

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Natural Gas » Laws & Incentives Natural Gas » Laws & Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Natural Gas Basics Benefits & Considerations Stations Vehicles Laws & Incentives Federal Laws and Incentives for Natural Gas The list below contains summaries of all Federal laws and incentives related to Natural Gas. Incentives Alternative Fuel Infrastructure Tax Credit Fueling equipment for natural gas, liquefied petroleum gas (propane),

239

ANALYTICAL STAR FORMATION RATE FROM GRAVOTURBULENT FRAGMENTATION  

SciTech Connect (OSTI)

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

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

2011-12-20T23:59:59.000Z

240

Physical Processes in Stars  

Science Journals Connector (OSTI)

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

R. J. TAYLER

1964-12-05T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

Explosive Nucleosynthesis in Stars  

Science Journals Connector (OSTI)

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

W. DAVID ARNETT; DONALD D. CLAYTON

1970-08-22T23:59:59.000Z

242

Young stars with discs  

Science Journals Connector (OSTI)

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

2000-01-01T23:59:59.000Z

243

LANSCE | Lujan Neutron Scattering Center  

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

Lujan Center Data Management Lujan Neutron Scattering Center Logo The Lujan Center within LANSCE utilizes a pulsed source and has a complement of 15 instruments. It maintains a...

244

About ENERGY STAR for commercial and industrial buildings | ENERGY STAR  

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

ENERGY STAR for commercial and industrial buildings ENERGY STAR for commercial and industrial buildings Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can we help you? Find out who's partnered with ENERGY STAR Become an ENERGY STAR partner Find ENERGY STAR certified buildings and plants ENERGY STAR certification Featured research and reports Facts and stats Climate change and buildings

245

Earn ENERGY STAR certification | ENERGY STAR Buildings & Plants  

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

Earn ENERGY STAR certification Earn ENERGY STAR certification Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can we help you? Build an energy program Improve building and plant performance Earn the ENERGY STAR and other recognition Benchmark energy use ENERGY STAR in action Communicate and educate ENERGY STAR communications toolkit Bring Your Green to Work with ENERGY STAR

246

THE STAR FORMATION LAW AT LOW SURFACE DENSITY  

SciTech Connect (OSTI)

We investigate the nature of the star formation law at low gas surface densities using a sample of 19 low surface brightness (LSB) galaxies with existing H I maps in the literature, UV imaging from the Galaxy Evolution Explorer satellite, and optical images from the Sloan Digital Sky Survey. All of the LSB galaxies have (NUV - r) colors similar to those for higher surface brightness star-forming galaxies of similar luminosity indicating that their average star formation histories are not very different. Based upon four LSB galaxies with both UV and far-infrared (FIR) data, we find FIR/UV ratios significantly less than 1, implying low amounts of internal UV extinction in LSB galaxies. We use the UV images and H I maps to measure the star formation rate (SFR) and hydrogen gas surface density within the same region for all the galaxies. The LSB galaxy star formation rate surface densities lie below the extrapolation of the power law fit to the SFR surface density as a function of the total gas density for higher surface brightness galaxies. Although there is more scatter, the LSB galaxies also lie below a second version of the star formation law in which the SFR surface density is correlated with the gas density divided by the orbital time in the disk. The downturn seen in both star formation laws is consistent with theoretical models that predict lower star formation efficiencies in LSB galaxies due to the declining molecular fraction with decreasing density.

Wyder, Ted K.; Martin, D. Christopher; Barlow, Tom A.; Foster, Karl; Friedman, Peter G.; Morrissey, Patrick; Neill, James D. [California Institute of Technology, MC 278-17, 1200 E. California Blvd., Pasadena, CA 91125 (United States); Neff, Susan G. [Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Greenbelt, MD, 20771 (United States); Schiminovich, David [Department of Astronomy, Columbia University, New York, NY 10027 (United States); Seibert, Mark; Madore, Barry F. [Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Bianchi, Luciana [Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218 (United States); Donas, Jose; Milliard, Bruno [Laboratoire d'Astrophysique de Marseille, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12 (France); Heckman, Timothy M.; Szalay, Alex S. [Department of Physics and Astronomy, Johns Hopkins University, Homewood Campus, Baltimore, MD 21218 (United States); Lee, Young-Wook; Yi, Sukyoung K. [Center for Space Astrophysics, Yonsei University, Seoul 120-749 (Korea, Republic of); Rich, R. Michael [Department of Physics and Astronomy, University of California, Los Angeles, CA 90095 (United States)

2009-05-10T23:59:59.000Z

247

Nomenclature of The Galactic Center Radio Sources  

E-Print Network [OSTI]

Since its identification as the Galactic Center, the radio source Sagittarius A has been a target of intense research. Due to the high density of sources in the Galactic Center and differing observing techniques, the nomenclature of sources in this region has changed over the years, with sources having several names, as well as the same names being used for different sources. We review this historical evolution in the context of current and previous scientific discussions, and outline how, why and when some of the commonly accepted names of Galactic Center sources were established.

Patrick Palmer; W. Miller Goss

1996-07-29T23:59:59.000Z

248

Energy Star | Open Energy Information  

Open Energy Info (EERE)

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

249

Center for Energy Nanoscience at USC  

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

People Click HERE for the complete Center Directory. Center Leadership Center Advisory Board Members...

250

Energy Efficient Data Centers  

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

Energy Efficient Data Centers Energy Efficient Data Centers Title Energy Efficient Data Centers Publication Type Report LBNL Report Number LBNL-54163 Year of Publication 2004 Authors Tschudi, William F., Tengfang T. Xu, Dale A. Sartor, Jonathan G. Koomey, Bruce Nordman, and Osman Sezgen Call Number LBNL-54163 Abstract Data Center facilities, prevalent in many industries and institutions are essential to Californias economy. Energy intensive data centers are crucial to Californias industries, and many other institutions (such as universities) in the state, and they play an important role in the constantly evolving communications industry. To better understand the impact of the energy requirements and energy efficiency improvement potential in these facilities, the California Energy Commissions PIER Industrial Program initiated this project with two primary focus areas: First, to characterize current data center electricity use; and secondly, to develop a research roadmap defining and prioritizing possible future public interest research and deployment efforts that would improve energy efficiency.

251

DOE Information Center  

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

DOE Information Center DOE Information Center The U.S. Department of Energy (DOE) Information Center provides citizens a consolidated facility to obtain information and records related to the DOE's various programs in Oak Ridge and abroad. Employees at the DOE Information Center are available to assist with your requests and searches from 8:00 a.m. to 5:00 p.m. (EST), Monday through Friday, except for federal holidays. Requests Documents can be requested in person or by telephone, email, or fax. Reproduction Please allow DOE Information Center staff adequate time to reproduce documents. Some material requires special handling, security reviews, etc. Delivery Unless special arrangements have been made with DOE Information Center staff, documents should be picked up during normal business hours.

252

Harnessing the Energy of the Stars | Department of Energy  

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

Harnessing the Energy of the Stars Harnessing the Energy of the Stars Harnessing the Energy of the Stars September 12, 2011 - 5:52pm Addthis A view of a cryogenically cooled National Ignition Facility (NIF) target as "seen" by the laser through the hohlraum's laser entrance hole. | Photo courtesy of Lawrence Livermore National Laboratory. A view of a cryogenically cooled National Ignition Facility (NIF) target as "seen" by the laser through the hohlraum's laser entrance hole. | Photo courtesy of Lawrence Livermore National Laboratory. Former Under Secretary Koonin Former Under Secretary Koonin Director - NYU's Center for Urban Science & Progress and Former Under Secretary for Science These are exciting times for fusion energy. Today I'm sharing that excitement with several hundred scientists at a conference on Inertial

253

Harnessing the Energy of the Stars | Department of Energy  

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

Harnessing the Energy of the Stars Harnessing the Energy of the Stars Harnessing the Energy of the Stars September 12, 2011 - 5:52pm Addthis A view of a cryogenically cooled National Ignition Facility (NIF) target as "seen" by the laser through the hohlraum's laser entrance hole. | Photo courtesy of Lawrence Livermore National Laboratory. A view of a cryogenically cooled National Ignition Facility (NIF) target as "seen" by the laser through the hohlraum's laser entrance hole. | Photo courtesy of Lawrence Livermore National Laboratory. Former Under Secretary Koonin Former Under Secretary Koonin Director - NYU's Center for Urban Science & Progress and Former Under Secretary for Science These are exciting times for fusion energy. Today I'm sharing that excitement with several hundred scientists at a conference on Inertial

254

On the appearance of hyperons in neutron stars  

E-Print Network [OSTI]

By employing a recently constructed hyperon-nucleon potential the equation of state of \\beta-equilibrated and charge neutral nucleonic matter is calculated. The hyperon-nucleon potential is a low-momentum potential which is obtained within a renormalization group framework. Based on the Hartree-Fock approximation at zero temperature the densities at which hyperons appear in neutron stars are estimated. For several different bare hyperon-nucleon potentials and a wide range of nuclear matter parameters it is found that hyperons in neutron stars are always present. These findings have profound consequences for the mass and radius of neutron stars.

Haris Djapo; Bernd-Jochen Schaefer; Jochen Wambach

2008-11-18T23:59:59.000Z

255

Solar-like oscillations in a massive star  

E-Print Network [OSTI]

Seismology of stars provides insight into the physical mechanisms taking place in their interior, with modes of oscillation probing different layers. Low-amplitude acoustic oscillations excited by turbulent convection were detected four decades ago in the Sun and more recently in low-mass main-sequence stars. Using data gathered by the Convection Rotation and Planetary Transits mission, we report here on the detection of solar-like oscillations in a massive star, V1449 Aql, which is a known large-amplitude (b Cephei) pulsator.

Belkacem, K; Goupil, M -J; Lefvre, L; Baudin, F; Deheuvels, S; Dupret, M -A; Appourchaux, T; Scuflaire, R; Auvergne, M; Catala, C; Michel, E; Miglio, A; Montalban, J; Thoul, A; Talon, S; Baglin, A; Noels, A

2009-01-01T23:59:59.000Z

256

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

conduct business in Missouri. New propane commercial mowers are eligible for 15% of the cost of the equipment. Dedicated propane mower conversions are eligible for 750. New center...

257

Call center construction underway  

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

Government Services Group are making significant progress on getting the Valor Telecommunications call center ready for occupancy. After only two weeks on the job, "design and...

258

The Center for Nanoscale  

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

for Nanoscale Materials (CNM) at Argonne for interdisciplinary nanoscience and nanotechnology researchers can apply to use CNM for both nonproprietary The Center's goal is to...

259

NREL: Education Center - Programs  

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

the work of NREL. Monthly tours are also offered to give visitors an overview of our sustainable campus and featured buildings. Printable Version Education Center Home Hours,...

260

Supergiant Pulses from Extragalactic Neutron Stars  

E-Print Network [OSTI]

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

Cordes, J M

2015-01-01T23:59:59.000Z

Note: This page contains sample records for the topic "difference star center" 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

CENTER REPORT Center for Environmental Policy  

E-Print Network [OSTI]

such as phosphate ores and water. Certificate in Environmental Policy and Management The Center for Environmental Policy oversees the administrative aspects of the Certificate in Environmental Policy and Management in Environmental Policy and Management Eliana Bardi, Biological Scientist Matt Cohen, Post Doctoral Associate Clay

Slatton, Clint

262

Selected topics in the evolution of low-mass stars  

E-Print Network [OSTI]

Low-mass stars play a key role in many different areas of astrophysics. In this article, I provide a brief overview of the evolution of low-mass stars, and discuss some of the uncertainties and problems currently affecting low-mass stellar models. Emphasis is placed on the following topics: the solar abundance problem, mass loss on the red giant branch, and the level of helium enrichment associated to the multiple populations that are present in globular clusters.

Catelan, M

2012-01-01T23:59:59.000Z

263

Alternative Fuels Data Center: About the Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

About About Printable Version Share this resource Send a link to Alternative Fuels Data Center: About the Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center: About the Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center: About the Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center: About the Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center: About the Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center: About the Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center: About the Alternative Fuels Data Center on AddThis.com... More in this section... Project Assistance News & Features

264

Northwestern University Transportation Center  

E-Print Network [OSTI]

Northwestern University Transportation Center 2011 Business Advisory Committee NUTC #12;#12;I have the pleasure of presenting our Business Advisory Committee members--a distinguished group of transportation industry lead- ers who have partnered with the Transportation Center in advancing the state of knowledge

Bustamante, Fabián E.

265

University Center Breakfast Menu  

E-Print Network [OSTI]

Includes iced water and your choice of iced tea or lemonade Choice of two salads: Tossed Green, CaliforniaUniversity Center Breakfast Menu Buffets Includes coffee, decaf, hot tea service, iced water Center Deli Buffet Includes iced water and your choice of iced tea or lemonade Choice of two salads

Lee, Herbie

266

ENERGY CENTER OF WISCONSIN  

E-Print Network [OSTI]

ENERGY CENTER OF WISCONSIN Report Summary 210-1 Life-Cycle Energy Costs and Greenhouse Gas report energy center Net energy balance and greenhouse gas emissions from renewable energy storage systems June 2003 223-1 #12;ECW Report Number 223-1 Net energy balance and greenhouse gas emissions from

267

& Education CenterOregon  

E-Print Network [OSTI]

Center 3. Bike Hub 4. Electric Avenue 5. Montgomery Green Street GEOTHERMAL & DISTRICT ENERGY Parking Structure 3 Ho man Hall West Heating Plant Blackstone Montgomery Research Greenhouses Simon Benson EFFICIENT HEATING AND COOLING LOOP #12;Academic and Student Recreation Center (ASRC) SW 6TH AND SW

Caughman, John

268

INTERNATIONAL PACIFIC RESEARCH CENTER  

E-Print Network [OSTI]

INTERNATIONAL PACIFIC RESEARCH CENTER APRIL 2005­MARCH 2006 REPORT SCHOOL OF OCEAN AND EARTH Center 1 The Year's Highlights 3 Indo-Pacific Ocean Climate 4 Regional-Ocean Influences 10 Asian Ocean Climate: To understand climate variations in the Pacific and Indian oceans on interannual

Wang, Yuqing

269

International Pacific Research Center  

E-Print Network [OSTI]

International Pacific Research Center APRIL 2007­MARCH 2008 REPORT School of Ocean and Earth Center i Foreword ii iv Indo-Pacific Ocean Climate 1 Regional-Ocean Influences 13 Asian by the following broad research themes and goals of the IPRC Science Plan. Indo-Pacific Ocean Climate

Wang, Yuqing

270

INTERNATIONAL PACIFIC RESEARCH CENTER  

E-Print Network [OSTI]

INTERNATIONAL PACIFIC RESEARCH CENTER Annual Report April 2006 ­ March 2007 School of Ocean Research Center 1 2 The Year's Highlights 3 Research Accomplishments Indo-Pacific Ocean Climate 4 Regional-Ocean Ocean Climate: To understand climate variations in the Pacific and Indian oceans on inter- annual

Wang, Yuqing

271

Northwestern University Transportation Center  

E-Print Network [OSTI]

and challenges for our society. Energy and sustainability, economic growth and development, quality of life in the world to recognize transportation as an interdisciplinary field, the Transportation Center was founded, as the tradition lives on, and the Center continues to renew itself and engage faculty and students with new

MacIver, Malcolm A.

272

ENERGY STAR Webinar: Financing Energy Efficient Upgrades with ENERGY STAR  

Broader source: Energy.gov [DOE]

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

273

Detection of intergalactic red-giant-branch stars in the Virgo cluster  

E-Print Network [OSTI]

It has been suspected for nearly 50 years that clusters of galaxies contain a population of intergalactic stars, ripped from galaxies during cluster formation or when the galaxies' orbits take them through the cluster center. Support for the existence of such a population of free-floating stars comes from measurements of the diffuse light in clusters, and from recent detections of planetary nebulae with positions and/or velocities far removed from any observed cluster galaxy. But estimates for the mass of the diffuse population and its distribution relative to the galaxies are still highly uncertain. Here we report the direct detection of intergalactic stars in deep images of a blank field in the Virgo Cluster. The data suggest that approximately 10% of the stellar mass of the cluster is in intergalactic stars. We observe a relatively homogeneous distribution of stars, with evidence of a slight gradient toward M87.

Henry C. Ferguson; Nial R. Tanvir; Ted von Hippel

1998-01-23T23:59:59.000Z

274

Energy Efficient Data Centers  

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

Federal Utility Partnership Working Group Federal Utility Partnership Working Group Will Lintner November 20, 2008 Williamsburg, VA 2 Why Data Centers? * Data centers are highly energy intensive and growing at a rapid rate - Consume 10 to 100 times more energy per square foot than typical office building * Data centers consumed about 45 billion kWh in 2005 and 61 billion kWh in 2006 - This accounts for nearly 1.2% and 1.5% of all U.S. electricity respectively * At current rate, power requirements for data centers could double in 5 years 3 Typical Data Center Energy Use Server Load /Computing Operations Cooling Equipment Power Conversions & Distribution 100 Units 33 Units Delivered 35 Units 4 4 Server Load/ Computing Operations Cooling Equipment Power Conversion & Distribution Alternative Power Generation * High voltage distribution

275

LANL: Superconductivity Technology Center  

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

Sitemap | Lab Home | Phone Sitemap | Lab Home | Phone ABOUT LANL ContactsPhonebookPolicy CenterOrganizationMapsJobs Emergency NEWS LIBRARY JOBS Search Materials Physics & Applications: STC STC Home OUR FOCUS HTS Physics HTS Materials Development HTS Materials Processing Power Applications Electronic Materials FUTURE APPLICATIONS Biomedical Developments Magnetic Levitation Train MHD Ship CONTACTS Center Leader Ken Marken Program Administrator Brenda Espinoza Center Office Location: TA-03, Bdg. 0032, Rm. 141 Exploring technology at STC Superconductivity Technology Center (STC) The Superconductivity Technology Center (STC) coordinates a multidisciplinary program for research, development, and technology transfer in the area of high-temperature superconductivity. Our focus is on effective collaborations with American industry, universities, and other national laboratories to develop electric power and electronic device applications of high-temperature superconductors (HTS).

276

ENERGY STAR SNAPSHOT - Spring 2009  

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

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

277

The evolution and explosion of massive Stars II: Explosive hydrodynamics and nucleosynthesis  

SciTech Connect (OSTI)

The nucleosynthetic yield of isotopes lighter than A = 66 (zinc) is determined for a grid of stellar masses and metallicities including stars of 11, 12, 13, 15, 18, 19, 20, 22, 25, 30, 35, and 40 M{sub {circle_dot}} and metallicities Z = 0, 10{sup {minus}4}, 0.01, 0.1, and 1 times solar (a slightly reduced mass grid is employed for non-solar metallicities). Altogether 78 different model supernova explosions are calculated. In each case nucleosynthesis has already been determined for 200 isotopes in each of 600 to 1200 zones of the presupernova star, including the effects of time dependent convection. Here each star is exploded using a piston to give a specified final kinetic energy at infinity (typically 1.2 {times} 10{sup 51} erg), and the explosive modifications to the nucleosynthesis, including the effects of neutrino irradiation, determined. A single value of the critical {sup 12}C({sub {alpha},{gamma}}){sup 16}O reaction rate corresponding to S(300 keV) = 170 keV barns is used in all calculations. The synthesis of each isotope is discussed along with its sensitivity to model parameters. In each case, the final mass of the collapsed remnant is also determined and often found not to correspond to the location of the piston (typically the edge of the iron core), but to a ``mass cut`` farther out. This mass cut is sensitive not only to the explosion energy, but also to the presupernova structure, stellar mass, and the metallicity. Unless the explosion mechanism, for unknown reasons, provides a much larger characteristic energy in more massive stars, it appears likely that stars larger than about 30 M{sub {center_dot}} will experience considerable reimplosion of heavy elements following the initial launch of a successful shock. While such explosions will produce a viable, bright Type II supernova light curve, lacking the radioactive tail, they will have dramatically reduced yields of heavy elements and may leave black hole remnants of up to 10 and more solar masses.

Woosley, S.E. [California Univ., Santa Cruz, CA (United States); [Lawrence Livermore National Lab., CA (United States); Weaver, T.A. [Lawrence Livermore National Lab., CA (United States)

1995-08-30T23:59:59.000Z

278

Crazy heart: kinematics of the "star pile" in Abell 545  

E-Print Network [OSTI]

We study the structure and internal kinematics of the "star pile" in Abell 545 - a low surface brightness structure lying in the center of the cluster.We have obtained deep long-slit spectroscopy of the star pile using VLT/FORS2 and Gemini/GMOS, which is analyzed in conjunction with deep multiband CFHT/MEGACAM imaging. As presented in a previous study the star pile has a flat luminosity profile and its color is consistent with the outer parts of elliptical galaxies. Its velocity map is irregular, with parts being seemingly associated with an embedded nucleus, and others which have significant velocity offsets to the cluster systemic velocity with no clear kinematical connection to any of the surrounding galaxies. This would make the star pile a dynamically defined stellar intra-cluster component. The complicated pattern in velocity and velocity dispersions casts doubts on the adequacy of using the whole star pile as a dynamical test for the innermost dark matter profile of the cluster. This status is fulfille...

Salinas, Ricardo; West, Michael J; Romanowsky, Aaron J; Lloyd-Davies, Ed; Schuberth, Ylva

2011-01-01T23:59:59.000Z

279

ENERGY STAR EEPS Partnership Agreement  

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

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

280

Creating a Star on Earth  

Broader source: Energy.gov [DOE]

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

Note: This page contains sample records for the topic "difference star center" 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

Harmonizing Global Metrics for Data Center Energy Efficiency, February 2,  

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

Harmonizing Global Metrics for Data Center Energy Efficiency, Harmonizing Global Metrics for Data Center Energy Efficiency, February 2, 2010 Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In This Section Campaigns Commercial building design Communications resources Energy management guidance Financial resources Portfolio Manager Products and purchasing Recognition Research and reports Service and product provider (SPP) resources

282

Upsilon measurement in STAR  

E-Print Network [OSTI]

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

Mauro R. Cosentino

2007-06-06T23:59:59.000Z

283

Star Canticle Issue 2  

E-Print Network [OSTI]

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

Multiple Contributors

1979-01-01T23:59:59.000Z

284

Teacher Resource Center  

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

Teacher Resource Center: Putting It All Together Teacher Resource Center: Putting It All Together TRC Home TRC Fact Sheet Library Curricular Resources Science Fair Resources Bibliographies sciencelines The Best of sciencelines Archives Annotated List of URLs Catalog Teacher's Lounge Full Workshop Catalog Customized Workshops Scheduled Workshops Special Opportunities Teacher Networks Science Lab Fermilab Science Materials Samplers Order Form Science Safety Issues Tech Room Fermilab Web Resources The Teacher Resource Center provides a preview collection of K-12 instructional materials. TRC services include professional development workshops, consultation assistance, bibliographies and reference assistance. Educators have access to curriculum materials, books, multimedia, educational supply catalogs, periodicals and newsletters. The collection

285

Cost Update, STAR-TOFp Implementation STAR-TOFp Group  

E-Print Network [OSTI]

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

Llope, William J.

286

Fallback and Black Hole Production in Massive Stars  

SciTech Connect (OSTI)

The compact remnants of core collapse supernovae--neutron stars and black holes--have properties that reflect both the structure of their stellar progenitors and the physics of the explosion. In particular, the masses of these remnants are sensitive to the density structure of the presupernova star and to the explosion energy. To a considerable extent, the final mass is determined by the ''fallback'', during the explosion, of matter that initially moves outwards, yet ultimately fails to escape. We consider here the simulated explosion of a large number of massive stars (10 to 100 M{sub {circle_dot}}) of Population I (solar metallicity) and III (zero metallicity), and find systematic differences in the remnant mass distributions. As pointed out by Chevalier (1989), supernovae in more compact progenitor stars have stronger reverse shocks and experience more fallback. For Population III stars above about 25 M{sub {circle_dot}} and explosion energies less than 1.5 x 10{sup 51} erg, black holes are a common outcome, with masses that increase monotonically with increasing main sequence mass up to a maximum hole mass of about 35 M{sub {circle_dot}}. If such stars produce primary nitrogen, however, their black holes are systematically smaller. For modern supernovae with nearly solar metallicity, black hole production is much less frequent and the typical masses, which depend sensitively on explosion energy, are smaller. We explore the neutron star initial mass function for both populations and, for reasonable assumptions about the initial mass cut of the explosion, find good agreement with the average of observed masses of neutron stars in binaries. We also find evidence for a bimodal distribution of neutron star masses with a spike around 1.2 M{sub {circle_dot}} (gravitational mass) and a broader distribution peaked around 1.4 M{sub {circle_dot}}.

Zhang, Wei-Qun; /KIPAC, Menlo Park; Woosley, S.E.; /UC, Santa Cruz; Heger, A.; /UC, Santa Cruz /Los Alamos

2007-01-08T23:59:59.000Z

287

Data Center Economizer Contamination and Humidity Study  

SciTech Connect (OSTI)

Data centers require continuous air conditioning to address high internal heat loads (heat release from equipment) and maintain indoor temperatures within recommended operating levels for computers. Air economizer cycles, which bring in large amounts of outside air to cool internal loads when weather conditions are favorable, could save cooling energy. There is reluctance from many data center owners to use this common cooling technique, however, due to fear of introducing pollutants and potential loss of humidity control. Concerns about equipment failure from airborne pollutants lead to specifying as little outside air as permissible for human occupants. To investigate contamination levels, particle monitoring was conducted at 8 data centers in Northern California. Particle counters were placed at 3 to 4 different locations within and outside of each data center evaluated in this study. Humidity was also monitored at many of the sites to determine how economizers affect humidity control. Results from this study indicate that economizers do increase the outdoor concentration in data centers, but this concentration, when averaged annually, is still below current particle concentration limits. Study results are summarized below: (1) The average particle concentrations measured at each location, both outside and at the servers, are shown in Table 1. Measurements show low particle concentrations at all data centers without economizers, regardless of outdoor particle concentrations. Particle concentrations were typically an order of magnitude below both outside particle concentrations and recently published ASHRAE standards. (2) Economizer use caused sharp increases in particle concentrations when the economizer vents were open. The particle concentration in the data centers, however, quickly dropped back to pre-economizer levels when the vents closed. Since economizers only allow outside air part of the time, the annual average concentrations still met the ASHRAE standards. However, concentration were still above the levels measured in data centers that do not use economizers (3) Current filtration in data centers is minimal (ASHRAE 40%) since most air is typically recycled. When using economizers, modest improvements in filtration (ASHRAE 85%) can reduce particle concentrations to nearly match the level found in data centers that do not use economizers. The extra cost associated with improve filters was not determined in this study. (4) Humidity was consistent and within the ASHRAE recommended levels for all data centers without economizers. Results show that, while slightly less steady, humidity in data centers with economizers can also be controlled within the ASHRAE recommended levels. However, this control of humidity reduces energy savings by limiting the hours the economizer vents are open. (5) The potential energy savings from economizer use has been measured in one data center. When economizers were active, mechanical cooling power dropped by approximately 30%. Annual savings at this center is estimated within the range of 60-80 MWh/year, representing approximately a 5% savings off the mechanical energy load of the data center. Incoming temperatures and humidity at this data center were conservative relative to the ASHRAE acceptable temperature and humidity ranges. Greater savings may be available if higher temperature humidity levels in the data center area were permitted. The average particle concentrations measured at each of the eight data center locations are shown in Table 1. The data centers ranged in size from approximately 5,000 ft{sup 2} to 20,000 ft{sup 2}. The indoor concentrations and humidity in Table 1 represents measurements taken at the server rack. Temperature measurements at the server rack consistently fell between 65-70 F. The Findings section contains a discussion of the individual findings from each center. Data centers currently operate under very low contamination levels. Economizers can be expected to increase the particle concentration in data centers, but the increase appears to still be

Shehabi, Arman; Tschudi, William; Gadgil, Ashok

2007-03-06T23:59:59.000Z

288

Star Formation in Mergers and Interacting Galaxies: Gathering the Fuel  

E-Print Network [OSTI]

Selected results from recent studies of star formation in galaxies at different stages of interaction are reviewed. Recent results from the Spitzer Space Telescope are highlighted. Ideas on how large-scale driving of star formation in interacting galaxies might mesh with our understanding of star formation in isolated galaxies and small scale mechanisms within galaxies are considered. In particular, there is evidence that on small scales star formation is determined by the same thermal and turbulent processes in cool compressed clouds as in isolated galaxies. If so, this affirms the notion that the primary role of large-scale dynamics is to gather and compress the gas fuel. In gas-rich interactions this is generally done with increasing efficiency through the merger process.

Curtis Struck

2006-10-06T23:59:59.000Z

289

Quark Stars as inner engines for Gamma Ray Bursts?  

E-Print Network [OSTI]

A model for Gamma ray bursts inner engine based on quark stars (speculated to exist in nature) is presented. We describe how and why these objects might constitute new candidates for GRB inner engines. At the heart of the model is the onset of exotic phases of quark matter at the surface of such stars, in particular the 2-flavor color superconductivity. A novel feature of such a phase is the generation of particles which are unstable to photon decay providing a natural mechanism for a fireball generation; an approach which is fundamentally different from models where the fireball is generated during collapse or conversion of neutron star to quark star processes. The model is capable of reproducing crucial features of Gamma ray bursts, such as the episodic activity of the engine (multiple and random shell emission) and the two distinct categories of the bursts (two regimes are isolated in the model with \\sim 2 s and \\sim 81 s burst total duration).

R. Ouyed; F. Sannino

2001-03-01T23:59:59.000Z

290

Relativistic tidal properties of neutron stars  

E-Print Network [OSTI]

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

Thibault Damour; Alessandro Nagar

2009-05-30T23:59:59.000Z

291

Thermal radiation from magnetic neutron star surfaces  

E-Print Network [OSTI]

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

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

2004-10-27T23:59:59.000Z

292

Reconstructing the Star Formation Histories of Galaxies  

E-Print Network [OSTI]

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

Uta Fritze; Thomas Lilly

2007-01-15T23:59:59.000Z

293

Data Center Optimization Plan Federal Data Center Consolidation Initiative  

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

Data Center Optimization Plan Data Center Optimization Plan Federal Data Center Consolidation Initiative Public Release 9.30.11 U.S. Department of Energy | Office of the Chief Information Officer 2 Federal Data Center Consolidation Initiative Department of Energy Data Center Optimization Plan Public Release - 09.30.11 1. Introduction ..................................................................................................................................... 3 2. Agency Goals for Data Center Optimization .................................................................................... 5 3. Implementing Shared Services/Multi-tenancy ................................................................................. 5 4. Agency Approach, Rationale and Timeline ...................................................................................... 6

294

Neutron Science Center  

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

to have rare opportunity to tour Neutron Science Center May 10, 2011 LANL Rosenfest will celebrate life of LANSCE founder Louis Rosen and offer tour LOS ALAMOS, New Mexico, May 10,...

295

Energy efficient data centers  

E-Print Network [OSTI]

Center 6.2 utilized fan coil units, rather than computerEfficiency kW/ton Fan Coil Unit Design Efficiency CFM/kWCenter 6.2 utilized fan coil units, rather than computer

Tschudi, William; Xu, Tengfang; Sartor, Dale; Koomey, Jon; Nordman, Bruce; Sezgen, Osman

2004-01-01T23:59:59.000Z

296

ELIAS Towe, Center Director  

E-Print Network [OSTI]

the generation of hydrogen as a fuel for fuel cells, novel fuel cell technologies, and spectrally broadband photovoltaic cells for solar energy conversion. The secondary focus of the Center is on nano

Goldstein, Seth Copen

297

Data Center Power Consumption  

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

Center Power Consumption Center Power Consumption A new look at a growing problem Fact - Data center power density up 10x in the last 10 years 2.1 kW/rack (1992); 14 kW/rack (2007) Racks are not fully populated due to power/cooling constraints Fact - Increasing processor power Moore's law Fact - Energy cost going up 3 yr. energy cost equivalent to acquisition cost Fact - Iterative power life cycle Takes as much energy to cool computers as it takes to power them. Fact - Over-provisioning Most data centers are over-provisioned with cooling and still have hot spots November 2007 SubZero Engineering An Industry at the Crossroads Conflict between scaling IT demands and energy efficiency Server Efficiency is improving year after year Performance/Watt doubles every 2 years Power Density is Going Up

298

Stars and gas in the Medusa merger  

E-Print Network [OSTI]

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

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

2008-08-28T23:59:59.000Z

299

Women's Center INTERNAL COORDINATOR OREGON STATE UNIVERSITY PRIDE CENTER  

E-Print Network [OSTI]

at the Center for two or less years, in order to infuse the center with new ideas, energy and perspectives. 4

Escher, Christine

300

Proto-Neutron and Neutron Stars in a Chiral SU(3) Model  

E-Print Network [OSTI]

A hadronic chiral SU(3) model is applied to neutron and proto-neutron stars, taking into account trapped neutrinos, finite temperature and entropy. The transition to the chirally restored phase is studied and global properties of the stars like minimum and maximum masses and radii are calculated for different cases. In addition, the effects of rotation on neutron star masses are included and the conservation of baryon number and angular momentum determine the maximum frequencies of rotation during the cooling.

V. Dexheimer; S. Schramm

2008-02-14T23:59:59.000Z

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


301

Wind from T Tauri Stars  

Science Journals Connector (OSTI)

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

Masayoshi Kiguchi; Shinji Narita; Chushiro Hayashi

1998-12-01T23:59:59.000Z

302

Verifying the ENERGY STAR Certification Application  

Broader source: Energy.gov [DOE]

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

303

Christmas burst reveals neutron star collision  

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

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

304

University of Connecticut Health Center  

E-Print Network [OSTI]

University of Connecticut Health Center UCONN Medical Group Comprehensive Spine Center (Patient: ____________________ AGE: _____ SEX: M / F Referring Physician: ___________ Primary Care Physician: _____________ 1. Where your symptoms begin? __/__/__/ *HCH2199* #12;University of Connecticut Health Center UCONN Medical

Oliver, Douglas L.

305

ENERGY STAR Snapshot Spring 2012  

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

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

306

PNNL: News Center - Currents Newsletter  

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

help scientists design energy storage solutions and mitigate climate change. Read more. News Center News Center Home News Releases Social Media Directory PNNL Leadership Our...

307

Karen Nunez, Procedures Center Manager  

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

Karen Nunez, Procedures Center Manager Print Procedures Center Manager Karen Nunez has been working somewhat "behind the scenes" at the ALS for the past seven years, ensuring that...

308

Information Center | Department of Energy  

Office of Environmental Management (EM)

Center Information Center The U.S. Department of Energy's (DOE) Office of Enterprise Assessments (EA) provides expert evaluations of management performance in safety, security and...

309

NREL: Education Center Home Page  

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

Photo of the NREL Education Center. Clean Energy Innovation Programs for Student and Community Groups NREL's Education Center offers a variety of program topics and experiences for...

310

Sample ENERGY STAR performance documents | ENERGY STAR Buildings & Plants  

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

Existing buildings Existing buildings » Use Portfolio Manager » Verify and document your savings » Sample ENERGY STAR performance documents Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Learn the benefits Get started Use Portfolio Manager The new ENERGY STAR Portfolio Manager How Portfolio Manager helps you save The benchmarking starter kit

311

ENERGY STAR Focus on Energy Efficiency in Metalcasting | ENERGY STAR  

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

Metalcasting Metalcasting Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Get started with ENERGY STAR Make the business case Build an energy management program Measure, track, and benchmark Tools for benchmarking energy management practices Tools for tracking and benchmarking facility energy performance ENERGY STAR Energy Performance Indicators for plants

312

ENERGY STAR certification for your building | ENERGY STAR Buildings &  

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

certification for your building certification for your building Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Learn the benefits Get started Use Portfolio Manager Save energy Find financing Earn recognition 20-percent recognition ENERGY STAR certification How to apply for ENERGY STAR certification Tips for low-cost verifications Submit a profile of your building

313

ENERGY STAR Building Upgrade Manual | ENERGY STAR Buildings & Plants  

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

ENERGY STAR Building Upgrade Manual ENERGY STAR Building Upgrade Manual Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section Learn the benefits Get started Use Portfolio Manager Save energy Stamp out energy waste Find cost-effective investments Engage occupants Purchase energy-saving products Put computers to sleep Get help from an expert Take a comprehensive approach

314

Portfolio Manager Technical Reference: ENERGY STAR Score | ENERGY STAR  

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

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

315

The evolution of star clusters: The resolved-star approach  

E-Print Network [OSTI]

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

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

2008-02-29T23:59:59.000Z

316

THE DEPENDENCE OF STAR FORMATION EFFICIENCY ON GAS SURFACE DENSITY  

SciTech Connect (OSTI)

Studies by Lada et al. and Heiderman et al. have suggested that star formation mostly occurs above a threshold in gas surface density {Sigma} of {Sigma}{sub c} {approx} 120 M{sub Sun} pc{sup -2} (A{sub K} {approx} 0.8). Heiderman et al. infer a threshold by combining low-mass star-forming regions, which show a steep increase in the star formation rate per unit area {Sigma}{sub SFR} with increasing {Sigma}, and massive cores forming luminous stars which show a linear relation. We argue that these observations do not require a particular density threshold. The steep dependence of {Sigma}{sub SFR}, approaching unity at protostellar core densities, is a natural result of the increasing importance of self-gravity at high densities along with the corresponding decrease in evolutionary timescales. The linear behavior of {Sigma}{sub SFR} versus {Sigma} in massive cores is consistent with probing dense gas in gravitational collapse, forming stars at a characteristic free-fall timescale given by the use of a particular molecular tracer. The low-mass and high-mass regions show different correlations between gas surface density and the area A spanned at that density, with A {approx} {Sigma}{sup -3} for low-mass regions and A {approx} {Sigma}{sup -1} for the massive cores; this difference, along with the use of differing techniques to measure gas surface density and star formation, suggests that connecting the low-mass regions with massive cores is problematic. We show that the approximately linear relationship between dense gas mass and stellar mass used by Lada et al. similarly does not demand a particular threshold for star formation and requires continuing formation of dense gas. Our results are consistent with molecular clouds forming by galactic hydrodynamic flows with subsequent gravitational collapse.

Burkert, Andreas [University Observatory Munich, Scheinerstrasse 1, D-81679 Munich (Germany); Hartmann, Lee, E-mail: burkert@usm.lmu.de, E-mail: lhartm@umich.edu [Department of Astronomy, University of Michigan, 830 Dennison, 500 Church St., Ann Arbor, MI 48109-1042 (United States)

2013-08-10T23:59:59.000Z

317

The Brightest AGB Stars in the Inner Bulge of M31  

E-Print Network [OSTI]

JHK images with angular resolutions approaching the diffraction limit of the 3.6 meter Canada-France-Hawaii Telescope are used to investigate the bright AGB content of the M31 bulge. The AGB-tip in a field 2.6 arcmin from the galaxy center occurs at K = 15.6, which is significantly fainter than measured in previous ground-based studies that sampled similar projected distances from the center of M31. Within 2.6 arcmin of the center of M31 the number density of bright AGB stars scales with r-band surface brightness, and the K brightness of the AGB-tip does not vary measureably with radius. It is concluded that the infrared bright AGB stars (1) belong to the bulge, and not the disk, and (2) are well mixed throughout the inner bulge, suggesting that they formed at a time when the overall structural properties of the M31 bulge were imprinted. The bolometric luminosity functions of the M31 bulge and Baade's Window are in excellent agreement, while the brightest AGB stars in the M31 bulge, the Galactic bulge, and M32 have similar M_K. These data suggest that the brightest stars in M32 and the bulges of M31 and the Milky-Way belong to an old, metal-rich population; these stars are bright not because they have a young or intermediate age, but because they have a high metallicity.

T. J. Davidge

2001-06-23T23:59:59.000Z

318

Conference Center Lecture Hall  

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

401 Library Take the elevators downstairs to the Gallery. 401 Library Take the elevators downstairs to the Gallery. Conference Center Lecture Hall The Lecture Hall is a fully-equipped site for meetings of up to 540 people. This total includes: 237 seats on the Lecture Hall main level; 161 seats in the Lecture Hall balcony; and 142 seats in the two flexible rooms under the balcony (with interior walls removed). These rooms can also be used for meetings, both individually (32 classroom-style seats) or together (72 classroom-style seats). An additional 80 people can be seated in the nearby seminar room (A1100). Photo of the Conference Center's Lecture Hall Conference Center Gallery Seminar Room (A1101) The Seminar Room is located just off the Atrium. Conference Center Lecture Hall Atrium The Conference Center Atrium provides an open, elegant space ideal for registration, informational displays, and social hours. Computers are located just off the Atruim for e-mail access.

319

ARM - News Center  

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

Center Center Media Contact Lynne Roeder lynne-dot-roeder-at-pnnl-dot-gov @armnewsteam Field Notes Blog Topics Field Notes89 AGU 3 AMIE 10 ARM Aerial Facility 2 ARM Mobile Facility 1 6 ARM Mobile Facility 2 47 BAECC 1 BBOP 4 MAGIC 12 MC3E 17 SGP 2 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center All Categories Features and Releases Facility News Field Notes Blog feed Events feed Employment Research Highlights Data Announcements Education News Archive What's this? Social Media Guidance News Center Forecast Calls for Better Models: Examining the Core Components of Arctic Clouds to Clear Their Influence on Climate Jan 07, 2014 [ Research Highlights ] Predicting how atmospheric aerosols influence cloud formation and the resulting feedback to climate is a challenge that limits the accuracy of atmospheric models. This is especially true in the Arctic, where mixed-phase (both ice- and liquid-based) clouds are frequently observed, but the processes that determine their composition are poorly understood. To obtain a closer look [...]

320

The shortest modulation period Blazhko RR Lyrae star: SS Cnc  

E-Print Network [OSTI]

Extended BV(RI)c CCD observations of SS Cnc, a short period RRab star are presented. Nearly 1400 data points in each band have been obtained spanning over 79 days during the spring of 2005. The star exhibits light curve modulation, the so called Blazhko effect with small amplitude (B maximum brightness varies 0.1 mag) and with the shortest modulation period (5.309 d) ever observed. In the Fourier spectrum of the V light curve the pulsation frequency components are detected up to the 24th harmonic order, and modulation side lobe frequencies with significantly asymmetric amplitudes are seen up to the 15th and 9th orders for the lower and higher frequency components, respectively. Detailed comparison of the modulation behavior of SS Cnc and RR Gem, the two recently discovered small amplitude, short modulation period Blazhko stars is presented. The modulation frequency (f_m) appears in the Fourier spectrum of both stars with similar amplitude. We also demonstrate that the modulation frequencies have basically different properties as the pulsation and modulation side lobe frequencies have, indicating that the physics behind these frequency components are not the same. The discovery of small amplitude modulations of RRab stars cautions that the large photometric surveys (MACHO, OGLE) may seriously underestimate the number of modulated RR Lyrae stars.

J. Jurcsik; B. Szeidl; . Sdor; I. Dkny; Zs. Hurta; K. Posztobnyi; K. Vida; M. Vradi; A. Szing

2006-03-20T23:59:59.000Z

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


321

Evolution of 3D Boson Stars with Waveform Extraction  

E-Print Network [OSTI]

Numerical results from a study of boson stars under nonspherical perturbations using a fully general relativistic 3D code are presented together with the analysis of emitted gravitational radiation. We have constructed a simulation code suitable for the study of scalar fields in space-times of general symmetry by bringing together components for addressing the initial value problem, the full evolution system and the detection and analysis of gravitational waves. Within a series of numerical simulations, we explicitly extract the Zerilli and Newman-Penrose scalar $\\Psi_4$ gravitational waveforms when the stars are subjected to different types of perturbations. Boson star systems have rapidly decaying nonradial quasinormal modes and thus the complete gravitational waveform could be extracted for all configurations studied. The gravitational waves emitted from stable, critical, and unstable boson star configurations are analyzed and the numerically observed quasinormal mode frequencies are compared with known linear perturbation results. The superposition of the high frequency nonspherical modes on the lower frequency spherical modes was observed in the metric oscillations when perturbations with radial and nonradial components were applied. The collapse of unstable boson stars to black holes was simulated. The apparent horizons were observed to be slightly nonspherical when initially detected and became spherical as the system evolved. The application of nonradial perturbations proportional to spherical harmonics is observed not to affect the collapse time. An unstable star subjected to a large perturbation was observed to migrate to a stable configuration.

Jayashree Balakrishna; Ruxandra Bondarescu; Gregory Daues; F. Siddhartha Guzman; Edward Seidel

2006-02-20T23:59:59.000Z

322

National Training Center | Department of Energy  

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

Organizational Chart National Training Center National Training Center MISSION The National Training Center (NTC), the Department's Center of Excellence for Security and Safety...

323

Laboratory Computing Resource Center  

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

Computing DOE Logo Computing DOE Logo Search BIO ... Search Argonne Home > BIO home > Laboratory Computing Resource Center BIO Home Page About BIO News Releases Research Publications People Contact Us Organization Chart Site Index Inside BIO BIO Safety About Argonne Argonne National Laboratory Logo Laboratory Computing Resource Center In 2002 Argonne National Laboratory established the Laboratory Computing Project to enable and promote the use of high-performance computing (HPC) across the Laboratory in support of its varied research missions. The Laboratory Computing Resource Center (LCRC) was established, and in April 2003 LCRC began full operations with Argonne’s first teraflops computing cluster, Jazz. In 2010 Jazz was replaced by Fusion, with a peak performance of 30 teraflops (and still growing). We just acquired Blues which will a performance of 100 teraflops.

324

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Carolina Incentives and Laws Carolina Incentives and Laws The following is a list of expired, repealed, and archived incentives, laws, regulations, funding opportunities, or other initiatives related to alternative fuels and vehicles, advanced technologies, or air quality. Biofuels Commercialization Grants Archived: 10/01/2013 The Biofuels Center of North Carolina (Center) is a private, nonprofit corporation the Legislature funds to implement the goal that by 2017, 10% of liquid fuels sold in North Carolina will come from biofuels grown and produced within the state. The Center awards funds to academic institutions, economic development organizations, nonprofit corporations, and other entities through an annual competitive awards process. Grants and contracts are designed to identify and bridge gaps in knowledge and

325

UV Star Formation Rates in the Local Universe  

E-Print Network [OSTI]

We measure star formation rates of ~50,000 optically-selected galaxies in the local universe (z~0.1), spanning a range from gas-rich dwarfs to massive ellipticals. We obtain dust-corrected SFRs by fitting the GALEX (UV) and SDSS (optical) photometry to a library of population synthesis models that include dust attenuation. For star-forming galaxies, our UV-based SFRs compare remarkably well with those derived from SDSS H alpha. Deviations from perfect agreement between these two methods are due to differences in the dust attenuation estimates. In contrast to H alpha, UV provides reliable SFRs for galaxies with weak or no H alpha emission, and where H alpha is contaminated with an emission from an AGN. We use full-SED SFRs to calibrate a simple prescription that uses GALEX UV magnitudes to produce good SFRs for normal star-forming galaxies. The specific SFR is considered as a function of stellar mass for (1) star-forming galaxies with no AGN, (2) those hosting an AGN, and for (3) galaxies without H alpha emission. We find that the three have distinct star formation histories, with AGN lying intermediate between the star-forming and the quiescent galaxies. Normal star forming galaxies (without an AGN) lie on a relatively narrow linear sequence. Remarkably, galaxies hosting a strong AGN appear to represent the massive continuation of this sequence. Weak AGN, while also massive, have lower SFR, sometimes extending to the realm of quiescent galaxies. We propose an evolutionary sequence for massive galaxies that smoothly connects normal star-forming galaxies to quiescent (red sequence) galaxies via strong and weak AGN. We confirm that some galaxies with no H alpha emission show signs of SF in the UV. We derive a UV-based cosmic SFR density at z=0.1 with smaller total error than previous measurements (abridged).

Samir Salim; R. Michael Rich; Stphane Charlot; Jarle Brinchmann; Benjamin D. Johnson; David Schiminovich; Mark Seibert; Ryan Mallery; Timothy M. Heckman; Karl Forster; Peter G. Friedman; D. Christopher Martin; Patrick Morrissey; Susan G. Neff; Todd Small; Ted K. Wyder; Luciana Bianchi; Jose Donas; Young-Wook Lee; Barry F. Madore; Bruno Milliard; Alex S. Szalay; Barry Y. Welsh; Sukyoung K. Yi

2007-05-07T23:59:59.000Z

326

ENERGY STAR Webinar: Financing Energy Efficient Upgrades with ENERGY STAR  

Broader source: Energy.gov [DOE]

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

327

EPA ENERGY STAR Webinar: ENERGY STAR Portfolio Manager 201  

Broader source: Energy.gov [DOE]

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

328

EPA ENERGY STAR Webcast: Value of ENERGY STAR Certification  

Office of Energy Efficiency and Renewable Energy (EERE)

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

329

ENERGY STAR Challenge for Industry  

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

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

330

Energy Star Lighting Verification Program (Program for the Evaluation and Analysis of Residential Lighting)  

SciTech Connect (OSTI)

The Program for the Evaluation and Analysis of Residential Lighting (PEARL) is a watchdog program. It was created in response to complaints received by utility program managers about the performance of certain Energy Star lighting products being promoted within their service territories and the lack of a self-policing mechanism within the lighting industry that would ensure the reliability of these products and their compliance with ENERGY STAR specifications. To remedy these problems, PEARL purchases and tests products that are available to the consumers in the marketplace. The Lighting Research Center (LRC) tests the selected products against the corresponding Energy Star specifications. This final report summarizes the experimental procedure and results of all cycles (Cycles 1 through 8) of PEARL program from the beginning of year 2000 to the end of 2007, along with the description of apparatus used, equipment calibration process, experimental methodology, and research findings from the testing. In each cycle of PEARL program, PEARL Board selects a list of Compact Fluorescent Lamp (CFL) and Residential Lighting Fixture (RLF) models that are Energy Star qualified. In Cycle 5, Cycle 7, and Cycle 8, no fixture models were selected. After that PEARL sponsors procure product samples for each selected model from different stores and locations in the retail market and send them to LRC for testing. LRC then receive and select the samples, and test them against Energy Star specifications. After the testing LRC analyze and report the results to PEARL Board. Totally 185 models of CFL and 52 models of RLF were tested in PEARL program. Along with the evolution of the Energy Star specifications from year 2000 to 2003, parameters that were required by Energy Star changed during the eight years of PEARL program. The testing parameters and number of samples tested in PEARL program also changed during this time. For example, in Cycle 1, three samples of each models were tested for their photometric and electrical parameters only; in Cycle 2, 1000-hour Lumen Maintenance and the Rapid Cycle Stress Test was added and an additional set of six samples of each models were tested for Rapid Cycle Stress Test. Also, Cycle 2 data analysis included the testing and verification results against both the 'then existing' specification dated 2000 and the 'then new' specification dated 8/9/2001. In Cycle 3, Lumen Maintenance at 40% life was added and the number of samples for photometric and electrical testing was increased to five. In Cycle 6, the number of samples for photometric and electrical testing increased again to ten so that five of them were tested in base-up position and five in base-down position. A total of 2375 CFL samples were tested in PEARL program, out of the more than 3000 CFL samples that were purchased for the testing purpose of this program.

Conan O'Rourke; Yutao Zhou

2007-12-31T23:59:59.000Z

331

Impact of Continuous Commissioning on the Energy Star Rating of Hospitals and Office Buildings  

E-Print Network [OSTI]

source EUI of an office type facility ............................................................................................ 23 Table 4: Linear regression equation for calculating the predicted source EUI of a hospital type facility... of Building Centered Variables................................................ 61 Table 10: Calculation of predicted source EUI ................................................................ 62 Table 11: Lookup table for Energy Star? Rating given...

Kulkarni, Aditya Arun

2012-02-14T23:59:59.000Z

332

PAHs and crystalline silicates in the bipolar post-AGB star IRAS 16279-4757 12  

E-Print Network [OSTI]

understood. A possibility, but implausible, is that these stars all evolved from oxygen-rich to carbon with PAHs and crystalline silicates. A two-component model and images suggest a dense oxygen-rich torus at the outflow, while the continuum emission is concentrat- ed towards the center. Our findings support

Zijlstra, Albert

333

FPL's solar stars shine at new 500-acre array By SUSAN SALISBURY  

E-Print Network [OSTI]

FPL's solar stars shine at new 500-acre array By SUSAN SALISBURY Palm Beach Post Staff Writer and water, Florida Power & Light Co. workers finished cleaning the mirrors at its new Martin County solar's dedication of the one-of-a-kind hybrid solar energy center, it's nice that the 5-by-5-foot mirrors

Belogay, Eugene A.

334

DOE Withdraws the Energy Star Label from 34 Compact Fluorescent Light Bulbs  

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

the Energy Star Label from 34 Compact Fluorescent the Energy Star Label from 34 Compact Fluorescent Light Bulbs DOE Withdraws the Energy Star Label from 34 Compact Fluorescent Light Bulbs January 26, 2010 - 11:41am Addthis Washington, DC - On January 25th, the General Counsel notified 25 manufacturers that the Department of Energy has withdrawn their right to use the Energy Star label on 34 different models of compact fluorescent light bulbs (CFLs). The Department took this action after its off-the-shelf testing revealed that the affected models do not last as long in regular use as Energy Star certification would require. As a result, these manufacturers have been informed that they can no longer ship or sell any of the 34 models of CFLs bearing the Energy Star label on the bulb or its packaging. All compact fluorescent light bulbs use about 75 percent less energy and

335

A Heavy Flavor Tracker for STAR  

SciTech Connect (OSTI)

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

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

2005-03-14T23:59:59.000Z

336

Thermal evolution of neutron stars with global and local neutrality  

E-Print Network [OSTI]

Globally neutral neutron stars, obtained from the solution of the called Einstein-Maxwell-Thomas-Fermi equations that account for all the fundamental interactions, have been recently introduced. These configurations have a more general character than the ones obtained with the traditional Tolman-Oppenheimer-Volkoff, which impose the condition of local charge neutrality. The resulting configurations have a less massive and thinner crust, leading to a new mass-radius relation. Signatures of this new structure of the neutron star on the thermal evolution might be a potential test for this theory. We compute the cooling curves by integrating numerically the energy balance and transport equations in general relativity, for globally neutral neutron stars with crusts of different masses and sizes, according to this theory for different core-crust transition interfaces. We compare and contrast our study with known results for local charge neutrality. We found a new behavior for the relaxation time, depending upon the...

de Carvalho, S M; Rueda, Jorge A; Ruffini, Remo

2014-01-01T23:59:59.000Z

337

Energy Frontier Research Centers | ORNL  

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

Materials Synthesis from Atoms to Systems Materials Synthesis from Atoms to Systems Materials Characterization Materials Theory and Simulation Energy Frontier Research Centers Center for Defect Physics in Structural Materials Fluid Interface Reactions, Structure and Transport Advanced Materials Home | Science & Discovery | Advanced Materials | Research Areas | Energy Frontier Research Centers SHARE Energy Frontier Research Centers Advanced Materials research at ORNL is home to two Department of Energy-Office of Basic Energy Sciences' Energy Frontier Research Centers, the Fluid Interface Reaction, Structure, and Transport Center (FIRST), which focuses on understanding interfacial processes critical to electrical energy storage and catalysis, and the Center for Defect Physics, (CDP)

338

Alternative Fuels Data Center: Publications  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Publications Publications Printable Version Share this resource Send a link to Alternative Fuels Data Center: Publications to someone by E-mail Share Alternative Fuels Data Center: Publications on Facebook Tweet about Alternative Fuels Data Center: Publications on Twitter Bookmark Alternative Fuels Data Center: Publications on Google Bookmark Alternative Fuels Data Center: Publications on Delicious Rank Alternative Fuels Data Center: Publications on Digg Find More places to share Alternative Fuels Data Center: Publications on AddThis.com... Publications Find publications about alternative transportation, including alternative fuels, advanced vehicles, and regulated fleets. Keyword Category Search more search options close × Filter by Document Category Books & Chapters Brochures & Fact Sheets Conference Papers & Proceedings

339

Alternative Fuels Data Center: Newsletters  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Publications » Newsletters Publications » Newsletters Printable Version Share this resource Send a link to Alternative Fuels Data Center: Newsletters to someone by E-mail Share Alternative Fuels Data Center: Newsletters on Facebook Tweet about Alternative Fuels Data Center: Newsletters on Twitter Bookmark Alternative Fuels Data Center: Newsletters on Google Bookmark Alternative Fuels Data Center: Newsletters on Delicious Rank Alternative Fuels Data Center: Newsletters on Digg Find More places to share Alternative Fuels Data Center: Newsletters on AddThis.com... Newsletters Read these government and industry newsletters to stay current with developments in alternative transportation technologies, including alternative fuels, advanced vehicles, and regulated fleets. Government Newsletters

340

Alternative Fuels Data Center: Publications  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Publications Publications Printable Version Share this resource Send a link to Alternative Fuels Data Center: Publications to someone by E-mail Share Alternative Fuels Data Center: Publications on Facebook Tweet about Alternative Fuels Data Center: Publications on Twitter Bookmark Alternative Fuels Data Center: Publications on Google Bookmark Alternative Fuels Data Center: Publications on Delicious Rank Alternative Fuels Data Center: Publications on Digg Find More places to share Alternative Fuels Data Center: Publications on AddThis.com... Publications Find publications about alternative transportation, including alternative fuels, advanced vehicles, and regulated fleets. Keyword Category alternative fuel price report Search more search options close × Filter by Document Category

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


341

Energy Efficient Data Centers  

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

Federal Utility Partnership Working Group Will Lintner November 28, 2007 San Diego, CA Why Data Centers? * Data centers are highly energy intensive and growing at a rapid rate - Consume 10 to 100 times more energy per square foot than typical office building * Data centers consumed about 45 billion kWh in 2005 and 61 billion kWh in 2006 - This accounts for nearly 1.2% and 1.5% of all U.S. electricity respectively * At current rate, power requirements for data centers could double in 5 years 2 Opportunity Potential Comparison of Projected Electricity Use - All Scenarios 2007 to 2011 140 2006 Baseline 58.7 Annual Energy Use (Billion kWh/year) 120 100 80 60 40 20 B u s i n e s s a s u s u a l C u r r e n t t r e n d s I m p r o v e d o p e r a t i o n a l m a n a g e m e n t Best practice S ta te o f th e a rt 0 2007 2008 2009 2010 2011

342

Arkansas Water Resources Center  

E-Print Network [OSTI]

Keywords --Algal Assay/Nutrients/Heavy Metals/Toxicity #12;TABLE OF CONTENTS Page Abstract. i ListArkansas Water Resources Center ALGAL GROWTH POTENTIALS AND HEAVY METAL CONCENTRATIONS) demonstrated the probable inhibition of algal growth potential by heavy metals in upper Beaver Lake. Upper

Soerens, Thomas

343

Patrick Scheuermann Center Director  

E-Print Network [OSTI]

propulsion test facilities; and ensured Stennis continued to serve as the systems engineering center at Stennis for NASA's Reusable Launch Vehicle program, a NASA-industry effort to develop a new generation of rockets to safely and cost-effectively send payloads to space. He also served as project manager

344

National Energy Software Center  

SciTech Connect (OSTI)

A short introduction is given to the services of the National Energy Software Library at the Argonne National Laboratory. The objectives, history, and software collection of the center are presented. Information on ordering from the software collection of the library is also included. 4 refs., 3 tabs. (DWL)

Eyberger, L.R.

1986-01-01T23:59:59.000Z

345

Arkansas Water Resources Center  

E-Print Network [OSTI]

. Geographical Information System (GIS) Support. The Center for Advanced Spatial Technology (CAST) and the GIS Laboratory in the Department of Crop, Soil, and Environmental Sciences provide support in developing GIS data the viability of alternate water supplies using abandoned, flooded coal mines for the City of Greenwood

Soerens, Thomas

346

HEEP CENTER Building # 1502  

E-Print Network [OSTI]

1 HEEP CENTER Building # 1502 EMERGENCY EVACUATION PLAN Prepared by: Harry Cralle and Mark Wright a building. Examples of such occasions include: smoke/fire, gas leak, bomb threat. Pre-planning and rehearsal are effective ways to ensure that building occupants recognize the evacuation alarm and know how to respond

Tomberlin, Jeff

347

Infrastructure Assurance Center  

E-Print Network [OSTI]

, the United States relied on natural gas to meet about 22% of its energy needs. Therefore, assuring efficient, natural gas processing plants, and other industrial customers, along with the changes in the utilizationInfrastructure Assurance Center NGReal-time: processing and analysis tool for natural gas delivery

348

Precision Joining Center  

SciTech Connect (OSTI)

A workshop to obtain input from industry on the establishment of the Precision Joining Center (PJC) was held on July 10--12, 1991. The PJC is a center for training Joining Technologists in advanced joining techniques and concepts in order to promote the competitiveness of US industry. The center will be established as part of the DOE Defense Programs Technology Commercialization Initiative, and operated by EG G Rocky Flats in cooperation with the American Welding Society and the Colorado School of Mines Center for Welding and Joining Research. The overall objectives of the workshop were to validate the need for a Joining Technologists to fill the gap between the welding operator and the welding engineer, and to assure that the PJC will train individuals to satisfy that need. The consensus of the workshop participants was that the Joining Technologist is a necessary position in industry, and is currently used, with some variation, by many companies. It was agreed that the PJC core curriculum, as presented, would produce a Joining Technologist of value to industries that use precision joining techniques. The advantage of the PJC would be to train the Joining Technologist much more quickly and more completely. The proposed emphasis of the PJC curriculum on equipment intensive and hands-on training was judged to be essential.

Powell, J.W.; Westphal, D.A.

1991-08-01T23:59:59.000Z

349

RETIREMENT CENTER MISSION STATEMENT  

E-Print Network [OSTI]

timely and informative LIR programs: "What's Happening with Health Care Reform;" "The 2012 Presidential, curiosity, and their continuing care and contributions to their families, their university Caregiver Support: See p. 3 to learn more about the Center's collaborative effort with the UCB Elder Care

Alvarez-Cohen, Lisa

350

ENERGY STAR Challenge for Industry  

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

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

351

Appendix 5 - STARS Architectual Overview  

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

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

352

Neutron skins and neutron stars  

Science Journals Connector (OSTI)

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

F. J. Fattoyev and J. Piekarewicz

2012-07-05T23:59:59.000Z

353

ENERGY STAR Portfolio Manager 101  

Office of Energy Efficiency and Renewable Energy (EERE)

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

354

ENERGY STAR Portfolio Manager 201  

Office of Energy Efficiency and Renewable Energy (EERE)

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

355

Inversion of the star transform  

E-Print Network [OSTI]

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

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

2014-05-06T23:59:59.000Z

356

Shooting Star | Open Energy Information  

Open Energy Info (EERE)

Shooting Star Shooting Star Jump to: navigation, search Name Shooting Star Facility Shooting Star Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner Exelon Wind Developer Infinity Wind Power Energy Purchaser Sunflower Electric Power Corporation Location Greensburg KS Coordinates 37.55019151°, -99.27585125° Loading map... {"minzoom":false,"mappingservice":"googlemaps3","type":"ROADMAP","zoom":14,"types":["ROADMAP","SATELLITE","HYBRID","TERRAIN"],"geoservice":"google","maxzoom":false,"width":"600px","height":"350px","centre":false,"title":"","label":"","icon":"","visitedicon":"","lines":[],"polygons":[],"circles":[],"rectangles":[],"copycoords":false,"static":false,"wmsoverlay":"","layers":[],"controls":["pan","zoom","type","scale","streetview"],"zoomstyle":"DEFAULT","typestyle":"DEFAULT","autoinfowindows":false,"kml":[],"gkml":[],"fusiontables":[],"resizable":false,"tilt":0,"kmlrezoom":false,"poi":true,"imageoverlays":[],"markercluster":false,"searchmarkers":"","locations":[{"text":"","title":"","link":null,"lat":37.55019151,"lon":-99.27585125,"alt":0,"address":"","icon":"","group":"","inlineLabel":"","visitedicon":""}]}

357

ENERGY STAR Success Story Mark Twain House Museum  

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

ENERGY STAR Success Story: ENERGY STAR Success Story: Mark Twain House & Museum Built in 1874, the Mark Twain House & Museum is considered one of the premier tourist attractions in the State of Connecticut. This 19-room Victorian home changed owners numerous times before the Mark Twain Memorial and Library Commission, a non-profit organization chartered by the State of Connecticut, purchased and restored the house in 1929 for historical and educational purposes. The Museum comprises the 12,298-square-foot Main House (the historic house of Mark Twain) and the 4,935-square- foot Carriage House (the location of all staff offices). The state-of-the-art 33,000-square-foot Museum Center was added in 2003, thrusting the Mark Twain House & Museum into the 21 st Century. The Main

358

Buildings Energy Data Book: 9.1 ENERGY STAR  

Buildings Energy Data Book [EERE]

3 3 ENERGY STAR Commercial and Institutional Buildings and Industrial Plants (1) Building Type 1999 Office 2000 K-12 School 2001 Retail 2002 Hospital (General and Surgical) 2003 Supermarket/Grocery 2004 Hotel 2005 Bank/Financial Institution 2006 Warehouse (Unrefrigerated) 2007 Courthouse 2008 Medical Office 2009 Residence Hall/Dormitory 2010 Senior Care Facility 2011 Data Center Total (2) Warehouse (Refrigerated) House of Worship Industrial Plants Total Note(s): Source(s): 1) Data as of February 13, 2012. Additional buildings may qualify after applications are reviewed. 2) Totals are less than sum of individual years since some buildings have multiple years listed. Totals include buildings qualified in 2012. EPA, Database of ENERGY STAR Labeled Buildings and Plants, accessed February 13, 2012

359

STAR Vertex Detector Upgrade Development  

SciTech Connect (OSTI)

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

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

2008-01-28T23:59:59.000Z

360

GRBs from the First Stars  

SciTech Connect (OSTI)

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

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

2007-04-16T23:59:59.000Z

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


361

Magnesium Isotopes in Halo Stars  

E-Print Network [OSTI]

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

Jorge Melendez; Judith G. Cohen

2007-08-29T23:59:59.000Z

362

Possible dark energy imprints in gravitational wave spectrum of mixed neutron-dark-energy stars  

E-Print Network [OSTI]

In the present paper we study the oscillation spectrum of neutron stars containing both ordinary matter and dark energy in different proportions. Within the model we consider, the equilibrium configurations are numerically constructed and the results show that the properties of the mixed neuron-dark-energy star can differ significantly when the amount of dark energy in the stars is varied. The oscillations of the mixed neuron-dark-energy stars are studied in the Cowling approximation. As a result we find that the frequencies of the fundamental mode and the higher overtones are strongly affected by the dark energy content. This can be used in the future to detect the presence of dark energy in the neutron stars and to constrain the dark-energy models.

Stoytcho S. Yazadjiev; Daniela D. Doneva

2011-12-19T23:59:59.000Z

363

ENERGY STAR Back-To-School Shopping Checklist  

E-Print Network [OSTI]

ENERGY STAR® Back-To-School Shopping Checklist Students can make a difference by shopping "smart" with ENERGY STAR® . Computing the Savings ENERGY STAR Qualified Computer Equipment Computer Monitor ENERGY up to 90 percent more energy than standard monitors. Printer If every home office were powered

364

Electron Microscopy Center  

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

Acknowledgment Acknowledgment EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Becoming a User Submit a Proposal End-of-Proposal Report Acknowledgment User Training User Safety User Status Instrument Access User Committee User Meetings Data Storage Policy Visiting the EMC Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers Acknowledgment Please acknowledge your use of the EMC in your publications and presentations with the following acknowledgment statement: The electron microscopy was accomplished at the Electron Microscopy Center at Argonne National Laboratory, a U.S. Department of Energy Office of Science Laboratory operated under Contract No. DE-AC02-06CH11357 by UChicago Argonne, LLC.

365

LHC Physics Center | (none)  

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

Physics Center Physics Center Fermilab Home Visit LPC Physics Programs LPC Guest and Visitors HATS@LPC, Workshops and CMSDAS Jet-Substructure HATS CMS Data Analysis School 2013 CMS Data Analysis School 2012 CMS Data Analysis School 2011 EJTERM (CMS Data Analysis School 2010) Confronting Theory with Experiment: November 2011 Standard Model Benchmarks at the Tevatron and LHC Standard Model Benchmarks at High-Energy Hadron Colliders GED workshop 20-22 Aug, 2012 Topic of the Week Upcoming Past Speakers Archive Program Info LPC Physics Forum LPC Snowmass Efforts The INFIERI Project Fellows LPC Fellows Program Newsletter - LPC Fellows LPC Fellows - 2014 LPC Fellows - 2013 LPC Fellows - 2012 LPC Fellows - 2011 Community Faces of the LPC LPC Fellows - Current LPC Coffee Hour Calendar LPC Conf. Room Calendar

366

Aperture center energy showcase  

SciTech Connect (OSTI)

Sandia and Forest City have established a Cooperative Research and Development Agreement (CRADA), and the partnership provides a unique opportunity to take technology research and development from demonstration to application in a sustainable community. A project under that CRADA, Aperture Center Energy Showcase, offers a means to develop exhibits and demonstrations that present feedback to community members, Sandia customers, and visitors. The technologies included in the showcase focus on renewable energy and its efficiency, and resilience. These technologies are generally scalable, and provide secure, efficient solutions to energy production, delivery, and usage. In addition to establishing an Energy Showcase, support offices and conference capabilities that facilitate research, collaboration, and demonstration were created. The Aperture Center project focuses on establishing a location that provides outreach, awareness, and demonstration of research findings, emerging technologies, and project developments to Sandia customers, visitors, and Mesa del Sol community members.

Torres, J. J.

2012-03-01T23:59:59.000Z

367

PIA - I-Manage STARS | Department of Energy  

Energy Savers [EERE]

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

368

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

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

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

369

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

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

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

370

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

Energy Savers [EERE]

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

371

Doyle Conservation Center (DCC)  

High Performance Buildings Database

Leominster, MA Built on a 50-acre reservation in Leominster, the Doyle Conservation Center (DCC) houses core Trustees staff and serves as a central training facility that showcases the organization's conservation activities. The DCC's LEED Gold rating reflects the mission of the Trustees of Reservations, which is "To preserve, for public use and enjoyment, properties of exceptional scenic, historic, and ecological value in Massachusetts." The DCC is accessible to the public and is often rented out by various groups and organizations.

372

Honda Transmission Technical Center  

High Performance Buildings Database

Russells Point, OH The Honda Transmission Technical Center is located on the Honda of America Manufacturing Plant facility site in Russells Point, Ohio. This facility is used for product engineering and market quality testing and analysis of automatic transmissions. The building contains a large workshop area for ten cars, a future dynamometer, two laboratories, an open office area, three conference rooms, a break room, restrooms, and related support areas.

373

Industrial Assessment Centers (IACs)  

Broader source: Energy.gov [DOE]

Small- and medium-sized manufacturers may be eligible to receive a no-cost assessment provided by DOE Industrial Assessment Centers (IACs). Teams located at 24 universities around the country conduct the energy audits to identify opportunities to improve productivity, reduce waste, and save energy. Each manufacturer typically identifies about $55,000 in potential annual savings on average. Over 15,000 IAC assessments have been conducted. IACs also train the next-generation of energy savvy engineers.

374

Wave Star Energy | Open Energy Information  

Open Energy Info (EERE)

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

375

Electron Microscopy Center  

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

Laboratory Laboratory Electron Microscopy Center Argonne Home > EMC > EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers An Office of Science User Facility The Electron Microscopy Center (EMC) at Argonne National Laboratory develops and maintains unique capabilities for electron beam characterization and applies those capabilities to solve materials problems. The EMC staff carry out research with collaborators and users from Argonne, universities, and other laboratories. The expertise and facilities of the EMC additionally serve a group of national and international researchers. The EMC emphasizes three major areas: materials research, technique and instrumentation development, and operation as a national research facility. Research by EMC personnel includes microscopy based studies in high Tc superconducting materials, irradiation effects in metals and semiconductors, phase transformations, and processing related structure and chemistry of interfaces in thin films.

376

About CRSP Management Center  

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

CRSP Act Power Projects Contact CRSP Customers Environmental Review-NEPA Financial Data Operations Planning & Projects Power Marketing Rates CRSP Act Power Projects Contact CRSP Customers Environmental Review-NEPA Financial Data Operations Planning & Projects Power Marketing Rates About Colorado River Storage Project Management Center CRSP Management Center Office The Ak-Chin Indian Community in Arizona, the city of Aspen, Colo., and Kirtland Air Force Base in New Mexico are a few of the vital customers of the Colorado River Storage Project's Management Center. We assist customers in saving their valuable electrical resources by actively promoting energy management and conservation programs and helping them determine their future energy needs. When customers want new products and services tailored to their individual needs, we explore their ideas. We are also committed to protecting the delicate balance of the Colorado River and its tributaries. Agencies that manage this river's resources must weigh its many roles: irrigation, recreation, hydropower and native and non-native endangered species habitat protection. Balancing these resources with the needs of water and electrical energy customers is a chief concern.

377

WIDE-FIELD SURVEY OF EMISSION-LINE STARS IN IC 1396  

SciTech Connect (OSTI)

We have made an extensive survey of emission-line stars in the IC 1396 H II region to investigate the low-mass population of pre-main-sequence (PMS) stars. A total of 639 H{alpha} emission-line stars were detected in an area of 4.2 deg{sup 2} and their i' photometry was measured. Their spatial distribution exhibits several aggregates near the elephant trunk globule (Rim A) and bright-rimmed clouds at the edge of the H II region (Rim B and SFO 37, 38, 39, 41), and near HD 206267, which is the main exciting star of the H II region. Based on the extinction estimated from the near-infrared color-color diagram, we have selected PMS star candidates associated with IC 1396. The age and mass were derived from the extinction-corrected color-magnitude diagram and theoretical PMS tracks. Most of our PMS candidates have ages of <3 Myr and masses of 0.2-0.6 M{sub Sun }. Although it appears that only a few stars were formed in the last 1 Myr in the east region of the exciting star, the age difference among subregions in our surveyed area is not clear from the statistical test. Our results may suggest that massive stars were born after the continuous formation of low-mass stars for 10 Myr. The birth of the exciting star could be the late stage of slow but contiguous star formation in the natal molecular cloud. It may have triggered the formation of many low-mass stars at the dense inhomogeneity in and around the H II region by a radiation-driven implosion.

Nakano, M. [Faculty of Education and Welfare Science, Oita University, Oita 870-1192 (Japan); Sugitani, K. [Graduate School of Natural Sciences, Nagoya City University, Mizuho-ku, Nagoya 467-8501 (Japan); Watanabe, M. [Department of Cosmosciences, Hokkaido University, Sapporo 060-0810 (Japan); Fukuda, N. [Department of Computer Simulation, Okayama University of Science, 1-1 Ridai-cho, Okayama 700-0005 (Japan); Ishihara, D. [Department of Physics, Nagoya University, Furo-cho, Chikusa-ku, Nagoya 464-8602 (Japan); Ueno, M., E-mail: mnakano@oita-u.ac.jp [Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshino-dai, Chuo-ku, Sagamihara 252-5210 (Japan)

2012-03-15T23:59:59.000Z

378

THE ESTIMATION OF STAR FORMATION RATES AND STELLAR POPULATION AGES OF HIGH-REDSHIFT GALAXIES FROM BROADBAND PHOTOMETRY  

SciTech Connect (OSTI)

We explore methods to improve the estimates of star formation rates and mean stellar population ages from broadband photometry of high-redshift star-forming galaxies. We use synthetic spectral templates with a variety of simple parametric star formation histories to fit broadband spectral energy distributions. These parametric models are used to infer ages, star formation rates, and stellar masses for a mock data set drawn from a hierarchical semi-analytic model of galaxy evolution. Traditional parametric models generally assume an exponentially declining rate of star formation after an initial instantaneous rise. Our results show that star formation histories with a much more gradual rise in the star formation rate are likely to be better templates, and are likely to give better overall estimates of the age distribution and star formation rate distribution of Lyman break galaxies (LBGs). For B- and V-dropouts, we find the best simple parametric model to be one where the star formation rate increases linearly with time. The exponentially declining model overpredicts the age by 100% and 120% for B- and V-dropouts, on average, while for a linearly increasing model, the age is overpredicted by 9% and 16%, respectively. Similarly, the exponential model underpredicts star formation rates by 56% and 60%, while the linearly increasing model underpredicts by 15% and 22%, respectively. For U-dropouts, the models where the star formation rate has a peak (near z {approx} 3) provide the best match for age-overprediction is reduced from 110% to 26%-and star formation rate-underprediction is reduced from 58% to 22%. We classify different types of star formation histories in the semi-analytic models and show how the biases behave for the different classes. We also provide two-band calibration formulae for stellar mass and star formation rate estimations.

Lee, Seong-Kook [Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218-2686 (United States); Ferguson, Henry C.; Somerville, Rachel S.; Wiklind, Tommy [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Giavalisco, Mauro, E-mail: joshua@pha.jhu.ed [Astronomy Department, University of Massachusetts, Amherst, MA 01003 (United States)

2010-12-20T23:59:59.000Z

379

John C. Stennis Space Center History of Stennis Space Center  

E-Print Network [OSTI]

Laboratory Propulsion Test Lead Center SSME Test Resp. 5/94 Stennis Space Center Estab. (5/88) Stennis Space · Dept. of Marine Science · Major Contractors · Pratt and Whitney Rocketdyne · Jacobs Technology Inc. · A, National Data Buoy Center · NOAA National Marine Fisheries Service · NOAA National Coastal Data Development

Waliser, Duane E.

380

Rochester Prevention Research Center National Center for Deaf Health Research  

E-Print Network [OSTI]

is being overweight or obese dangerous to your health? #12;Rochester Prevention Research Center NationalRochester Prevention Research Center National Center for Deaf Health Research Obesity and Your Health: The Deaf Weight Wise Research Project Scott Smith, MD, MPH Matt Starr, MPH Deaf Health Talks

Goldman, Steven A.

Note: This page contains sample records for the topic "difference star center" 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

CenterPulse Wisconsin National Primate Research Center  

E-Print Network [OSTI]

CenterPulse Wisconsin National Primate Research Center University of Wisconsin-Madison Contents Welcome to our year in review, CenterPulse. We hope you enjoy the new format. In making our news more Affiliates 3 Just Published 7 In the news 7 WIMR Opening and Board Tour 8 Reduced Diet Thwarts Aging 10 Kate

Wisconsin at Madison, University of

382

MSU EASTERN AGRICULTURAL RESEARCH CENTER NDSU WILLISTON RESEARCH EXTENSION CENTER  

E-Print Network [OSTI]

MSU EASTERN AGRICULTURAL RESEARCH CENTER NDSU WILLISTON RESEARCH EXTENSION CENTER 2006 AGRICULTURAL://www.sidney.ars.usda.gov/state/ North Dakota State University Williston Research Extension Center 14120 Hwy 2 Williston, ND 58801 (701 may have been more or less. Weather Summary Williston, nd Precipitation Temperature Month 2006 Avg

Dyer, Bill

383

MSU EASTERN AGRICULTURAL RESEARCH CENTER NDSU WILLISTON RESEARCH EXTENSION CENTER  

E-Print Network [OSTI]

MSU EASTERN AGRICULTURAL RESEARCH CENTER NDSU WILLISTON RESEARCH EXTENSION CENTER 2007 AGRICULTURAL Dakota State University Williston Research Extension Center 14120 Hwy 2 Williston, ND 58801 (701) 774-4315 Fax: (701) 774-4307 E-mail: NDSU.Williston.REC@.ndsu.edu http

Dyer, Bill

384

"Infotonics Technology Center"  

SciTech Connect (OSTI)

During this grant period July 15, 2002 thru September 30, 2004, the Infotonics Technology Center developed the critical infrastructure and technical expertise necessary to accelerate the development of sensors, alternative lighting and power sources, and other specific subtopics of interest to Department of Energy. Infotonics fosters collaboration among industry, universities and government and operates as a national center of excellence to drive photonics and microsystems development and commercialization. A main goal of the Center is to establish a unique, world-class research and development facility. A state-of-the-art microsystems prototype and pilot fabrication facility was established to enable rapid commercialization of new products of particular interest to DOE. The Center has three primary areas of photonics and microsystems competency: device research and engineering, packaging and assembly, and prototype and pilot-scale fabrication. Center activities focused on next generation optical communication networks, advanced imaging and information sensors and systems, micro-fluidic systems, assembly and packaging technologies, and biochemical sensors. With targeted research programs guided by the wealth of expertise of Infotonics???????????????????????????????????????????????????????????????¢???????????????????????????????????????????????????????????????????????????????????????????????????????????????????????????????? business and scientific staff, the fabrication and packaging facility supports and accelerates innovative technology development of special interest to DOE in support of its mission and strategic defense, energy, and science goals.

Fritzemeier, L., Boysel, M.B., and Smith, D.R.

2005-01-14T23:59:59.000Z

385

Data Center Energy Benchmarking: Part 4 - Case Study on a Computer-testing Center (No. 21)  

E-Print Network [OSTI]

data center & non-chilling Load Data Center Computer Loadpower density (W/ft2) Total Non-Data Center Load Data CenterComputer Load Data Center CRAH Units Chillers (Data Center

Xu, Tengfang; Greenberg, Steve

2007-01-01T23:59:59.000Z

386

Shear viscosity in hybrid stars  

Science Journals Connector (OSTI)

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

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

2012-05-03T23:59:59.000Z

387

Evolution of the Dark Matter Distribution at the Galactic Center  

Science Journals Connector (OSTI)

Annihilation radiation from neutralino dark matter at the Galactic center (GC) would be greatly enhanced if the dark matter were strongly clustered around the supermassive black hole (SBH). The existence of a dark matter spike is made plausible by the observed, steeply rising stellar density near the GC SBH. Here the time-dependent equations describing gravitational interaction of the dark matter with the stars are solved. Scattering of dark matter particles by stars would substantially lower the dark matter density near the GC SBH over 10Gyr, due both to kinetic heating and to capture of dark matter particles by the SBH. This evolution implies a decrease by several orders of magnitude in the observable flux of annihilation products compared with models that associate a steep, dark matter spike with the SBH.

David Merritt

2004-05-20T23:59:59.000Z

388

Neutron star equations of state with optical potential constraint  

E-Print Network [OSTI]

Nuclear matter and neutron stars are studied in the framework of an extended relativistic mean-field (RMF) model with higher-order derivative and density dependent couplings of nucleons to the meson fields. The derivative couplings lead to an energy dependence of the scalar and vector self-energies of the nucleons. It can be adjusted to be consistent with experimental results for the optical potential in nuclear matter. Several parametrisations, which give identical predictions for the saturation properties of nuclear matter, are presented for different forms of the derivative coupling functions. The stellar structure of spherical, non-rotating stars is calculated for these new equations of state (EoS). A substantial softening of the EoS and a reduction of the maximum mass of neutron stars is found if the optical potential constraint is satisfied.

Antic, Sofija

2015-01-01T23:59:59.000Z

389

Neutron star equations of state with optical potential constraint  

E-Print Network [OSTI]

Nuclear matter and neutron stars are studied in the framework of an extended relativistic mean-field (RMF) model with higher-order derivative and density dependent couplings of nucleons to the meson fields. The derivative couplings lead to an energy dependence of the scalar and vector self-energies of the nucleons. It can be adjusted to be consistent with experimental results for the optical potential in nuclear matter. Several parametrisations, which give identical predictions for the saturation properties of nuclear matter, are presented for different forms of the derivative coupling functions. The stellar structure of spherical, non-rotating stars is calculated for these new equations of state (EoS). A substantial softening of the EoS and a reduction of the maximum mass of neutron stars is found if the optical potential constraint is satisfied.

Sofija Antic; Stefan Typel

2015-01-29T23:59:59.000Z

390

Alternative Fuels Data Center: Disclaimer  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

AFDC AFDC Printable Version Share this resource Send a link to Alternative Fuels Data Center: Disclaimer to someone by E-mail Share Alternative Fuels Data Center: Disclaimer on Facebook Tweet about Alternative Fuels Data Center: Disclaimer on Twitter Bookmark Alternative Fuels Data Center: Disclaimer on Google Bookmark Alternative Fuels Data Center: Disclaimer on Delicious Rank Alternative Fuels Data Center: Disclaimer on Digg Find More places to share Alternative Fuels Data Center: Disclaimer on AddThis.com... Disclaimer The U.S. Department of Energy's (DOE) Alternative Fuels Data Center (AFDC) offers a wealth of information in the form of text, drawings, specifications, images, maps, and databases. This information combines research results, data analysis, descriptions of laws and incentives,

391

Alternative Fuels Data Center: Webmaster  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

About About Printable Version Share this resource Send a link to Alternative Fuels Data Center: Webmaster to someone by E-mail Share Alternative Fuels Data Center: Webmaster on Facebook Tweet about Alternative Fuels Data Center: Webmaster on Twitter Bookmark Alternative Fuels Data Center: Webmaster on Google Bookmark Alternative Fuels Data Center: Webmaster on Delicious Rank Alternative Fuels Data Center: Webmaster on Digg Find More places to share Alternative Fuels Data Center: Webmaster on AddThis.com... More in this section... Project Assistance News & Features Spanish Resources Contacts Webmaster Please use this form to send us your comments, report problems, and/or ask questions about information on the Alternative Fuels Data Center website. If your comment applies to a particular page, please provide the relevant

392

LANSCE | Lujan Neutron Scattering Center  

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

Department of Energy, National Office of Science Department of Energy, National Office of Science science.energy.gov Department of Energy, National Nuclear Security Administration nnsa.energy.gov Lujan Neutron Scattering Center Logo Lujan Center Mission The Lujan Center delivers science by exploiting the unique characteristics of intense beams of pulsed neutrons for academia, national security, and industry. Lujan Center Vision The Lujan Center will operate a world class user program in the service of the nation. Lujan Center scientists will be recognized for their leadership and innovation in neutron scattering. Lujan Center at LANSCE The Lujan Center is one of five user facilities supported by the LANSCE accelerator which is stewarded. Funding to operate 10 instruments in a national user program is provided by the Department of Energy's Office of

393

Center for Beam Physics, 1992  

SciTech Connect (OSTI)

This report contains the following information on the center for beam physics: Facilities; Organizational Chart; Roster; Profiles of Staff; Affiliates; Center Publications (1991--1993); and 1992 Summary of Activities.

Not Available

1993-06-01T23:59:59.000Z

394

Alternative Fuels Data Center: Contacts  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

About About Printable Version Share this resource Send a link to Alternative Fuels Data Center: Contacts to someone by E-mail Share Alternative Fuels Data Center: Contacts on Facebook Tweet about Alternative Fuels Data Center: Contacts on Twitter Bookmark Alternative Fuels Data Center: Contacts on Google Bookmark Alternative Fuels Data Center: Contacts on Delicious Rank Alternative Fuels Data Center: Contacts on Digg Find More places to share Alternative Fuels Data Center: Contacts on AddThis.com... More in this section... Project Assistance News & Features Spanish Resources Contacts Contacts Use these contacts for questions or comments about the Alternative Fuels Data Center. Website Contact Send us your comments, report problems, and/or ask questions about information on this site.

395

Nuclear Equation of State and Neutron Star Cooling  

E-Print Network [OSTI]

We investigate the effects of the nuclear equation of state (EoS) to the neutron star cooling. New era for nuclear EoS has begun after the discovery of $\\sim 2\\msun$ neutron stars PSR J1614$-$2230 and PSR J0348$+$0432 [1, 2]. Also recent works on the mass and radius of neutron stars from low-mass X-ray binaries [3] strongly constrain the EoS of nuclear matter. On the other hand, observations of the neutron star in Cassiopeia A (Cas A) more than 10 years confirmed the existence of nuclear superfluidity [4, 5]. Nuclear superfluidity reduces the heat capacities as well as neutrino emissivities. With nuclear superfluidity the neutrino emission processes are highly suppressed, and the existence of superfluidity makes the cooling path quite different from that of the standard cooling process. Superfluidity also allows new neutrino emission process, which is called `Pair Breaking and Formation'(PBF). PBF is a fast cooling process and can explain the fast cooling rate of neutron star in Cas A. Therefore, it is essent...

Lim, Yeunhwan; Lee, Chang-Hwan

2015-01-01T23:59:59.000Z

396

Large-Area Fast-Timing Systems In STAR  

SciTech Connect (OSTI)

The STAR experiment at RHIC concentrates on the tracking of charged hadrons via ionization, and the detection of electrons and photons via calorimetry, in a wide and azimuthally complete acceptance. STAR's ability to directly identify charged hadrons was initially limited to low momenta. This has been addressed via the construction of a large-area Time-of-Flight (TOF) system based on small Multigap Resistive Plate Chambers (MRPCs). The installation of the STAR TOF system was completed last fall. The full system is ran well in the recent RHIC Run 10. The operation of the system, and its performance for particle identification, during RHIC Runs 9 and 10 will be described. STAR's ability to identify muons is also extremely limited. Another large-area TOF system based on much larger MRPCs is envisioned. This system will be located outside the STAR magnet and is called the Muon Telescope Detector (MTD). Several different prototype MTD systems were operated in Runs 7 through 10, and a patch of near-final MTD detectors is under construction for use in the upcoming Run 11. The performance of the MTD prototype detectors, and the design of the Run 11 installation and the full system, will be described.

Llope, W. J. [Rice University, Houston, TX, 77005 (United States)

2011-06-01T23:59:59.000Z

397

GEORGE WATTS HILL ALUMNI CENTER  

E-Print Network [OSTI]

BR IN KH O U S- BU LLITT CHILLER BUILDING F KENAN STADIUM GEORGE WATTS HILL ALUMNI CENTER EHRINGHAUS

North Carolina at Chapel Hill, University of

398

BNL Guest, User and Visitor Center  

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

Working with Brookhaven National Laboratory Working with Brookhaven National Laboratory The Guest, User, Visitor Center (GUV Center) welcomes researchers from universities, government laboratories, and industry from within the US and abroad who are interested in visiting Brookhaven National Laboratory (BNL) or performing experiments at one of their scientific user facilities. The GUV Center is a central contact point for services for all guest, users, and visitors and is staffed with employees who know BNL well and can assist you in answering any questions you may have or directing you to individuals who can. Please feel free to contact them at guvcenter@bnl.gov or via phone at 631-344-3333. Access requirements depend upon the nature of your visit to BNL so if you are participating in a meeting your requirements will be different than

399

Drought Update Colorado Climate Center  

E-Print Network [OSTI]

Drought Update Colorado Climate Center Roger Pielke, Sr., Director Prepared by Tara Green and Odie Bliss http://climate.atmos.colostate.edu #12;© 2003 by The Colorado Climate Center. 2 http://www.ncdc.noaa.gov/oa/climate/research/2003/mar/st005dv00pcp200303.html #12;© 2003 by The Colorado Climate Center. 3 #12;© 2003

400

Ethics Center Annual Report III  

E-Print Network [OSTI]

#12;Ethics Center Annual Report III 2012-2013 TEXAS TECH UNIVERSITY #12;#12;TEXAS TECH UNIVERSITY August 31, 2013 Prepared by the TTU Ethics Center Annual Report III 2012-2013 #12;1 AnnualReportIII|8 proposed a university ethics center to provide the campus with ethics education resources. Since its

Rock, Chris

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


401

Pricing data center demand response  

Science Journals Connector (OSTI)

Demand response is crucial for the incorporation of renewable energy into the grid. In this paper, we focus on a particularly promising industry for demand response: data centers. We use simulations to show that, not only are data centers large loads, ... Keywords: data center, demand response, power network, prediction based pricing

Zhenhua Liu; Iris Liu; Steven Low; Adam Wierman

2014-06-01T23:59:59.000Z

402

Davison Health Center Dear Doctor,  

E-Print Network [OSTI]

5/131 Davison Health Center Dear Doctor, The Wesleyan University Davison Health Center is happy specific requirements detailed below. Our health center is equivalent to a typical outpatient community for allergy immunotherapy services within the context of our level of care, please complete the included

Royer, Dana

403

Data Center Airflow Management Retrofit  

Broader source: Energy.gov [DOE]

Case study bulletin describes the data center airflow management retrofit. The study includes information about how the data center energy densities (measured in power-use per square foot), increase energy savings for cooling, and how it can be realized by optimizing airflow pathways within the data center.

404

University of Connecticut Health Center  

E-Print Network [OSTI]

by a designated licensed health care professional here at UCHC who did not participate in the original denialUniversity of Connecticut Health Center (Patient Identification) Request to View Record DHHS Government Center University of Connecticut Health Center J.F. Kennedy Federal Building ­ Room

Oliver, Douglas L.

405

A Walking Tour Health Center  

E-Print Network [OSTI]

and caring. #12;3. River of Ponds Tapestry Enter the Health Center, look to the left, and see the massiveHealing Pathways A Walking Tour of the UConn Health Center Public Art Collection Made possible by a generous gift from the Health Center Auxiliary #12;#12;Welcome! Everywhere you walk, whether outdoors

Oliver, Douglas L.

406

SNAPSHOT … THE ENERGY STAR  

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

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

407

ENERGY STAR Score for Warehouses  

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

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

408

National Carbon Capture Center Launches Post-Combustion Test Center |  

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

Carbon Capture Center Launches Post-Combustion Test Center Carbon Capture Center Launches Post-Combustion Test Center National Carbon Capture Center Launches Post-Combustion Test Center June 6, 2011 - 2:32pm Addthis Jenny Hakun What does this mean for me? Commercial deployment of the processes tested here could cut carbon pollution. Innovation is important to finding ways to make energy cleaner. And testing the ideas and processes that researchers come up with is critical to moving ideas from the lab to the marketplace. That's why the Department of Energy recently commissioned an Alabama testing facility that will help move research forward and speed up deployment of innovative post-combustion carbon dioxide (CO2) capture technologies for coal-based power plants. The Post-Combustion Carbon Capture Center (or PC4) facility tests new

409

National Carbon Capture Center Launches Post-Combustion Test Center |  

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

National Carbon Capture Center Launches Post-Combustion Test Center National Carbon Capture Center Launches Post-Combustion Test Center National Carbon Capture Center Launches Post-Combustion Test Center June 7, 2011 - 1:00pm Addthis Washington, D.C. - The recent successful commissioning of an Alabama-based test facility is another step forward in research that will speed deployment of innovative post-combustion carbon dioxide (CO2) capture technologies for coal-based power plants, according to the U.S. Department of Energy (DOE). Technologies tested at the Post-Combustion Carbon Capture Center (or PC4) are an important component of Carbon Capture and Storage, whose commercial deployment is considered by many experts as essential for helping to reduce human-generated CO2 emissions that contribute to potential climate change.

410

SciTech Connect: Energy Frontier Research Center Center for Materials...  

Office of Scientific and Technical Information (OSTI)

Technical Report: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Citation Details In-Document Search Title: Energy Frontier Research Center Center...

411

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Connecticut Incentives and Laws Connecticut Incentives and Laws The following is a list of expired, repealed, and archived incentives, laws, regulations, funding opportunities, or other initiatives related to alternative fuels and vehicles, advanced technologies, or air quality. Hydrogen and Fuel Cell Promotion Archived: 08/31/2013 The Connecticut Center for Advanced Technology (CCAT), with funding from the Department of Economic and Community Development (DECD), has established a Connecticut Hydrogen-Fuel Cell Coalition (Coalition). The Coalition works to enhance economic growth through the development, manufacture, and deployment of fuel cell and hydrogen technologies and associated fueling systems. Representatives from industry, government, academia, labor, and other stakeholders make up the Coalition. CCAT

412

Providence Newberg Medical Center  

High Performance Buildings Database

Newberg, OR In 2002, Providence Health & Services began planning a new 188,000 square foot medical center in Newberg, Oregon to respond to the growing community's need for accessible health care. Since this was Providence's first new hospital in almost thirty years, its leaders decided to approach the project through innovative planning, design, and construction, including the achievement of lifecycle energy savings and a potential LEED certification. The hospital is comprised of 40 inpatient beds with views out to the surrounding rural landscape or into lushly planted internal courtyards.

413

A Heavy Flavor Tracker for STAR  

SciTech Connect (OSTI)

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

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

2008-02-25T23:59:59.000Z

414

Neutron skins and neutron stars  

SciTech Connect (OSTI)

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

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

2013-11-07T23:59:59.000Z

415

Nuclear Physics of Neutron Stars  

E-Print Network [OSTI]

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

J. Piekarewicz

2009-01-28T23:59:59.000Z

416

Towards a realistic axion star  

E-Print Network [OSTI]

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

J. Barranco; A. Bernal

2008-08-01T23:59:59.000Z

417

Beryllium abundances in metal-poor stars  

Science Journals Connector (OSTI)

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

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

2009-01-01T23:59:59.000Z

418

Cold quark matter in compact stars  

SciTech Connect (OSTI)

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

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

2013-03-25T23:59:59.000Z

419

Haier: ENERGY STAR Referral (ESA408J)  

Broader source: Energy.gov [DOE]

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

420

Haier: ENERGY STAR Referral (ESA3087)  

Broader source: Energy.gov [DOE]

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

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


421

Equator Appliance: ENERGY STAR Referral (EZ 3720)  

Broader source: Energy.gov [DOE]

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

422

Review: Magnetic fields of O stars  

E-Print Network [OSTI]

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

Wade, G A

2014-01-01T23:59:59.000Z

423

ENERGY STAR Webinar: Portfolio Manager 101  

Broader source: Energy.gov [DOE]

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

424

How to Apply for the ENERGY STAR  

Broader source: Energy.gov [DOE]

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

425

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

426

Electron Microscopy Center  

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

Overview Overview The mission of the Electron Microscopy Center (EMC) is to: Conduct materials research using advanced microstructural characterization methods; Maintain unique resources and facilities for scientific research for the both the Argonne National Laboratory and national scientific community. Develop and expand the frontiers of microanalysis by fostering the evolution of synergistic state-of-the-art resources in instrumentation, techniques and scientific expertise; The staff members of the EMC carry out their own research as well as participate in collaborative programs with other scientists at Argonne National Laboratory as well as researchers, educators and students worldwide. The Electron Microscopy Center (EMC) at Argonne National Laboratory develops and maintains unique capabilities for electron beam characterization and applies those capabilities to solve materials problems. The EMC staff perform collaborative research with members of other Divisions at Argonne National Laboratory and with collaborators from universities and other laboratories. The expertise and facilities of the EMC additionally serve a group of national and international researchers. The EMC emphasizes three major areas: materials research, technique and instrumentation development, and operation as a national research facility. Research by EMC personnel includes microscopy based studies in high Tc superconducting materials, irradiation effects in metals and semiconductors, phase transformations, and processing related structure and chemistry of interfaces in thin films.

427

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

E-Print Network [OSTI]

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

Barnes, Joshua Edward

428

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

E-Print Network [OSTI]

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

Barnes, Joshua Edward

429

National Fuel Cell Technology Evaluation Center (Text Version...  

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

is a map that identifies the different labs, the office space, and the high performance computing center. There is a link, if you just search on NREL ESIF there is a lot of...

430

NuSTAR: Nuclear Spectroscopic Telescope Array  

SciTech Connect (OSTI)

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

Craig, Bill

2012-06-13T23:59:59.000Z

431

Black Stars and Gamma Ray Bursts  

E-Print Network [OSTI]

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

Tanmay Vachaspati

2007-06-08T23:59:59.000Z

432

ENERGY STAR Guide to Retro-Commissioning  

Broader source: Energy.gov [DOE]

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

433

Alternative Fuels Data Center: Propane  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Propane Propane Printable Version Share this resource Send a link to Alternative Fuels Data Center: Propane to someone by E-mail Share Alternative Fuels Data Center: Propane on Facebook Tweet about Alternative Fuels Data Center: Propane on Twitter Bookmark Alternative Fuels Data Center: Propane on Google Bookmark Alternative Fuels Data Center: Propane on Delicious Rank Alternative Fuels Data Center: Propane on Digg Find More places to share Alternative Fuels Data Center: Propane on AddThis.com... More in this section... Propane Basics Benefits & Considerations Stations Vehicles Laws & Incentives Propane Fuel Prices Find propane fuel prices and trends. Propane, also known as liquefied petroleum gas (LPG) or autogas, has been used worldwide as a vehicle fuel for decades. It is stored as a liquid, and

434

Alternative Fuels Data Center: Hydrogen  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Hydrogen Hydrogen Printable Version Share this resource Send a link to Alternative Fuels Data Center: Hydrogen to someone by E-mail Share Alternative Fuels Data Center: Hydrogen on Facebook Tweet about Alternative Fuels Data Center: Hydrogen on Twitter Bookmark Alternative Fuels Data Center: Hydrogen on Google Bookmark Alternative Fuels Data Center: Hydrogen on Delicious Rank Alternative Fuels Data Center: Hydrogen on Digg Find More places to share Alternative Fuels Data Center: Hydrogen on AddThis.com... More in this section... Hydrogen Basics Benefits & Considerations Stations Vehicles Laws & Incentives Hydrogen Hydrogen is a potentially emissions-free alternative fuel that can be produced from diverse domestic energy sources. Research is under way to make hydrogen vehicles practical for widespread use.

435

Alternative Fuels Data Center: Biodiesel  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Biodiesel Biodiesel Printable Version Share this resource Send a link to Alternative Fuels Data Center: Biodiesel to someone by E-mail Share Alternative Fuels Data Center: Biodiesel on Facebook Tweet about Alternative Fuels Data Center: Biodiesel on Twitter Bookmark Alternative Fuels Data Center: Biodiesel on Google Bookmark Alternative Fuels Data Center: Biodiesel on Delicious Rank Alternative Fuels Data Center: Biodiesel on Digg Find More places to share Alternative Fuels Data Center: Biodiesel on AddThis.com... More in this section... Biodiesel Basics Benefits & Considerations Stations Vehicles Laws & Incentives Biodiesel Fuel Prices Find biodiesel fuel prices and trends. Biodiesel is a domestically produced, renewable fuel that can be manufactured from vegetable oils, animal fats, or recycled restaurant

436

Alternative Fuels Data Center: Electricity  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Electricity Electricity Printable Version Share this resource Send a link to Alternative Fuels Data Center: Electricity to someone by E-mail Share Alternative Fuels Data Center: Electricity on Facebook Tweet about Alternative Fuels Data Center: Electricity on Twitter Bookmark Alternative Fuels Data Center: Electricity on Google Bookmark Alternative Fuels Data Center: Electricity on Delicious Rank Alternative Fuels Data Center: Electricity on Digg Find More places to share Alternative Fuels Data Center: Electricity on AddThis.com... More in this section... Electricity Basics Benefits & Considerations Stations Vehicles Laws & Incentives Electricity Fuel Prices Find electricity fuel prices and trends. Electricity can be used to power all-electric vehicles and plug-in hybrid

437

Regency Centers | Open Energy Information  

Open Energy Info (EERE)

Regency Centers Regency Centers Jump to: navigation, search Name Regency Centers Place Jacksonville, FL Zip 32202 Website http://www.regencycenters.com References Regency Centers[1] Information About Partnership with NREL Partnership with NREL Yes Partnership Type Test & Evaluation Partner Partnering Center within NREL Electricity Resources & Building Systems Integration Partnership Year 2009 Link to project description http://www.nrel.gov/features/20090619_buildings.html LinkedIn Connections CrunchBase Profile No CrunchBase profile. Create one now! Regency Centers is a company located in Jacksonville, FL. Recency Centers is one of 23 National Accounts Companies partnering with NREL and PNNL for testing and validation of design concepts that will reduce energy consumption in commercial buildings[2].

438

Alternative Fuels Data Center: Glossary  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

AFDC AFDC Printable Version Share this resource Send a link to Alternative Fuels Data Center: Glossary to someone by E-mail Share Alternative Fuels Data Center: Glossary on Facebook Tweet about Alternative Fuels Data Center: Glossary on Twitter Bookmark Alternative Fuels Data Center: Glossary on Google Bookmark Alternative Fuels Data Center: Glossary on Delicious Rank Alternative Fuels Data Center: Glossary on Digg Find More places to share Alternative Fuels Data Center: Glossary on AddThis.com... Glossary Use this comprehensive glossary to define terms commonly used in the alternative fuels and advanced vehicles industry. If you have questions about specific technologies or fuels, contact the Technical Response Service at 1-800-254-6735. Click on the appropriate letter. · A· B· C· D· E· F· G· H· I· J· K· L· M· N· O· P· Q· R· S· T· U· V· W· X· Y· Z·

439

Alternative Fuels Data Center: Widgets  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Widgets to someone by Widgets to someone by E-mail Share Alternative Fuels Data Center: Widgets on Facebook Tweet about Alternative Fuels Data Center: Widgets on Twitter Bookmark Alternative Fuels Data Center: Widgets on Google Bookmark Alternative Fuels Data Center: Widgets on Delicious Rank Alternative Fuels Data Center: Widgets on Digg Find More places to share Alternative Fuels Data Center: Widgets on AddThis.com... Widgets The Alternative Fuels Data Center (AFDC) offers widgets about alternative fuels and advanced technology vehicles. Get these widgets for your website, blog, or social networking site so your readers can access current information from the AFDC. Also find more widgets from the U.S. Department of Energy's Office of Energy Efficiency and Renewable Energy. Alternative Fueling Station Locator

440

Alternative Fuels Data Center: Ethanol  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Ethanol Ethanol Printable Version Share this resource Send a link to Alternative Fuels Data Center: Ethanol to someone by E-mail Share Alternative Fuels Data Center: Ethanol on Facebook Tweet about Alternative Fuels Data Center: Ethanol on Twitter Bookmark Alternative Fuels Data Center: Ethanol on Google Bookmark Alternative Fuels Data Center: Ethanol on Delicious Rank Alternative Fuels Data Center: Ethanol on Digg Find More places to share Alternative Fuels Data Center: Ethanol on AddThis.com... More in this section... Ethanol Basics Benefits & Considerations Stations Vehicles Laws & Incentives Ethanol Fuel Prices Find ethanol fuel prices and trends. Ethanol is a renewable fuel made from corn and other plant materials. The use of ethanol is widespread-almost all gasoline in the U.S. contains

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


441

Alternative Fuels Data Center: Tools  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Tools to someone by Tools to someone by E-mail Share Alternative Fuels Data Center: Tools on Facebook Tweet about Alternative Fuels Data Center: Tools on Twitter Bookmark Alternative Fuels Data Center: Tools on Google Bookmark Alternative Fuels Data Center: Tools on Delicious Rank Alternative Fuels Data Center: Tools on Digg Find More places to share Alternative Fuels Data Center: Tools on AddThis.com... Tools The Alternative Fuels Data Center offers a large collection of helpful tools. These calculators, interactive maps, and data searches can assist fleets, fuel providers, and other transportation decision makers in their efforts to reduce petroleum use. Calculators Vehicle Cost Calculator Compare cost of ownership and emissions for most vehicle models. Icon_mobile_version mobile

442

Solar Energy Resource Center | Department of Energy  

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

Energy Resource Center Solar Energy Resource Center The SunShot Initiative's Solar Energy Resource Center contains work developed by DOE, national laboratories and SunShot...

443

Data Center Energy Efficiency | Department of Energy  

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

Program Areas Data Center Energy Efficiency Data Center Energy Efficiency The Federal Energy Management Program (FEMP) supports data center efficiency initiatives by encouraging...

444

Industrial Assessment Centers Quarterly Update, Spring 2014 ...  

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

Assessment Centers Quarterly Update, Spring 2014 Read the Industrial Assessment Centers (IAC) Quarterly Update -- Spring 2014 Industrial Assessment Centers (IAC) Quarterly Update...

445

The DOE Information Center | Department of Energy  

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

Community Engagement The DOE Information Center The DOE Information Center The DOE Information Center provides citizens a consolidated facility to obtain information and records...

446

Evaluating Economizer Use In Data Centers  

E-Print Network [OSTI]

Evaluating Economizer Use in Data Centers Benjamin Chu,eelet Keywords: Data centers, economizers, HVAC, indoor airfor data centers are economizers, which turn off the power

Chu, Benjamin

2009-01-01T23:59:59.000Z

447

WINDExchange: Wind Energy Regional Resource Centers  

Wind Powering America (EERE)

Bookmark and Share Regional Resource Centers About Economic Development Siting Wind Energy Regional Resource Centers The U.S. Department of Energy's Regional Resource Centers...

448

The Nature of the Massive Young Stars in W75 N  

E-Print Network [OSTI]

We have observed the W75 N massive star forming region in SiO(J=2-1 & J=1-0) at 3" - 5" resolution and in 6 cm, 2 cm, and 7 mm continuum emission at 1.4" - 0.2" resolution. The abundance ratio of [SiO]/[H2] is roughly 5-7 x 10^-11 which is typical for what is expected in the ambient component of molecular clouds with active star formation. The SiO morphology is diffuse and centered on the positions of the ultracompact HII regions - no collimated, neutral jet was discovered. The ionized gas surrounding the protostars have emission measures ranging from 1-15 x 10^6 pc cm^-6, densities from 0.4-5 x 10^4 cm^-3, and derived spectral types of the central ionizing stars ranging from B0.5 to B2. Most of the detected sources have spectral indicies which suggest optically thin to moderately optically thick HII regions produced by a central ionizing star. The spread in ages between the oldest and youngest early-B protostars in the W75 N cluster is 0.1-5 x 10^6 years. This evolutionary timescale for W75 N is consistent with that found for early-B stars born in clusters forming more massive stars (Mstar > 25 Msun).

D. S. Shepherd; S. E. Kurtz; L. Testi

2003-10-15T23:59:59.000Z

449

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

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

Join ENERGY STAR as a partner Join ENERGY STAR as a partner Secondary menu About us Press room Contact Us Portfolio Manager Login Facility owners and managers Existing buildings Commercial new construction Industrial energy management Small business Service providers Service and product providers Verify applications for ENERGY STAR certification Design commercial buildings Energy efficiency program administrators Commercial and industrial program sponsors Associations State and local governments Federal agencies Tools and resources Training In this section How can ENERGY STAR help your business? Get started Join ENERGY STAR as a partner Service and Product Provider associations partnering with ENERGY STAR ENERGY STAR service & product provider training series Service and product provider's marketing toolkit

450

STAR Highlights on Heavy Ion Physics  

E-Print Network [OSTI]

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

Shusu Shi

2014-09-30T23:59:59.000Z

451

Shear viscosity in neutron star cores  

E-Print Network [OSTI]

We calculate the shear viscosity $\\eta = \\eta_{e\\mu}+\\eta_{n}$ in a neutron star core composed of nucleons, electrons and muons ($\\eta_{e\\mu}$ being the electron-muon viscosity, mediated by collisions of electrons and muons with charged particles, and $\\eta_{n}$ the neutron viscosity, mediated by neutron-neutron and neutron-proton collisions). Deriving $\\eta_{e\\mu}$, we take into account the Landau damping in collisions of electrons and muons with charged particles via the exchange of transverse plasmons. It lowers $\\eta_{e\\mu}$ and leads to the non-standard temperature behavior $\\eta_{e\\mu}\\propto T^{-5/3}$. The viscosity $\\eta_{n}$ is calculated taking into account that in-medium effects modify nucleon effective masses in dense matter. Both viscosities, $\\eta_{e\\mu}$ and $\\eta_{n}$, can be important, and both are calculated including the effects of proton superfluidity. They are presented in the form valid for any equation of state of nucleon dense matter. We analyze the density and temperature dependence of $\\eta$ for different equations of state in neutron star cores, and compare $\\eta$ with the bulk viscosity in the core and with the shear viscosity in the crust.

P. S. Shternin; D. G. Yakovlev

2008-08-14T23:59:59.000Z

452

Evolution of Low-Mass Population III Stars  

E-Print Network [OSTI]

We present the evolutionary models of metal-free stars in the mass range from 0.8 to 1.2 Msun with up-to-date input physics. The evolution is followed to the onset of hydrogen mixing into a convection, driven by the helium flash at red giant or asymptotic giant branch phase. The models of mass M >= 0.9 Msun undergo the central hydrogen flash, triggered by the carbon production due to the 3-alpha reactions. We find that the border of the off-center and central ignition of helium core flash falls between 1.1 and 1.2 Msun; the models of mass M hydrogen mixing at the tip of red giant branch while the models of M = 1.2 Msun during the helium shell flashes on the asymptotic giant branch. The equation of state for the Coulomb liquid region, where electron conduction and radiation compete, is shown to be important since it affects the thermal state in the helium core and influences the red giant branch evolution. It is also found that the non-resonant term of 3-alpha reactios plays an important role, although it has negligible effect in the evolution of stars of younger populations. We compare our models with the computations by several other sets of authors, to confirm the good agreement except for one study which finds the helium ignition much closer to the center with consequences important for subsequent evolution.

Takuma Suda; Masayuki Y. Fujimoto; Naoki Itoh

2005-04-25T23:59:59.000Z

453

Toy stars in one dimension  

Science Journals Connector (OSTI)

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

J. J. Monaghan; D. J. Price

2004-06-01T23:59:59.000Z

454

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

E-Print Network [OSTI]

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

Katherine Freese; Peter Bodenheimer; Paolo Gondolo; Douglas Spolyar

2008-12-28T23:59:59.000Z

455

Galactic Center Gamma-Ray Excess from Dark Matter Annihilation: Is There a Black Hole Spike?  

Science Journals Connector (OSTI)

If the supermassive black hole Sgr A* at the center of the Milky Way grew adiabatically from an initial seed embedded in a Navarro-Frenk-White dark matter (DM) halo, then the DM profile near the hole has steepened into a spike. We calculate the dramatic enhancement to the gamma-ray flux from the Galactic center (GC) from such a spike if the 13GeV excess observed in Fermi data is due to DM annihilations. We find that for the parameter values favored in recent fits, the point-source-like flux from the spike is 35 times greater than the flux from the inner 1 of the halo, far exceeding all Fermi point source detections near the GC. We consider the dependence of the spike signal on astrophysical and particle parameters and conclude that if the GC excess is due to DM, then a canonical adiabatic spike is disfavored by the data. We discuss alternative Galactic histories that predict different spike signals, including (i)the nonadiabatic growth of the black hole, possibly associated with halo and/or black hole mergers, (ii)gravitational interaction of DM with baryons in the dense core, such as heating by stars, or (iii)DM self-interactions. We emphasize that the spike signal is sensitive to a different combination of particle parameters than the halo signal and that the inclusion of a spike component to any DM signal in future analyses would provide novel information about both the history of the GC and the particle physics of DM annihilations.

Brian D. Fields; Stuart L. Shapiro; Jessie Shelton

2014-10-09T23:59:59.000Z

456

Electron Microscopy Center  

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

Submit an EMC Proposal Submit an EMC Proposal EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Becoming a User Submit a Proposal End-of-Proposal Report Acknowledgment User Training User Safety User Status Instrument Access User Committee User Meetings Data Storage Policy Visiting the EMC Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers Submit an EMC Proposal EMC Proposal Submission Deadline Dates for FY2014: November 1, 2013 March 7, 2014 July 11, 2014 Is your proposal a multi-facility proposal? In other words, do you intend to submit proposals to EMC and APS or CNM for your research project? If your answer is "yes," go now to the Proposal Gateway.

457

Electron Microscopy Center  

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

EMC Users Committee EMC Users Committee EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Becoming a User Submit a Proposal End-of-Proposal Report Acknowledgment User Training User Safety User Status Instrument Access User Committee User Meetings Data Storage Policy Visiting the EMC Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers EMC Users Committee An EMC Users Committee has been organized to enhance communication between the user community and the EMC. While the EMC relies on and encourages strong interaction among its users and between its staff and users, the Users Committee provides an additional formal mechanism for user input into EMC planning and operations to ensure that users' needs and concerns are addressed.

458

factsheet: National Prototype Center  

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

the World Safer the World Safer This enduring national asset integrates science and technology for manufacturing success that meets our customer's special manufacturability challenges. Since its establishment in 1997, more than 5,0 0 0 i ndustr ies and government agencies have capitalized on the resources of the National Prototype Center (NPC). These customers received subject -matter expertise as well as critical manufacturing resources enabling development of i n novat ive manufacturing solutions. Specializing in high-risk, complex prototype work, the NPC integrates manufacturing, engineering and science to build first-of-a-kind products. It also modifies or enhances existing products and develops new, innovative manufacturing processes to solve the toughest manufacturing problems.

459

National Fertilizer Development Center  

Office of Legacy Management (LM)

h-L h-L National Fertilizer Development Center May 15, 1980 nww Hr. William Et Mott, Director Environmental Control Technology Division Office of Environment Dcpartiaent of Energy Washington, DC 20545 Dear Mr. Mott: This is in response to your letter of May 5 requesting ccmments on a report dated Xarct; 1930 which summarizes a preliminary radiological survey of facilities used in the early 1950's for studies of recovery of uranium from leached zone ore. I have made a few suggested changes to the report, which is being returned to you. * Thaul, you for the opportunity to review this report. Sincerely, , Enclosure Development Branch . 1 -a' . I . . . PRELIMINARY SURVEY OF TENNESSEE VALLEY AUTHORITY MUSCLE SHOALS, ALA&A Work .performed by the Health and Safety Research Division

460

Alternative Fuels Data Center  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Do alternative fuel vehicles Do alternative fuel vehicles (AFVs) improve air quality? How does the use of alternative fuels affect smog formation? You may find answers to these and other questions through the U.S. Department of Energy's (DOE) Alternative Fuels Data Center (AFDC)-the nation's most com- prehensive repository of perfor- mance data and general informa- tion on AFVs. To date, more than 600 vehi- cles-including light-duty cars, trucks, vans, transit buses, and heavy-duty trucks-have been tested on various alternative and conventional fuels with the goal of identifying the potential for alter- native fuels to displace petroleum and improve our nation's air quality. Although comparing regu- lated emissions between fuels may seem straightforward, evaluating emissions is complicated by

Note: This page contains sample records for the topic "difference star center" 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

EV Technical Center  

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

December 2000 December 2000 AQMD CONTRACT #00192 Project Number: TC-00-0101 Report Number: TC-00-0101-TR02 Electric Vehicle Technical Center Prepared by: Ricardo Solares Juan C. Argueta Southern California Edison December 20, 2000 Page i DISCLAIMER OF WARRANTIES AND LIMITATION OF LIABILITIES This report was prepared by the Electric Transportation Division of Southern California Edison, a subsidiary of Edison International. Neither the Electric Transportation Division of Southern California Edison, Southern California Edison, Edison International, nor any person working for or on behalf of any of them makes any warranty or representation, express or implied, (i) with respect to the use of any information, product, process or procedure discussed in this report, including

462

Electron Microscopy Center  

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

An Office of Science User Facility An Office of Science User Facility The Electron Microscopy Center (EMC) at Argonne National Laboratory develops and maintains unique capabilities for electron beam characterization and applies those capabilities to solve materials problems. The EMC staff carry out research with collaborators and users from Argonne, universities, and other laboratories. The expertise and facilities of the EMC additionally serve a group of national and international researchers. The EMC emphasizes three major areas: materials research, technique and instrumentation development, and operation as a national research facility. Research by EMC personnel includes microscopy based studies in high Tc superconducting materials, irradiation effects in metals and semiconductors, phase transformations, and processing related structure and chemistry of interfaces in thin films.

463

Electron Microscopy Center  

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

End-of-Proposal Report End-of-Proposal Report EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Becoming a User Submit a Proposal End-of-Proposal Report Acknowledgment User Training User Safety User Status Instrument Access User Committee User Meetings Data Storage Policy Visiting the EMC Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers End-of-Proposal Report In accordance with the User Agreement, please provide the EMC with the following information when your proposal expires (one year after its acceptance date or when the experiments end, whichever is sooner). A research summary/progress report using these two templates:

464

Valley Forge Corporate Center  

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

55 Jefferson Ave. 55 Jefferson Ave. Valley Forge Corporate Center Norristown, PA 19403-2497 Pauline Foley Assistant General Counsel 610.666.8248 | Fax - 610.666.8211 foleyp@pjm.com October 30, 2013 Via Electronic Mail: juliea.smith@hq.doe.gov Christopher.lawrence@hq.doe.gov Julie A. Smith Office of Electricity Delivery and Energy Reliability Mail Code: OE-20 U.S. Department of Energy 1000 Independence Avenue, SW Washington, D.C. 20585 Re: Department of Energy - Improving Performance of Federal Permitting and Review of Infrastructure Projects. Request for Information ("RFI") 78 Fed. Reg. 53436 (August 29, 2013) Dear Ms. Smith: Please accept the following comments submitted on behalf of PJM Interconnection, L.L.C. ("PJM") in response to the RFI issued in the above captioned matter. This letter responds

465

EV Technical Center  

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

Carrier Route Vehicles Carrier Route Vehicles Quarterly Report, June 2001 AQMD CONTRACT #00192 Project Number: TC-00-0101 Report Number: TC-00-0101-TR04 Electric Vehicle Technical Center An ISO 9001 Certified Facility Prepared by: Michel Wehrey Juan C. Argueta Julie M. Phung Southern California Edison June 15, 2001 Page i DISCLAIMER OF WARRANTIES AND LIMITATION OF LIABILITIES This report was prepared by the Electric Transportation Division of Southern California Edison, a subsidiary of Edison International. Neither the Electric Transportation Division of Southern California Edison, Southern California Edison, Edison International, nor any person working for or on behalf of any of them makes any warranty or representation, express or implied, (i) with respect to the

466

Electron Microscopy Center  

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

SAMM SAMM EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers Sub-Ångstrom Microscopy and Microanalysis Facility In order to meet the scientific challenges of the future, the EMC has built a new state-of-the-art laboratory space for advanced electron microscopy. The new building has been designed to provide next- generation science with an operating environment that cannot be attained by renovating existing facilities. The EMC staff learned as much as possible from similar efforts around the world, including the SuperSTEM building at Daresbury, the Triebenberg Special Laboratory, the AML at Oak Ridge National Laboratory, the new NIST building, and various facilities for nanoscience.

467

Electron Microscopy Center  

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

Becoming a User Becoming a User EMC Home Overview Personnel Resources Highlights Publications Visit EMC Contact Info Information for Users Becoming a User Submit a Proposal End-of-Proposal Report Acknowledgment User Training User Safety User Status Instrument Access User Committee User Meetings Data Storage Policy Visiting the EMC Instrument Calendars Info for EMC Staff SÅMM Facility TEAM Project Microscopy Links Argonne Facilities DOE/BES Facilities DOE/BES BES Electron Beam Microcharacterization Centers Procedure to Become a User at the EMC 1. Summary All users have to fulfill certain requirements before access to the EMC can be granted. The following list provides short descriptions of the requirements. Details can be found on this page and via the relevant links at the left. Register for access to Argonne's scientific user facilities (or update your user registration information).

468

LANSCE | Lujan Center | Highlights  

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

Highlights New Evidence to Aid Search for Charge 'Stripes' in Superconductors Findings identify signature that will help scientists investigate and understand materials that carry current with no resistance "The scientists ground up crystals of the test material into a fine powder and placed samples of it in line with a beam of neutrons at the Los Alamos Neutron Scattering Center at Los Alamos National Laboratory. Similar to the way light reflecting off an object enters your eyes to create an image, the neutron beams diffracted by the crystals' atoms yield information about the positions of the atoms. The scientists used that information to infer the material's electronic structure, and repeated the experiment at gradually warmer temperatures."

469

Supernova Science Center  

SciTech Connect (OSTI)

The Supernova Science Center (SNSC) was founded in 2001 to carry out theoretical and computational research leading to a better understanding of supernovae and related transients. The SNSC, a four-institutional collaboration, included scientists from LANL, LLNL, the University of Arizona (UA), and the University of California at Santa Cruz (UCSC). Intitially, the SNSC was funded for three years of operation, but in 2004 an opportunity was provided to submit a renewal proposal for two years. That proposal was funded and subsequently, at UCSC, a one year no-cost extension was granted. The total operational time of the SNSC was thus July 15, 2001 - July 15, 2007. This document summarizes the research and findings of the SNSC and provides a cummulative publication list.

S. E. Woosley

2008-05-05T23:59:59.000Z

470

Industrial Assessment Center  

SciTech Connect (OSTI)

The University of Dayton (UD) performed energy assessments, trained students and supported USDOE objectives. In particular, the UD Industrial Assessment Center (IAC) performed 96 industrial energy assessment days for mid-sized manufacturers. The average identified and implemented savings on each assessment were $261,080 per year and $54,790 per year. The assessments served as direct training in industrial energy efficiency for 16 UD IAC students. The assessments also served as a mechanism for the UD IAC to understand manufacturing energy use and improve upon the science of manufacturing energy efficiency. Specific research results were published in 16 conference proceedings and journals, disseminated in 22 additional invited lectures, and shared with the industrial energy community through the UD IAC website.

J. Kelly Kissock; Becky Blust

2007-04-17T23:59:59.000Z

471

HPC Code Center Request Form | Computatioinal Scince Center, Brookhaven  

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

HPC Code Center Request Form HPC Code Center Request Form All fields are required unless marked as optional. Full Name Institution/Company Email Address Telephone Number Department * Basic Energy Sciences Directorate (DC) Bioscience Department (BO) Business Development & Analysis Office (BU) Business Operations (DI) CEGPA Directorate (DK) Center for Functional Nanomaterials (NC) Chemistry Department (CO) Collider Accelerator Department (AD) Community, Education, Government and Public Affairs (PA) Computational Science Center (CC) Condensed Matter Physics and Materials Science Department (PM) Counterintelligence (CI) Department of Energy (AE) Deputy Director for Operations Directorate (DE) Director's Office Directorate (DO) Diversity Office (DV) Energy & Utilities Division (EU) Environment, Safety and Health

472

Center for Inverse Design: Collaboration Tool for the Center...  

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

Collaboration Tool for the Center for Inverse Design The SharePoint collaboration tool provides access to research results obtained from various theoretical and experimental...

473

THE CIRCUMNUCLEAR STAR FORMATION ENVIRONMENT OF NGC 6946: Br ? AND H{sub 2} RESULTS FROM KECK INTEGRAL FIELD SPECTROSCOPY  

SciTech Connect (OSTI)

We present a three-dimensional data cube of the K-band continuum and the Br ?, H{sub 2} S(0), and S(1) lines within the central 18.''5 13.''8 (520 pc 390 pc) region of NGC 6946. Data were obtained using OSIRIS, a near-infrared Integral Field Spectrograph at Keck Observatory, with Laser Guide Star Adaptive Optics. The 0.''3 resolution allows us to investigate the stellar bulge and the forming star clusters in the nuclear region on 10 pc scales. We detect giant H II regions associated with massive young star clusters in the nuclear spiral/ring (R ? 30 pc) and in the principal shocks along the nuclear bar. Comparisons of the Br ? fluxes with Pa ? line emission and radio continuum indicate A{sub K} ? 3, A{sub V} ? 25 for the nuclear star-forming regions. The most luminous H II regions are restricted to within 70 pc of the center, despite the presence of high gas columns at larger radii (R ? 200 pc). H{sub 2} emission is restricted to clouds within R ? 60 pc of the center, resembling the distribution of HCN line emission. We propose that gas-assisted migration of the young star clusters is contributing to the buildup of the nuclear bar and nuclear star cluster (R < 30 pc) in this galaxy.

Tsai, Chao-Wei [Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125 (United States); Turner, Jean L. [Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095-1547 (United States); Beck, Sara C. [Department of Physics and Astronomy, Tel Aviv University, Ramat Aviv (Israel); Meier, David S. [Department of Physics, New Mexico Institute of Mining and Technology, Socorro, NM 87801 (United States); Wright, Shelley A., E-mail: Chao-Wei.Tsai@jpl.nasa.gov [Dunlap Institute for Astronomy and Astrophysics, University of Toronto, Toronto, Ontario (Canada)

2013-10-20T23:59:59.000Z

474

Building Energy Software Tools Directory: Star Perfomer  

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

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

475

Kaon Condensation in a Neutron Star under Strong Magnetic Fields by Using the Modified Quark-meson Coupling Model  

E-Print Network [OSTI]

We have considered the antikaon condensation in a neutron star in the presence of strong magnetic fields by using the modified quark-meson coupling (MQMC) model. The structure of the neutron star is investigated with various magnetic fields and different kaon optical potentials, and the effects of the magnetic fields for kaon condensation is discussed. When employing strong magnetic fields inside a neutron star with hyperons and kaon condensation, the magnetic fields can cause the equation of state to be stiff; thus, a large maximum mass of the neutron star can be obtained.

C. Y. Ryu; S. W. Hong

2011-08-27T23:59:59.000Z

476

International Center for Advanced Renewable Energy  

E-Print Network [OSTI]

. . . . . . . . . . . . . . . . . 08 Consortium for Clean Coal Utilization . . . . . . . . . . . . . . . 09 Tyson Research Center

Subramanian, Venkat

477

Data Centers and Servers | Department of Energy  

Office of Environmental Management (EM)

Data Centers and Servers Data Centers and Servers Photo of the Green Data Center at the Research Support Facility. Data centers are one of the most energy-intensive building types,...

478

On the capture of dark matter by neutron stars  

E-Print Network [OSTI]

We calculate the number of dark matter particles that a neutron star accumulates over its lifetime as it rotates around the center of a galaxy, when the dark matter particle is a self-interacting boson but does not self-annihilate. We take into account dark matter interactions with baryonic matter and the time evolution of the dark matter sphere as it collapses within the neutron star. We show that dark matter self-interactions play an important role in the rapid accumulation of dark matter in the core of the neutron star. We consider the possibility of determining an exclusion region of the parameter space for dark matter mass and dark matter interaction cross sections based on the observation of old neutron stars with strong dark matter self-interactions. We show that for a dark matter density of $~10^3$ GeV/cm$^3$ and dark matter mass $m_\\chi$ less than approximately 10 GeV, there is a potential exclusion region for dark matter interactions with nucleons that is three orders of magnitude more stringent than without self-interactions. The potential exclusion region for dark matter self-interaction cross sections is many orders of magnitude stronger than the current Bullet Cluster limit. For example, for high dark matter density regions, we find that for $m_\\chi\\sim 10$ GeV when the dark matter interaction cross section with the nucleons ranges from $\\sigma_{\\chi n}\\sim 10^{-52}$ cm$^2$ to $10^{-57}$ cm$^2$, the dark matter self-interaction cross section limit is $\\sigma_{\\chi\\chi}ten orders of magnitude stronger than the Bullet Cluster limit.

Tolga Guver; Arif Emre Erkoca; Mary Hall Reno; Ina Sarcevic

2014-04-09T23:59:59.000Z

479

THE STAR FORMATION IN RADIO SURVEY: GBT 33 GHz OBSERVATIONS OF NEARBY GALAXY NUCLEI AND EXTRANUCLEAR STAR-FORMING REGIONS  

SciTech Connect (OSTI)

We present 33 GHz photometry of 103 galaxy nuclei and extranuclear star-forming complexes taken with the Green Bank Telescope as part of the Star Formation in Radio Survey. Among the sources without evidence for an active galactic nucleus, and also having lower frequency radio data, we find a median thermal fraction at 33 GHz of Almost-Equal-To 76% with a dispersion of Almost-Equal-To 24%. For all sources resolved on scales {approx}<0.5 kpc, the thermal fraction is even larger, being {approx}>90%. This suggests that the rest-frame 33 GHz emission provides a sensitive measure of the ionizing photon rate from young star-forming regions, thus making it a robust star formation rate (SFR) indicator. Taking the 33 GHz SFRs as a reference, we investigate other empirical calibrations relying on different combinations of warm 24 {mu}m dust, total infrared (IR; 8-1000 {mu}m), H{alpha} line, and far-UV continuum emission. The recipes derived here generally agree with others found in the literature, albeit with a large dispersion that most likely stems from a combination of effects. Comparing the 33 GHz to total IR flux ratios as a function of the radio spectral index, measured between 1.7 and 33 GHz, we find that the ratio increases as the radio spectral index flattens which does not appear to be a distance effect. Consequently, the ratio of non-thermal to total IR emission appears relatively constant, suggesting only moderate variations in the cosmic-ray electron injection spectrum and ratio of synchrotron to total cooling processes among star-forming complexes. Assuming that this trend solely arises from an increase in the thermal fraction sets a maximum on the scatter of the non-thermal spectral indices among the star-forming regions of {sigma}{sub {alpha}{sup N}{sup T}}{approx}<0.13.

Murphy, E. J. [Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101 (United States); Bremseth, J. [Department of Physics and Astronomy, Pomona College, Claremont, CA 91711 (United States); Mason, B. S.; Condon, J. J. [National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903 (United States); Schinnerer, E. [Max Planck Institut fuer Astronomie, Koenigstuhl 17, D-69117 Heidelberg (Germany); Aniano, G. [Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544 (United States); Armus, L. [Spitzer Science Center, California Institute of Technology, MC 314-6, Pasadena, CA 91125 (United States); Helou, G. [California Institute of Technology, MC 100-22, Pasadena, CA 91125 (United States); Turner, J. L. [Department of Physics and Astronomy, UCLA, Los Angeles, CA 90095 (United States); Jarrett, T. H., E-mail: emurphy@obs.carnegiescience.edu [Infrared Processing and Analysis Center, California Institute of Technology, MC 100-22, Pasadena, CA 91125 (United States)

2012-12-20T23:59:59.000Z

480

SWP Carbon Sequestration Training Center  

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

Training Center Presentation, Training Center Presentation, October 2010 SWP Carbon Sequestration Training Center Principal Investigators: New Mexico Tech, Andrew Campbell and Peter Mozley University of Utah, Brian McPherson Texas A&M University, Tarla Peterson SWP Training Center Presentation, October 2010 Background  Funded by DOE/NETL.  Purpose is to train more scientists and engineers for work in geological sequestration.  Three year grant.  Designed to be self sustaining. SWP Training Center Presentation, October 2010 Our goal is provide education about CCS at a variety of educational levels in order to promote a pipeline of future CCS scientists and engineers.  High School  K-12 Teachers  Undergraduate  Graduate  Professionals  Outreach SWP Training Center Presentation,

Note: This page contains sample records for the topic "difference star center" 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

Alternative Fuels Data Center: Biobutanol  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Biobutanol to someone Biobutanol to someone by E-mail Share Alternative Fuels Data Center: Biobutanol on Facebook Tweet about Alternative Fuels Data Center: Biobutanol on Twitter Bookmark Alternative Fuels Data Center: Biobutanol on Google Bookmark Alternative Fuels Data Center: Biobutanol on Delicious Rank Alternative Fuels Data Center: Biobutanol on Digg Find More places to share Alternative Fuels Data Center: Biobutanol on AddThis.com... More in this section... Biobutanol Drop-In Biofuels Methanol P-Series Renewable Natural Gas xTL Fuels Biobutanol Biobutanol is a 4-carbon alcohol (butyl alcohol) produced from the same feedstocks as ethanol including corn, sugar beets, and other biomass feedstocks. Butanol is generally used as an industrial solvent in products such as lacquers and enamels, but it also can be blended with other fuels

482

Alternative Fuels Data Center: Telework  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Telework to someone by Telework to someone by E-mail Share Alternative Fuels Data Center: Telework on Facebook Tweet about Alternative Fuels Data Center: Telework on Twitter Bookmark Alternative Fuels Data Center: Telework on Google Bookmark Alternative Fuels Data Center: Telework on Delicious Rank Alternative Fuels Data Center: Telework on Digg Find More places to share Alternative Fuels Data Center: Telework on AddThis.com... More in this section... Idle Reduction Parts & Equipment Maintenance Driving Behavior Fleet Rightsizing System Efficiency Ridesharing Mass Transit Active Transit Multi-Modal Transportation Telework Telework Photo of a woman working from home. Telework is a flexible work arrangement where employees work from home (telecommute) or attend conferences and meetings from their computer

483

Alternative Fuels Data Center: Biogas  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Biogas to someone by Biogas to someone by E-mail Share Alternative Fuels Data Center: Biogas on Facebook Tweet about Alternative Fuels Data Center: Biogas on Twitter Bookmark Alternative Fuels Data Center: Biogas on Google Bookmark Alternative Fuels Data Center: Biogas on Delicious Rank Alternative Fuels Data Center: Biogas on Digg Find More places to share Alternative Fuels Data Center: Biogas on AddThis.com... More in this section... Biobutanol Drop-In Biofuels Methanol P-Series Renewable Natural Gas xTL Fuels Renewable Natural Gas (Biogas) Biogas-also known as biomethane, swamp gas, landfill gas, or digester gas-is the gaseous product of anaerobic digestion (decomposition without oxygen) of organic matter. In addition to providing electricity and heat, biogas is useful as a vehicle fuel. When processed to purity standards,

484

Alternative Fuels Data Center: Methanol  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Methanol to someone by Methanol to someone by E-mail Share Alternative Fuels Data Center: Methanol on Facebook Tweet about Alternative Fuels Data Center: Methanol on Twitter Bookmark Alternative Fuels Data Center: Methanol on Google Bookmark Alternative Fuels Data Center: Methanol on Delicious Rank Alternative Fuels Data Center: Methanol on Digg Find More places to share Alternative Fuels Data Center: Methanol on AddThis.com... More in this section... Biobutanol Drop-In Biofuels Methanol P-Series Renewable Natural Gas xTL Fuels Methanol Methanol (CH3OH), also known as wood alcohol, is an alternative fuel under the Energy Policy Act of 1992. As an engine fuel, methanol has chemical and physical fuel properties similar to ethanol. Methanol use in vehicles has declined dramatically since the early 1990s, and automakers no longer

485

Alternative Fuels Data Center: Ridesharing  

Alternative Fuels and Advanced Vehicles Data Center [Office of Energy Efficiency and Renewable Energy (EERE)]

Ridesharing to someone Ridesharing to someone by E-mail Share Alternative Fuels Data Center: Ridesharing on Facebook Tweet about Alternative Fuels Data Center: Ridesharing on Twitter Bookmark Alternative Fuels Data Center: Ridesharing on Google Bookmark Alternative Fuels Data Center: Ridesharing on Delicious Rank Alternative Fuels Data Center: Ridesharing on Digg Find More places to share Alternative Fuels Data Center: Ridesharing on AddThis.com... More in this section... Idle Reduction Parts & Equipment Maintenance Driving Behavior Fleet Rightsizing System Efficiency Ridesharing Mass Transit Active Transit Multi-Modal Transportation Telework Ridesharing Photo of people car pooling. Rideshare programs help people share vehicles to commute together. Also known as carpooling, ridesharing conserves fuel and reduces vehicle

486

Build Your Business with ENERGY STAR  

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

Service and Product Providers: Service and Product Providers: Build Your Business with ENERGY STAR ® Let ENERGY STAR Be Your Market Advantage Look to ENERGY STAR to help you bring value to your customers and more sales to your organization. Service and Product Providers (SPPs) are integral in helping existing commercial buildings use energy more efficiently. Partnering with ENERGY STAR provides you with access to free tools and resources to help you devise and implement energy- efficient strategies that are right for your custo