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  1. Lone Star Transmission LLC | Open Energy Information

    Open Energy Info (EERE)

    Transmission LLC Jump to: navigation, search Name: Lone Star Transmission LLC Place: Juno Beach, Florida Zip: 33408 Product: Wholly owned subsidiary of FPL Energy, developing...

  2. Clean Cities: Lone Star Clean Fuels Alliance (Central Texas)...

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

    Lone Star Clean Fuels Alliance (Central Texas) Coalition The Lone Star Clean Fuels Alliance (Central Texas) coalition works with vehicle fleets, fuel providers, community leaders,...

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

    Open Energy Info (EERE)

    Q2) Wind Farm Jump to: navigation, search Name Lone Star I (Q2) Wind Farm Facility Lone Star I (Q2) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

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

    Open Energy Info (EERE)

    Q3) Wind Farm Jump to: navigation, search Name Lone Star I (Q3) Wind Farm Facility Lone Star I (Q3) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  5. Lone Star Wind Alliance LSWA | Open Energy Information

    Open Energy Info (EERE)

    Wind Alliance LSWA Jump to: navigation, search Name: Lone Star Wind Alliance (LSWA) Place: Houston, Texas Sector: Wind energy Product: Texas-based research centres, focusing on...

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

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Lone Star II (1Q08) Wind Farm Facility Lone Star II (1Q08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

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

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Lone Star II (4Q07) Wind Farm Facility Lone Star II (4Q07) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

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

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Lone Star I (4Q07) Wind Farm Facility Lone Star I (4Q07) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  9. Lone Star II (2Q08) Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Lone Star II (2Q08) Wind Farm Facility Lone Star II (2Q08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  10. STAR

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

    STAR Basics The basics of STAR computing at PDSF. Read More » Local STAR Libraries These are the STAR libraries built locally at PDSF. Read More » STAR Test Environment The instructions describe how to set up the STAR environment independent of the production environment. Read More » Data Management STAR data transfer, HPSS usage, databases and job scheduler. Read More » File Systems STAR has space on 7 elizas... Read More » Shifter image of STAR SL13a WORK-IN PROGRESS A demonstrator STAR

  11. Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides

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

    Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print "Ferroelectricity," by analogy to ferromagnetism, is defined as the presence of spontaneous electrical polarization in a material, often arising from distortions in the material's crystal structure. In oxides of the metals lead and bismuth, such distortions were for many years attributed to the existence of "lone pair" electrons: pairs of chemically inert, nonbonding valence electrons in hybrid orbitals

  12. Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides

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

    Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print Wednesday, 28 February 2007 00:00 "Ferroelectricity," by analogy to ferromagnetism, is defined as the presence of spontaneous electrical polarization in a material, often arising from distortions in the material's crystal structure. In oxides of the metals lead and bismuth, such distortions were for many years attributed to the existence of

  13. Calloway Makes Sweet 16, Lone Oak Competes in DOE National Science Bowl |

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

    Department of Energy Calloway Makes Sweet 16, Lone Oak Competes in DOE National Science Bowl Calloway Makes Sweet 16, Lone Oak Competes in DOE National Science Bowl April 29, 2014 - 2:43pm Addthis Calloway County High School's Mia Beth Morehead, coach, Landon Fike, Cody Bergman, Sam Morehead, Josh Betts, and Hudson Elliott from Murray, Kentucky, pose for a team photo during the 2014 National Science Bowl competition, Thursday, April 24, 2014, in Washington, DC. Calloway County High School's

  14. Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides

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

    Beyond the Lone-Pair Model for Structurally Distorted Metal Oxides Print "Ferroelectricity," by analogy to ferromagnetism, is defined as the presence of spontaneous electrical polarization in a material, often arising from distortions in the material's crystal structure. In oxides of the metals lead and bismuth, such distortions were for many years attributed to the existence of "lone pair" electrons: pairs of chemically inert, nonbonding valence electrons in hybrid orbitals

  15. 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...

  16. ENERGY STAR

    SciTech Connect (OSTI)

    2011-12-16

    ENERGY STAR is a voluntary labeling and recognition program that seeks to accelerate the adoption of clean and efficient domestic energy technologies.

  17. STARS no star on Kauai

    SciTech Connect (OSTI)

    Jones, M.

    1993-04-01

    The island of Kuai, home to the Pacific Missile Range Facility, is preparing for the first of a series of Star Wars rocket launches expected to begin early this year. The Strategic Defense Initiative plans 40 launches of the Stategic Target System (STARS) over a 10-year period. The focus of the tests appears to be weapons and sensors designed to combat multiple-warhead ICBMs, which will be banned under the START II Treaty that was signed in January. The focus of this article is to express the dubious value of testing the STARS at a time when their application will not be an anticipated problem.

  18. Chameleon stars

    SciTech Connect (OSTI)

    Dzhunushaliev, Vladimir; Folomeev, Vladimir; Singleton, Douglas

    2011-10-15

    We consider a gravitating spherically symmetric configuration consisting of a scalar field nonminimally coupled to ordinary matter in the form of a perfect fluid. For this system we find static, regular, asymptotically flat solutions for both relativistic and nonrelativistic cases. It is shown that the presence of the nonminimal interaction leads to substantial changes both in the radial matter distribution of the star and in the star's total mass. A simple stability test indicates that, for the choice of parameters used in the paper, the solutions are unstable.

  19. Star Power

    SciTech Connect (OSTI)

    2014-10-17

    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.

  20. Star Power

    ScienceCinema (OSTI)

    None

    2014-11-18

    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.

  1. Kepler-424 b: A 'lonely' hot Jupiter that found A companion

    SciTech Connect (OSTI)

    Endl, Michael; Caldwell, Douglas A.; Barclay, Thomas; Huber, Daniel; Havel, Mathieu; Howell, Steve B.; Quintana, Elisa; Isaacson, Howard; Buchhave, Lars A.; Brugamyer, Erik; Robertson, Paul; Cochran, William D.; MacQueen, Phillip J.; Lucas, Phillip; Fischer, Debra; Ciardi, David R.

    2014-11-10

    Hot Jupiter systems provide unique observational constraints for migration models in multiple systems and binaries. We report on the discovery of the Kepler-424 (KOI-214) two-planet system, which consists of a transiting hot Jupiter (Kepler-424b) in a 3.31 day orbit accompanied by a more massive outer companion in an eccentric (e = 0.3) 223 day orbit. The outer giant planet, Kepler-424c, is not detected transiting the host star. The masses of both planets and the orbital parameters for the second planet were determined using precise radial velocity (RV) measurements from the Hobby-Eberly Telescope (HET) and its High Resolution Spectrograph (HRS). In stark contrast to smaller planets, hot Jupiters are predominantly found to be lacking any nearby additional planets; they appear to be {sup l}onely{sup .} This might be a consequence of these systems having a highly dynamical past. The Kepler-424 planetary system has a hot Jupiter in a multiple system, similar to ? Andromedae. We also present our results for Kepler-422 (KOI-22), Kepler-77 (KOI-127), Kepler-43 (KOI-135), and Kepler-423 (KOI-183). These results are based on spectroscopic data collected with the Nordic Optical Telescope (NOT), the Keck 1 telescope, and HET. For all systems, we rule out false positives based on various follow-up observations, confirming the planetary nature of these companions. We performed a comparison with planetary evolutionary models which indicate that these five hot Jupiters have heavy element contents between 20 and 120 M {sub ?}.

  2. Maintaining STAR - Hanford Site

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

    Getting Started Maintaining STAR VPP CampaignPosters VPP Tools VPP Presentations VPP Awareness VPP Communications VPP Conferences Maintaining STAR Email Email Page | Print Print...

  3. Energy Star Appliances

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

    Updates and News ENERGY STAR appliances have been a successful program offer for many BPA utility customers and are expected to continue. However, as ENERGY STAR specifications...

  4. Shooting Star | Open Energy Information

    Open Energy Info (EERE)

    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...

  5. STAR Test Environment

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

    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

  6. ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems...

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

    ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems June 21, 2016 1:00PM to 2:00PM EDT Hosted by ...

  7. ENERGY STAR | Open Energy Information

    Open Energy Info (EERE)

    ENERGY STAR Jump to: navigation, search Logo: ENERGY STAR Name: ENERGY STAR Year Founded: 1992 Website: www.energystar.govindex.cfm?c References: About ENERGY STAR1 Contents 1...

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

    SciTech Connect (OSTI)

    Wangoh, L.; Quackenbush, N. F.; Marley, P. M.; Banerjee, S.; Sallis, S.; Fischer, D. A.; Woicik, J. C.; Piper, L. F. J.

    2014-05-05

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

  9. ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems...

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

    ENERGY STAR and Green Building Rating Systems ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems October 13, 2015 2:00PM to 3:00PM EDT Online Hosted by the U.S....

  10. 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:...

  11. Star Biomass | Open Energy Information

    Open Energy Info (EERE)

    Biomass Jump to: navigation, search Name: Star Biomass Place: India Sector: Biomass Product: Plans to set up biomass projects in Rajasthan. References: Star Biomass1 This article...

  12. STAR-Running on Carver

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

    STAR-Running on Carver STAR-Running on Carver STAR software has been copied from the usual installation on /common on PDSF to /project/projectdirs/star/common. At this point the installation is simply intended for testing and not all libraries are in place - for now SL10k, SL11b and SL11c are available with root/5.22.00 and a copy of $OPTSTAR and cernlib. An example of how to setup the STAR software on Carver is in /project/projectdirs/star/starenv. To use it simply source star_setup. This

  13. ENERGY STAR Product Rebates

    Broader source: Energy.gov [DOE]

    When mail-in rebates are active, as a general rule, all appliances must be ENERGY STAR rated; however, additional requirements may apply to different types of appliances. Rebate requests must...

  14. Cold Hybrid Star Properties

    SciTech Connect (OSTI)

    Moshfegh, H. R.; Darehmoradi, M.; Mojarrad, M. Ghazanfari

    2011-10-28

    Properties of neutron stars with quark core are investigated. The equation of state of hadronic matter is calculated using Myers and Swiatecki two nucleon interaction within Thomas-Fermi semiclassical approximation (TF). For quark matter we employ The MIT bag model with constant and density dependent bag parameter. With use of the obtained equation of states we have calculated mass-radius relation of such hybrid stars.

  15. STAR Facility Tritium Accountancy

    SciTech Connect (OSTI)

    R. J. Pawelko; J. P. Sharpe; B. J. Denny

    2007-09-01

    The Safety and Tritium Applied Research (STAR) facility has been established to provide a laboratory infrastructure for the fusion community to study tritium science associated with the development of safe fusion energy and other technologies. STAR is a radiological facility with an administrative total tritium inventory limit of 1.5g (14,429 Ci) [1]. Research studies with moderate tritium quantities and various radionuclides are performed in STAR. Successful operation of the STAR facility requires the ability to receive, inventory, store, dispense tritium to experiments, and to dispose of tritiated waste while accurately monitoring the tritium inventory in the facility. This paper describes tritium accountancy in the STAR facility. A primary accountancy instrument is the tritium Storage and Assay System (SAS): a system designed to receive, assay, store, and dispense tritium to experiments. Presented are the methods used to calibrate and operate the SAS. Accountancy processes utilizing the Tritium Cleanup System (TCS), and the Stack Tritium Monitoring System (STMS) are also discussed. Also presented are the equations used to quantify the amount of tritium being received into the facility, transferred to experiments, and removed from the facility. Finally, the STAR tritium accountability database is discussed.

  16. STAR facility tritium accountancy

    SciTech Connect (OSTI)

    Pawelko, R. J.; Sharpe, J. P.; Denny, B. J.

    2008-07-15

    The Safety and Tritium Applied Research (STAR) facility has been established to provide a laboratory infrastructure for the fusion community to study tritium science associated with the development of safe fusion energy and other technologies. STAR is a radiological facility with an administrative total tritium inventory limit of 1.5 g (14,429 Ci) [1]. Research studies with moderate tritium quantities and various radionuclides are performed in STAR. Successful operation of the STAR facility requires the ability to receive, inventory, store, dispense tritium to experiments, and to dispose of tritiated waste while accurately monitoring the tritium inventory in the facility. This paper describes tritium accountancy in the STAR facility. A primary accountancy instrument is the tritium Storage and Assay System (SAS): a system designed to receive, assay, store, and dispense tritium to experiments. Presented are the methods used to calibrate and operate the SAS. Accountancy processes utilizing the Tritium Cleanup System (TCS), and the Stack Tritium Monitoring System (STMS) are also discussed. Also presented are the equations used to quantify the amount of tritium being received into the facility, transferred to experiments, and removed from the facility. Finally, the STAR tritium accountability database is discussed. (authors)

  17. Blue Star Energy Services | Open Energy Information

    Open Energy Info (EERE)

    Blue Star Energy Services (Redirected from BlueStar) Jump to: navigation, search Name: Blue Star Energy Services Place: Illinois Phone Number: 866-258-3782 Website:...

  18. Wave Star Energy | Open Energy Information

    Open Energy Info (EERE)

    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 Energy1...

  19. Silver Star Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Star Wind Farm Jump to: navigation, search Name Silver Star Wind Farm Facility Silver Star Sector Wind energy Facility Type Commercial Scale Wind Facility Status In Service Owner...

  20. 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...

  1. ENERGY STAR Webinar: How to Apply for the ENERGY STAR

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) is hosting a webinar on how to apply for ENERGY STAR certification in Portfolio Manager. Understand the value of the ENERGY STAR certification, see...

  2. ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems...

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

    2:00PM to 3:00PM EDT ENERGY STAR Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will help attendees how to use EPA tools and resources to...

  3. General Relativity&Compact Stars

    SciTech Connect (OSTI)

    Glendenning, Norman K.

    2005-08-16

    Compact stars--broadly grouped as neutron stars and white dwarfs--are the ashes of luminous stars. One or the other is the fate that awaits the cores of most stars after a lifetime of tens to thousands of millions of years. Whichever of these objects is formed at the end of the life of a particular luminous star, the compact object will live in many respects unchanged from the state in which it was formed. Neutron stars themselves can take several forms--hyperon, hybrid, or strange quark star. Likewise white dwarfs take different forms though only in the dominant nuclear species. A black hole is probably the fate of the most massive stars, an inaccessible region of spacetime into which the entire star, ashes and all, falls at the end of the luminous phase. Neutron stars are the smallest, densest stars known. Like all stars, neutron stars rotate--some as many as a few hundred times a second. A star rotating at such a rate will experience an enormous centrifugal force that must be balanced by gravity or else it will be ripped apart. The balance of the two forces informs us of the lower limit on the stellar density. Neutron stars are 10{sup 14} times denser than Earth. Some neutron stars are in binary orbit with a companion. Application of orbital mechanics allows an assessment of masses in some cases. The mass of a neutron star is typically 1.5 solar masses. They can therefore infer their radii: about ten kilometers. Into such a small object, the entire mass of our sun and more, is compressed.

  4. A Star on Earth

    ScienceCinema (OSTI)

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

    2014-06-06

    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.

  5. Synthetic guide star generation

    SciTech Connect (OSTI)

    Payne, Stephen A; Page, Ralph H; Ebbers, Christopher A; Beach, Raymond J

    2008-06-10

    A system for assisting in observing a celestial object and providing synthetic guide star generation. A lasing system provides radiation at a frequency at or near 938 nm and radiation at a frequency at or near 1583 nm. The lasing system includes a fiber laser operating between 880 nm and 960 nm and a fiber laser operating between 1524 nm and 1650 nm. A frequency-conversion system mixes the radiation and generates light at a frequency at or near 589 nm. A system directs the light at a frequency at or near 589 nm toward the celestial object and provides synthetic guide star generation.

  6. A Star on Earth

    SciTech Connect (OSTI)

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

    2014-03-05

    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.

  7. Synthetic guide star generation

    DOE Patents [OSTI]

    Payne, Stephen A.; Page, Ralph H.; Ebbers, Christopher A.; Beach, Raymond J.

    2004-03-09

    A system for assisting in observing a celestial object and providing synthetic guide star generation. A lasing system provides radiation at a frequency at or near 938 nm and radiation at a frequency at or near 1583 nm. The lasing system includes a fiber laser operating between 880 nm and 960 nm and a fiber laser operating between 1524 nm and 1650 nm. A frequency-conversion system mixes the radiation and generates light at a frequency at or near 589 nm. A system directs the light at a frequency at or near 589 nm toward the celestial object and provides synthetic guide star generation.

  8. ENERGY STAR Webinar: How to Apply for ENERGY STAR

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) ENERGY STAR is hosting a webinar on how to apply 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 help your property get from application to award.

  9. CFL Manufacturers: ENERGY STAR Letters

    Broader source: Energy.gov [DOE]

    DOE issued letters to 25 manufacturers of compact fluorescent lamps (CFLs) involving various models after PEARL Cycle 9 testing indicated that the models do not meet the ENERGY STAR specification and, therefore, are disqualified from the ENERGY STAR Program.

  10. Energy Star | Open Energy Information

    Open Energy Info (EERE)

    Energy 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,...

  11. Neutron Star Science with the NuSTAR

    SciTech Connect (OSTI)

    Vogel, J. K.

    2015-10-16

    The Nuclear Spectroscopic Telescope Array (NuSTAR), launched in June 2012, helped scientists obtain for the first time a sensitive high-­energy X-­ray map of the sky with extraordinary resolution. This pioneering telescope has aided in the understanding of how stars explode and neutron stars are born. LLNL is a founding member of the NuSTAR project, with key personnel on its optics and science team. We used NuSTAR to observe and analyze the observations of different neutron star classes identified in the last decade that are still poorly understood. These studies not only help to comprehend newly discovered astrophysical phenomena and emission processes for members of the neutron star family, but also expand the utility of such observations for addressing broader questions in astrophysics and other physics disciplines. For example, neutron stars provide an excellent laboratory to study exotic and extreme phenomena, such as the equation of state of the densest matter known, the behavior of matter in extreme magnetic fields, and the effects of general relativity. At the same time, knowing their accurate populations has profound implications for understanding the life cycle of massive stars, star collapse, and overall galactic evolution.

  12. Local STAR Libraries

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

    Local STAR Libraries Local STAR Libraries The libraries listed below are built locally at PDSF and are available under the chos environment sl53. The 32sl44 chos environment has been retire but the libraries are still listed for reference. Version Tag ROOT Version Status Mode Date Comment SL12b (new) SL12b 5.22.00 built debug 4/17/12 SL5.3 SL12a SL12a 5.22.00 built debug 3/14/12 SL5.3 SL11e SL11e 5.22.00 built debug 11/30/11 SL5.3 SL11d (pro) SL11d 5.22.00 built debug 8/1/11 SL5.3 SL11c SL11c_1

  13. ENERGY STAR Webinar: How to Apply for the ENERGY STAR

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) is hosting a webinar on how to apply for ENERGY STAR certification in Portfolio Manager.

  14. EXTENDED SCHMIDT LAW: ROLE OF EXISTING STARS IN CURRENT STAR...

    Office of Scientific and Technical Information (OSTI)

    Country of Publication: United States Language: English Subject: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DENSITY; GALACTIC EVOLUTION; MASS; STARS; SURFACES EVOLUTION; PHYSICAL ...

  15. WIPP Hazardous Waste Permit - Class 1* (star) Modifications

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

    * (star) Modifications Submitted for NMED Approval

  16. STAR Teaching Program Application Period

    Broader source: Energy.gov [DOE]

    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...

  17. Streamlining ENERGY STAR Appliance Testing

    Broader source: Energy.gov [DOE]

    To save taxpayer dollars and help lower the costs of innovative energy-efficient technologies, the Energy Department is streamlining ENERGY STAR testing for appliances.

  18. ENERGY STAR Webinar: How to Apply for the ENERGY STAR

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) is hosting a webinar on how to apply 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 help your property get from application to award.

  19. TRIGGERED STAR FORMATION SURROUNDING WOLF-RAYET STAR HD 211853

    SciTech Connect (OSTI)

    Liu Tie; Wu Yuefang; Zhang Huawei; Qin Shengli

    2012-05-20

    The environment surrounding Wolf-Rayet (W-R) star HD 211853 is studied in molecular, infrared, as well as radio, and H I emission. The molecular ring consists of well-separated cores, which have a volume density of 10{sup 3} cm{sup -3} and kinematic temperature {approx}20 K. Most of the cores are under gravitational collapse due to external pressure from the surrounding ionized gas. From the spectral energy distribution modeling toward the young stellar objects, the sequential star formation is revealed on a large scale in space spreading from the W-R star to the molecular ring. A small-scale sequential star formation is revealed toward core 'A', which harbors a very young star cluster. Triggered star formations are thus suggested. The presence of the photodissociation region, the fragmentation of the molecular ring, the collapse of the cores, and the large-scale sequential star formation indicate that the 'collect and collapse' process functions in this region. The star-forming activities in core 'A' seem to be affected by the 'radiation-driven implosion' process.

  20. StarTex Power | Open Energy Information

    Open Energy Info (EERE)

    StarTex Power Place: Texas Website: www.startexpower.com Twitter: @StarTexPower Facebook: https:www.facebook.comStarTexPower Outage Hotline: 1-866-917-8271 References: EIA...

  1. MagStar Technologies | Open Energy Information

    Open Energy Info (EERE)

    MagStar Technologies Jump to: navigation, search Name: MagStar Technologies Place: Hopkins, MN Information About Partnership with NREL Partnership with NREL Yes Partnership Type...

  2. StarSolar Corporation | Open Energy Information

    Open Energy Info (EERE)

    StarSolar Corporation Jump to: navigation, search Name: StarSolar Corporation Place: Cambridge, Massachusetts Product: Developing a nanostructured 'photonic crystal' PV cell with...

  3. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will introduce and demonstrate the EPA's ENERGY STAR Portfolio Manager tool.

  4. 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,...

  5. Five Star Technologies | Open Energy Information

    Open Energy Info (EERE)

    Star Technologies Jump to: navigation, search Name: Five Star Technologies Place: Independence, Ohio Zip: 44131 Sector: Solar Product: US manufacturer of inks and pastes for the...

  6. Star Point Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Point Wind Farm Jump to: navigation, search Name Star Point Wind Farm Facility Star Point Wind Farm Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  7. EPA ENERGY STAR Webcast: Value of ENERGY STAR Certification

    Broader source: Energy.gov [DOE]

    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...

  8. EPA ENERGY STAR Webinar: ENERGY STAR Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    Continue to learn about EPA’s 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...

  9. A Heavy Flavor Tracker for STAR

    SciTech Connect (OSTI)

    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.

    2005-03-14

    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.

  10. ENERGY STAR Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  11. ENERGY STAR Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    Continue to learn about EPA’s 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;...

  12. Green Star Products Inc GSPI | Open Energy Information

    Open Energy Info (EERE)

    Star Products Inc GSPI Jump to: navigation, search Name: Green Star Products Inc (GSPI) Place: Chula Vista, California Zip: 91911 Product: Green Star is building two 200-hectare...

  13. Home Performance with ENERGY STAR

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

    Home Performance with ENERGY STAR 2014 Building Technologies Office Peer Review Ely Jacobsohn, Ely.Jacobsohn@ee.doe.gov Home Performance with ENERGY STAR Program Manager Project Summary: Home Performance with ENERGY STAR Timeline: Key Partners: Start date: 2001 Planned end date: Ongoing Key Milestones 1. Program Action Plan: Jan ͛13 2. D̯χ̯ D̯ν·̼Ϊ̯ι͇ν΄ D͋̽ ·13 3. ͜Σ͇Ϣνχιϴ ΡΪιΙ GιΪϢζ΄ ̯ͧΣ ·14 4. Sponsor Guide (ϭ1΅5)΄ ͱ̯ι ·14 Budget: Total DOE $ to

  14. Neutron skins and neutron stars

    SciTech Connect (OSTI)

    Piekarewicz, J.

    2013-11-07

    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.

  15. ENERGY STAR Webinar: ENERGY STAR and Green Building Rating Systems

    Office of Energy Efficiency and Renewable Energy (EERE)

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will help attendees how to use EPA tools and resources to help meet requirements for green building rating systems, such as the U.S. Green Building Council's Leadership in Energy and Environmental Design (LEED), the Green Globes system, and others.

  16. Cold quark matter in compact stars

    SciTech Connect (OSTI)

    Franzon, B.; Fogaca, D. A.; Navarra, F. S.; Horvath, J. E.

    2013-03-25

    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.

  17. Residential Energy Star Appliance Rebate Program

    Broader source: Energy.gov [DOE]

    Refrigerators and freezers must be installed in homes within the PGE or Pacific Power service territory to qualify.  All Energy Star freezers qualify for the $35 rebate.  Only Energy Star...

  18. 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.

  19. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will introduce and demonstrate the EPA's ENERGY STAR Portfolio Manager tool. Attendees will learn how to...

  20. Haier: ENERGY STAR Referral (ESA408J)

    Office of Energy Efficiency and Renewable Energy (EERE)

    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.

  1. Alliance Star Energy LLC | Open Energy Information

    Open Energy Info (EERE)

    Star Energy LLC Jump to: navigation, search Name: Alliance Star Energy LLC Place: California Phone Number: (619) 574-0527 Outage Hotline: (619) 574-0527 References: EIA Form...

  2. K Star Solar | Open Energy Information

    Open Energy Info (EERE)

    Solar Jump to: navigation, search Name: K-Star Solar Place: New York Product: Long Island-based PV systems installer. References: K-Star Solar1 This article is a stub. You can...

  3. The nuclear physics of neutron stars

    SciTech Connect (OSTI)

    Piekarewicz, J.

    2014-05-09

    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.

  4. NuSTAR: Nuclear Spectroscopic Telescope Array

    ScienceCinema (OSTI)

    Craig, Bill

    2014-06-24

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

  5. NuSTAR: Nuclear Spectroscopic Telescope Array

    SciTech Connect (OSTI)

    Craig, Bill

    2012-06-13

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

  6. ENERGY STAR Webinar: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    This webinar continues on the U.S. Environmental Protection Agency's (EPA's) new ENERGY STAR Portfolio Manager tool.

  7. LoanSTAR Revolving Loan Program

    Broader source: Energy.gov [DOE]

    Provides an overview of the LoanStar Revolving Loan program. Author: Texas State Energy Conservation Office

  8. Hot Jupiters and cool stars

    SciTech Connect (OSTI)

    Villaver, Eva; Mustill, Alexander J.; Livio, Mario; Siess, Lionel

    2014-10-10

    Close-in planets are in jeopardy, as their host stars evolve off the main sequence (MS) to the subgiant and red giant phases. In this paper, we explore the influences of the stellar mass (in the range 1.5-2 M {sub ☉}), mass-loss prescription, planet mass (from Neptune up to 10 Jupiter masses), and eccentricity on the orbital evolution of planets as their parent stars evolve to become subgiants and red giants. We find that planet engulfment along the red giant branch is not very sensitive to the stellar mass or mass-loss rates adopted in the calculations, but quite sensitive to the planetary mass. The range of initial separations for planet engulfment increases with decreasing mass-loss rates or stellar masses and increasing planetary masses. Regarding the planet's orbital eccentricity, we find that as the star evolves into the red giant phase, stellar tides start to dominate over planetary tides. As a consequence, a transient population of moderately eccentric close-in Jovian planets is created that otherwise would have been expected to be absent from MS stars. We find that very eccentric and distant planets do not experience much eccentricity decay, and that planet engulfment is primarily determined by the pericenter distance and the maximum stellar radius.

  9. Shifter image of STAR SL13a

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

    Shifter image of STAR SL13a Shifter image of STAR SL13a WORK-IN PROGRESS A demonstrator STAR Shifter image is available for testing at Edison. At this time there is only one STAR image available for starver=SL13a. To deploy it on a single 32 core Cori node for 30 minutes execute the following sequence of commands (marked in bold) /* login to Edison, keep graphics port open */ my-laptop$ ssh -A -X edison.nersc.gov /* load needed module */ edison06:~>$ module load shifter /* verify you see STAR

  10. The mass spectrum of the first stars

    SciTech Connect (OSTI)

    Susa, Hajime; Tominaga, Nozomu; Hasegawa, Kenji

    2014-09-01

    We perform cosmological hydrodynamics simulations with non-equilibrium primordial chemistry to obtain 59 minihalos that host first stars. The obtained minihalos are used as the initial conditions of local three-dimensional radiation hydrodynamics simulations to investigate the formation of the first stars. We find that two-thirds of the minihalos host multiple stars, while the other third has single stars. The mass of the stars found in our simulations are in the range of 1 M {sub ☉} ≲ M ≲ 300 M {sub ☉}, peaking at several× 10 M {sub ☉}. Most of the very massive stars of ≳ 140 M {sub ☉} are born as single stars, although not all of the single stars are very massive. We also find a few stars of ≲ 1 M {sub ☉} that are kicked by the gravitational three body interactions to the position distant from the center of mass. The frequency that a star forming minihalo contains a binary system is ∼50%. We also investigate the abundance pattern of the stellar remnants by summing up the contributions from the first stars in the simulations. Consequently, the pattern is compatible with that of the low metallicity damped Lyα systems or the extremely metal-poor (EMP) stars, if the mass spectrum obtained in our experiment is shifted to the low mass side by 0.2 dex. If we consider the case that an EMP star is born in the remnant of the individual minihalo without mixing with others, the chemical signature of the pair instability supernova is more prominent, because most of them are born as single stars.

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

    SciTech Connect (OSTI)

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

    2005-06-01

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

  12. Storage and Assay of Tritium in STAR

    SciTech Connect (OSTI)

    Longhurst, Glen R.; Anderl, Robert A.; Pawelko, Robert J.; Stoots, Carl J.

    2005-07-15

    The Safety and Tritium Applied Research (STAR) facility at the Idaho National Engineering and Environmental Laboratory (INEEL) is currently being commissioned to investigate tritium-related safety questions for fusion and other technologies. The tritium inventory for the STAR facility will be maintained below 1.5 g to avoid the need for STAR to be classified as a Category 3 nuclear facility. A key capability in successful operation of the STAR facility is the ability to receive, inventory, and dispense tritium to the various experiments underway there. The system central to that function is the Tritium Storage and Assay System (SAS).The SAS has four major functions: (1) receiving and holding tritium, (2) assaying, (3) dispensing, and (4) purifying hydrogen isotopes from non-hydrogen species.This paper describes the design and operation of the STAR SAS and the procedures used for tritium accountancy in the STAR facility.

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

    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...

  14. EPA ENERGY STAR Webinar: 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...

  15. Home Performance with ENERGY STAR-- Webinar Slides

    Broader source: Energy.gov [DOE]

    "Existing Homes Efficiency – If You Want BetterBuildings – Go with Home Performance with ENERGY STAR," webinar slides from the U.S. Department of Energy.

  16. Rapid cooling and structure of neutron stars

    SciTech Connect (OSTI)

    Van Riper, K.A.; Lattimer, J.M.

    1992-07-01

    This report discusses the following topics on neutron stars: direct URCA neutrino emission; thermal evolution models; analytic model for diffusion through the crust; and core superfluidity. (LSP).

  17. Rapid cooling and structure of neutron stars

    SciTech Connect (OSTI)

    Van Riper, K.A. ); Lattimer, J.M. . Dept. of Earth and Space Sciences)

    1992-01-01

    This report discusses the following topics on neutron stars: direct URCA neutrino emission; thermal evolution models; analytic model for diffusion through the crust; and core superfluidity. (LSP).

  18. Energy Star Rebate Finder | Open Energy Information

    Open Energy Info (EERE)

    Rebate Finder Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Energy Star Rebate Finder AgencyCompany Organization: United States Environmental Protection Agency...

  19. William Fowler and Elements in the Stars

    Office of Scientific and Technical Information (OSTI)

    ... Integrated Flux Distributions in Neutron Capture in Stars, DOE Technical Report, September 23, 1965 Helium (3) Rich Solar Flares, DOE Technical Report, May 3, 1977 Top Additional ...

  20. Reading Municipal Light Department - Residential Energy Star...

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

    Pumps Air conditioners Programmable Thermostats Other EE Maximum Rebate One rebate per Energy Star appliance or two rebates on the purchase of programmable thermostats Program...

  1. Star Energy Systems | Open Energy Information

    Open Energy Info (EERE)

    Systems Jump to: navigation, search Name: Star Energy Systems Place: Ahmedabad, Gujarat, India Zip: 380 009 Sector: Solar Product: Solar PV product distributor. Coordinates:...

  2. Green Star Alternative Energy | Open Energy Information

    Open Energy Info (EERE)

    Alternative Energy Jump to: navigation, search Name: Green Star Alternative Energy Place: San Diego, California Zip: 92108 Sector: Wind energy Product: A US-based wind energy...

  3. Blue Star Energy Services | Open Energy Information

    Open Energy Info (EERE)

    Services Jump to: navigation, search Name: Blue Star Energy Services Place: Illinois Phone Number: 866-258-3782 Website: www.aepenergy.com Twitter: @aepenergy Facebook: https:...

  4. Star, Idaho: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Star, Idaho: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 43.6921071, -116.4934631 Show Map Loading map... "minzoom":false,"mappingservice":...

  5. Green Star Energy LLC | Open Energy Information

    Open Energy Info (EERE)

    LLC Jump to: navigation, search Name: Green Star Energy LLC Place: Houston, Texas Zip: 77002 Product: Houston-based producer of sugar cane processed ethanol, with additional...

  6. RegenaStar | Open Energy Information

    Open Energy Info (EERE)

    navigation, search Name: RegenaStar Place: Pune, Maharashtra, India Product: Pune-based joint venture between Regenatec and Cleanstar that focuses on jatropha cultivation for...

  7. TURBOVELOCITY STARS: KICKS RESULTING FROM THE TIDAL DISRUPTION OF SOLITARY STARS

    SciTech Connect (OSTI)

    Manukian, Haik; Guillochon, James; Ramirez-Ruiz, Enrico; O'Leary, Ryan M.

    2013-07-10

    The centers of most known galaxies host supermassive black holes (SMBHs). In orbit around these black holes are a centrally concentrated distribution of stars, both in single and in binary systems. Occasionally, these stars are perturbed onto orbits that bring them close to the SMBH. If the star is in a binary system, the three-body interaction with the SMBH can lead to large changes in orbital energy, depositing one of the two stars on a tightly-bound orbit, and its companion into a hyperbolic orbit that may escape the galaxy. In this Letter, we show that the disruption of solitary stars can also lead to large positive increases in orbital energy. The kick velocity depends on the amount of mass the star loses at pericenter, but not on the ratio of black hole to stellar mass, and are at most the star's own escape velocity. We find that these kicks are usually too small to result in the ejection of stars from the Milky Way, but can eject the stars from the black hole's sphere of influence, reducing their probability of being disrupted again. We estimate that {approx} 10{sup 5} stars, {approx} 1% of all stars within 10 pc of the galactic center, are likely to have had mass removed by the central black hole through tidal interaction, and speculate that these 'turbovelocity' stars will at first be redder, but eventually bluer, and always brighter than their unharassed peers.

  8. THE GALEX NEARBY YOUNG-STAR SURVEY

    SciTech Connect (OSTI)

    Rodriguez, David R.; Faherty, Jacqueline K.; Zuckerman, B.; Kastner, Joel H.; Bessell, M. S.; Murphy, Simon J.

    2013-09-10

    We describe a method that exploits data from the Galaxy Evolution Explorer (GALEX) ultraviolet and Wide-field Infrared Survey Explorer and Two Micron All Sky Survey infrared source catalogs, combined with proper motions and empirical pre-main sequence isochrones, to identify candidate nearby, young, low-mass stars. Applying our method across the full GALEX-covered sky, we identify 2031 mostly M-type stars that, for an assumed age of 10 (100) Myr, all lie within {approx}150 ({approx}90) pc of Earth. The distribution of M spectral subclasses among these {approx}2000 candidate young stars peaks sharply in the range M3-M4; these subtypes constitute 50% of the sample, consistent with studies of the M star population in the immediate solar neighborhood. We focus on a subset of 58 of these candidate young M stars in the vicinity of the Tucana-Horologium association. Only 20 of these 58 candidates were detected in the ROSAT All-Sky X-ray Survey-reflecting the greater sensitivity of GALEX for the purposes of identifying active nearby, young stars, particularly for stars of type M4 and later. Based on statistical analysis of the kinematics and/or spectroscopic followup of these 58 M stars, we find that 50% (29 stars) indeed have properties consistent with Tuc-Hor membership, while 12 are potential new members of the Columba association, and 2 may be AB Dor moving group members. Hence, {approx}75% of our initial subsample of 58 candidates are likely members of young (age {approx} 10-40 Myr) stellar moving groups within 100 pc, verifying that the stellar color- and kinematics-based selection algorithms described here can be used to efficiently isolate nearby, young, low-mass objects from among the field star population. Future studies will focus on characterizing additional subsamples selected from among this list of candidate nearby, young M stars.

  9. MHK Technologies/WaveStar | Open Energy Information

    Open Energy Info (EERE)

    to the MHK database homepage WaveStar.jpg Technology Profile Primary Organization Wave Star Energy Project(s) where this technology is utilized *MHK ProjectsWave Star Energy 1...

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

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

    Intirion: ENERGY STAR Referral (MFRA-4GF) Intirion: ENERGY STAR Referral (MFRA-4GF) August 14, 2012 DOE referred the matter of Intirion refrigerator model MFRA-4GF to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Intirion: ENERGY STAR Referral (MFRA-4GF) (89.26 KB) More Documents & Publications Samsung: ENERGY STAR Referral (RF26VAB) Friedrich:

  11. Kenmore: ENERGY STAR Referral (90701) | Department of Energy

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

    90701) Kenmore: ENERGY STAR Referral (90701) May 10, 2013 DOE referred the matter of Kenmore-brand dehumidifier, model number 90701, to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Kenmore: ENERGY STAR Referral (90701) (174.75 KB) More Documents & Publications Kenmore: ENERGY STAR Referral (253.16582104) Haier: ENERGY STAR Referral (DE45EK)

  12. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will introduce and demonstrate the EPA's ENERGY STAR Portfolio Manager tool. Attendees will learn how to navigate the new Portfolio Manager, add a property and enter details about it, enter energy and water consumption data, and more.

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

    Broader source: Energy.gov [DOE]

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

  14. University of Minnesota (NorthernSTAR Building America Partnership...

    Open Energy Info (EERE)

    (NorthernSTAR Building America Partnership) Jump to: navigation, search Name: University of Minnesota (NorthernSTAR Building America Partnership) Place: St. Paul, MN Information...

  15. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission You are...

  16. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Authors: Harrison,...

  17. The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission (Journal...

    Office of Scientific and Technical Information (OSTI)

    Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Citation Details In-Document Search Title: The Nuclear Spectroscopic Telescope Array (NuSTAR) Mission Authors: Harrison,...

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

    Energy Savers [EERE]

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

  19. Energy Star Lighting Verification Program (Program for the Evaluation...

    Office of Scientific and Technical Information (OSTI)

    Technical Report: Energy Star Lighting Verification Program (Program for the Evaluation and Analysis of Residential Lighting) Citation Details In-Document Search Title: Energy Star ...

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

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

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

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

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

    ... to use the widely-recognized ENERGY STAR brand * Access to marketing toolkit on password protected ENERGY STAR website * Access to other resources such as standardized ...

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

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

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

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

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

    FAQ's for: ENERGY STAR Verification Testing Pilot Program dated December 2010 FAQ's for: ENERGY STAR Verification Testing Pilot Program dated December 2010 This document is the ...

  4. China National BlueStar Group Corporation | Open Energy Information

    Open Energy Info (EERE)

    BlueStar Group Corporation Jump to: navigation, search Name: China National BlueStar Group Corporation Place: Beijing, Beijing Municipality, China Zip: 100029 Product: State-owned...

  5. Prairie Star (07) Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Prairie Star (07) Wind Farm Facility Prairie Star (07) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  6. Silver Star Hot Springs Geothermal Area | Open Energy Information

    Open Energy Info (EERE)

    Silver Star Hot Springs Geothermal Area Jump to: navigation, search GEOTHERMAL ENERGYGeothermal Home Silver Star Hot Springs Geothermal Area Contents 1 Area Overview 2 History and...

  7. Blue Star Energy Services (Pennsylvania) | Open Energy Information

    Open Energy Info (EERE)

    Star Energy Services (Pennsylvania) Jump to: navigation, search Name: Blue Star Energy Services Place: Pennsylvania Website: www.bluestarenergy.com Twitter: @keealliance Facebook:...

  8. Electrolux: ENERGY STAR Referral (EIDW6305***) | Department of...

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

    the EPA for appropriate action after DOE testing showed that the model may not meet the ENERGY STAR specification. Electrolux: ENERGY STAR Referral (EIDW6305***) More Documents &...

  9. Sino Power Star Co Ltd SPSCAP | Open Energy Information

    Open Energy Info (EERE)

    Power Star Co Ltd SPSCAP Jump to: navigation, search Name: Sino Power Star Co Ltd (SPSCAP) Place: Beijing, Beijing Municipality, China Zip: 102628 Sector: Vehicles Product:...

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

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

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

  11. Eco Energy Cities Plc STAR group | Open Energy Information

    Open Energy Info (EERE)

    Energy Cities Plc STAR group Jump to: navigation, search Name: Eco Energy Cities Plc (STAR group) Place: Shanghai, Shanghai Municipality, China Sector: Carbon, Renewable Energy...

  12. ENERGY STAR Labeled Buildings and Plants | Open Energy Information

    Open Energy Info (EERE)

    STAR Labeled Buildings and Plants Jump to: navigation, search Name ENERGY STAR Labeled Buildings and Plants Data Format Excel Spreadsheet Geographic Scope United States TODO:...

  13. Prairie Star (08) Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Wind Farm Jump to: navigation, search Name Prairie Star (08) Wind Farm Facility Prairie Star (08) Sector Wind energy Facility Type Commercial Scale Wind Facility Status In...

  14. Home Performance with ENERGY STAR -- Webinar Slides | Department...

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

    with ENERGY STAR -- Webinar Slides Home Performance with ENERGY STAR -- Webinar Slides "Existing Homes Efficiency - If You Want BetterBuildings - Go with Home Performance with...

  15. North Star Electric Coop, Inc | Open Energy Information

    Open Energy Info (EERE)

    North Star Electric Coop, Inc Jump to: navigation, search Name: North Star Electric Coop, Inc Address: 441 State Hwy 172 NW Place: Baudette, MN Zip: 56623 Phone Number:...

  16. Evaluation Prompts ENERGY STAR Program to Replace Web Tool, Saving...

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

    U.S. Environmental Protection Agency's ENERGY STAR Residential Program, is part of the Case Study Series, highlighting how "Evaluation Prompts ENERGY STAR Program to Replace Web ...

  17. SUPERMASSIVE DARK STARS: DETECTABLE IN JWST

    SciTech Connect (OSTI)

    Freese, Katherine; Ilie, Cosmin; Spolyar, Douglas; Valluri, Monica; Bodenheimer, Peter

    2010-06-20

    The first phase of stellar evolution in the history of the universe may be dark stars (DSs), powered by dark matter (DM) heating rather than by nuclear fusion. Weakly interacting massive particles (WIMPs), which may be their own antipartners, collect inside the first stars and annihilate to produce a heat source that can power the stars for millions to billions of years. In this paper, we show that these objects can grow to be supermassive dark stars (SMDSs) with masses {approx_gt}(10{sup 5}-10{sup 7}) M{sub sun}. The growth continues as long as DM heating persists, since DSs are large and cool (surface temperature {approx_lt}5 x 10{sup 4} K) and do not emit enough ionizing photons to prevent further accretion of baryons onto the star. The DM may be provided by two mechanisms: (1) gravitational attraction of DM particles on a variety of orbits not previously considered and (2) capture of WIMPs due to elastic scattering. Once the DM fuel is exhausted, the SMDS becomes a heavy main-sequence star; these stars eventually collapse to form massive black holes (BHs) that may provide seeds for supermassive BHs in the universe. SMDSs are very bright, with luminosities exceeding (10{sup 9}-10{sup 11}) L{sub sun}. We demonstrate that for several reasonable parameters, these objects will be detectable with the James Webb Space Telescope. Such an observational discovery would confirm the existence of a new phase of stellar evolution powered by DM.

  18. Wave-Based Subsurface Guide Star

    SciTech Connect (OSTI)

    Lehman, S K

    2011-07-26

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

  19. Simulations Reveal Unusual Death for Ancient Stars

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

    Simulations Reveal Unusual Death for Ancient Stars Simulations Reveal Unusual Death for Ancient Stars Findings made possible with NERSC resources and Berkeley Lab Code September 29, 2014 Contact: Linda Vu, +1 510 495 2402, lvu@lbl.gov SMSweb.jpg This image is a slice through the interior of a supermassive star of 55,500 solar masses along the axis of symmetry. It shows the inner helium core in which nuclear burning is converting helium to oxygen, powering various fluid instabilities (swirling

  20. BINARY DISRUPTION BY MASSIVE BLACK HOLES: HYPERVELOCITY STARS, S STARS, AND TIDAL DISRUPTION EVENTS

    SciTech Connect (OSTI)

    Bromley, Benjamin C.; Kenyon, Scott J.; Geller, Margaret J.; Brown, Warren R. E-mail: skenyon@cfa.harvard.edu E-mail: wbrown@cfa.harvard.edu

    2012-04-20

    We examine whether disrupted binary stars can fuel black hole growth. In this mechanism, tidal disruption produces a single hypervelocity star (HVS) ejected at high velocity and a former companion star bound to the black hole. After a cluster of bound stars forms, orbital diffusion allows the black hole to accrete stars by tidal disruption at a rate comparable to the capture rate. In the Milky Way, HVSs and the S star cluster imply similar rates of 10{sup -5} to 10{sup -3} yr{sup -1} for binary disruption. These rates are consistent with estimates for the tidal disruption rate in nearby galaxies and imply significant black hole growth from disrupted binaries on 10 Gyr timescales.

  1. KNOW THE STAR, KNOW THE PLANET. I. ADAPTIVE OPTICS OF EXOPLANET HOST STARS

    SciTech Connect (OSTI)

    Roberts, Lewis C.; Turner, Nils H.; Ten Brummelaar, Theo A.; Mason, Brian D.; Hartkopf, William I. E-mail: nils@chara-array.org E-mail: bdm@usno.navy.mil

    2011-11-15

    The results of an adaptive optics survey of exoplanet host stars for stellar companions are presented. We used the Advanced Electro-Optical System telescope and its adaptive optics system to collect deep images of the stars in the I band. Sixty-two exoplanet host stars were observed and fifteen multiple star systems were resolved. Of these eight are known multiples, while seven are new candidate binaries. For all binaries, we measured the relative astrometry of the pair and the differential magnitude in the I band. We improved the orbits of HD 19994 and {tau} Boo. These observations will provide improved statistics on the duplicity of exoplanet host stars and provide an increased understanding of the dynamics of known binary star exoplanet hosts.

  2. PIA - I-Manage STARS | Department of Energy

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

    PIA - I-Manage STARS PIA - I-Manage STARS PIA - I-Manage STARS PIA - I-Manage STARS (453.06 KB) More Documents & Publications PIA - INL PeopleSoft - Human Resource System PIA - Human Resources - Personal Information Change Request - Idaho National Engineering Laboratory PIA - INL Education Programs Business Enclave

  3. Home Performance with Energy Star | Department of Energy

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

    Performance with Energy Star Home Performance with Energy Star Residential Buildings Integration Project for the 2013 Building Technologies Office's Program Peer Review resbldgs05_jacobsohn_040313.pdf (1.79 MB) More Documents & Publications Home Performance with ENERGY STAR -- 10 Years of Continued Growth! Home Performance with ENERGY STAR - 2014 BTO Peer Review Residential Buildings Integration Program

  4. Neutron-star matter within the energy-density functional theory and neutron-star structure

    SciTech Connect (OSTI)

    Fantina, A. F.; Chamel, N.; Goriely, S.; Pearson, J. M.

    2015-02-24

    In this lecture, we will present some nucleonic equations of state of neutron-star matter calculated within the nuclear energy-density functional theory using generalized Skyrme functionals developed by the Brussels-Montreal collaboration. These equations of state provide a consistent description of all regions of a neutron star. The global structure of neutron stars predicted by these equations of state will be discussed in connection with recent astrophysical observations.

  5. Emerson: ENERGY STAR Referral (CR289E)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Emerson-brand refrigerator, model CR289E, to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  6. ASKO: ENERGY STAR Referral (D5253XXL)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of ASKO dishwasher model D5253XXL to the EPA for appropriate action after DOE testing showed that the model may not meet the ENERGY STAR specification.

  7. Samsung: ENERGY STAR Referral (RF26VAB)

    Broader source: Energy.gov [DOE]

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

  8. EPA ENERGY STAR Webcast: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  9. Whirlpool: ENERGY STAR Referral (ASD2524VE)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Whirlpool's Amana-brand dishwasher model ASD2524VE to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  10. Neutron stars in Einstein-aether theory

    SciTech Connect (OSTI)

    Eling, Christopher; Jacobson, Ted; Miller, M. Coleman

    2007-08-15

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

  11. Xcel Energy- Home Performance with ENERGY STAR

    Broader source: Energy.gov [DOE]

    Customers are not eligible to receive rebates from Home Performance with ENERGY STAR as well as other Xcel Energy programs for the same improvement. More program details and requirements are avai...

  12. Star of Excellence for Safety Performance

    Broader source: Energy.gov [DOE]

    AIKEN, S.C. – EM liquid waste contractor Savannah River Remediation (SRR) recently received the DOE Voluntary Protection Program (VPP) Star of Excellence award for its commitment to ensure the safety of employees.

  13. Home Performance with ENERGY STAR Program

    Broader source: Energy.gov [DOE]

    The New Jersey Board of Public Utilities (NJ BPU) offers a Home Performance with ENERGY STAR Program for residents that want to improve the energy efficiency of their homes. The program is set up...

  14. Danby: ENERGY STAR Referral (DAC10507EE)

    Broader source: Energy.gov [DOE]

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

  15. ASKO: ENERGY STAR Referral (D5122XXLB)

    Broader source: Energy.gov [DOE]

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

  16. Mayor Antonio Villaraigosa (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

    Los Angeles Mayor Antonio Villaraigosa delivered this presentation touting the energy efficiency and renewable energy related accomplishments of his city at the Energy All Stars event on January 19...

  17. Doyle Beneby (Energy All Stars Presentation)

    Office of Energy Efficiency and Renewable Energy (EERE)

    CPS Energy CEO Doyle Beneby delivered this presentation focusing on the importance of public-private partnerships to the energy economy at the Energy All Stars event on January 19, 2013, at the US...

  18. EPA ENERGY STAR Webcast: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

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

  19. Simulations Reveal Unusual Death for Ancient Stars

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

    around the sun. Visualizations were done in VisIT. (Image credit: Ken Chen) Certain primordial stars-those between 55,000 and 56,000 times the mass of our Sun, or solar ...

  20. Michael Liebreich (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  1. EPA ENERGY STAR Webcast: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  2. Dayton: ENERGY STAR Referral (5NTX1)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Dayton-brand refrigerator-freezer model 5NTX1 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  3. EPA ENERGY STAR Webcast- Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  4. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  5. Bill Nye (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  6. ENERGY STAR Webinar: Portfolio Manager 301

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency (EPA) ENERGY STAR, this webinar will show attendees how to upload templates to update property data, setting goals and targets to plan energy...

  7. EPA ENERGY STAR Webcast- Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    Continue to learn about EPA’s 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;...

  8. EPA ENERGY STAR Webcast: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    Continue to learn about EPA’s 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;...

  9. ENERGY STAR Webinar: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    This webinar continues on the U.S. Environmental Protection Agency's (EPA's) new ENERGY STAR Portfolio Manager tool. Attendees will learn the more advanced functionalities, such as managing and...

  10. Two ENERGY STAR Products Fail Testing

    Broader source: Energy.gov [DOE]

    DOE testing has identified two additional models of home appliances that do not meet the ENERGY STAR Program’s energy efficiency requirements.  A refrigerator manufactured by the Perlick...

  11. Jennifer Granholm (Energy All Stars Presentation)

    Office of Energy Efficiency and Renewable Energy (EERE)

    Former Michigan Governor Jennifer Granholm delivered this presentation advocating for an energy Race to the Top competition between the states at the Energy All Stars event on January 19, 2013, at...

  12. Sue Tierney (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

    Sue Tierney delivered this presentation" The Future of Energy: Toward the 21st Century Energy System We Need (With an Eye on the Rear View Mirror)" at the Energy All Stars event on January 19, 2013...

  13. Haier: ENERGY STAR Referral (DE45EK)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Haier-brand dehumidifier, model DE45EK, to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  14. Edgestar: ENERGY STAR Referral (DEP400EW)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Edgestar-brand dehumidifier, model DEP400EW, to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  15. Midea: ENERGY STAR Referral (MWF-08CR)

    Broader source: Energy.gov [DOE]

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

  16. Danby: ENERGY STAR Referral (DDR7009REE)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Danby-brand dehumidifier, model DDR7009REE, to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  17. Danby: ENERGY STAR Referral (DUFM304WDB)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Danby-brand freezer, model DUFM304WDB, to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  18. Solar Star NAFB LLC | Open Energy Information

    Open Energy Info (EERE)

    NAFB LLC Jump to: navigation, search Name: Solar Star NAFB LLC Place: Nevada Phone Number: (702) 643-8097 Outage Hotline: (702) 643-8097 References: EIA Form EIA-861 Final Data...

  19. Searching for Be stars in the open cluster NGC 663

    SciTech Connect (OSTI)

    Yu, P. C.; Lin, C. C.; Chen, W. P.; Lee, C. D.; Ip, W. H.; Ngeow, C. C.; Laher, Russ; Surace, Jason

    2015-02-01

    We present Be star candidates in the open cluster NGC 663, identified by H? imaging photometry with the Palomar Transient Factory Survey, as a pilot program to investigate how the Be star phenomena, the emission spectra, extended circumstellar envelopes, and fast rotation, correlate with massive stellar evolution. Stellar membership of the candidates was verified by 2MASS magnitudes and colors and by proper motions (PMs). We discover four new Be stars and exclude one known Be star from being a member due to its inconsistent PMs. The fraction of Be stars to member stars [N(Be)/N(members)] in NGC 663 is 3.5%. The spectral type of the 34 Be stars in NGC 663 shows bimodal peaks at B0B2 and B5B7, which is consistent with the statistics in most star clusters. Additionally, we also discover 23 emission-line stars of different types, including non-member Be stars, dwarfs, and giants.

  20. STAR FORMATION IN TWO LUMINOUS SPIRAL GALAXIES

    SciTech Connect (OSTI)

    Hunter, Deidre A.; Ashburn, Allison; Wright, Teresa; Elmegreen, Bruce G.; Rubin, Vera C.; Jzsa, Gyula I. G.; Struve, Christian

    2013-10-01

    We examined star formation in two very luminous (M{sub V} = 22 to 23) Sc-type spiral galaxies, NGC 801 and UGC 2885, using ultra-deep H? images. We combine these H? images with UBV and Two-Micron All-Sky Survey JHK images and H I maps to explore the star formation characteristics of disk galaxies at high luminosity. H? traces star formation in these galaxies to 4-6 disk scale lengths, but the lack of detection of H? further out is likely due to the loss of Lyman continuum photons. Considering gravitational instabilities alone, we find that the gas and stars in the outer regions are marginally stable in an average sense, but considering dissipative gas and radial and azimuthal forcing, the outer regions are marginally unstable to forming spiral arms. Star formation is taking place in spiral arms, which are regions of locally higher gas densities. Furthermore, we have traced smooth exponential stellar disks over four magnitudes in V-band surface brightness and 4-6 disk scale lengths, in spite of a highly variable gravitational instability parameter. Thus, gravitational instability thresholds do not seem relevant to the stellar disk. One possibility for creating an exponential disk is that the molecular cloud densities and star formation rates have exponential profiles and this fact forces the stellar disk to build up such a profile. Another possibility is that the stellar disk is continuously adjusted to an exponential shape regardless of the star formation profile, for example, through global dynamical processes that scatter stars. However, such scattering processes are only known to operate in spiral systems, in which case they cannot explain the same dilemma of smooth exponential disks observed in dwarf irregular galaxies.

  1. 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 radiation at unusually varying wavelengths. December 1, 2011 Los Alamos National Laboratory sits on top of a once-remote mesa in northern New Mexico with the Jemez mountains as a backdrop to research and innovation covering multi-disciplines from bioscience, sustainable energy sources, to plasma physics and new materials. Los

  2. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will introduce and demonstrate the EPA's ENERGY STAR Portfolio Manager tool. Attendees will learn how to navigate Portfolio Manager, add a property and enter details about it, enter energy and water consumption data, and more. This webinar runs from 1:00 to 2:00 p.m. Eastern Standard Time.

  3. NorthStar Medical Technologies LLC

    National Nuclear Security Administration (NNSA)

    Environmental Assessment for NorthStar Medical Technologies LLC Commercial Domestic Production of the Medical Isotope Molybdenum-99 (DOE/EA-1929) Prepared for U.S. Department of Energy National Nuclear Security Administration Defense Nuclear Nonproliferation/ Global Threat Reduction Initiative August 2012 EA for NorthStar Medical Technologies LLC Commercial Domestic Production of the Medical Isotope Mo-99 i COVER SHEET ENVIRONMENTAL ASSESSMENT FOR NORTHSTAR MEDICAL TECHNOLOGIES LLC COMMERCIAL

  4. Support for ENERGY STAR Enforcement | Department of Energy

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

    Support for ENERGY STAR Enforcement Support for ENERGY STAR Enforcement By offering a means for consumers to buy products more energy-efficient than required by law, ENERGY STAR has huge potential to save money for consumers by offering buyers more options in energy-efficient products. In a new initiative, the Department is expanding verification and supporting enforcement of ENERGY STAR to preserve the viability and effectiveness of the ENERGY STAR program. Through independent testing, we are

  5. Sunpentown: ENERGY STAR Referral (RF-330SS) | Department of Energy

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

    Sunpentown: ENERGY STAR Referral (RF-330SS) Sunpentown: ENERGY STAR Referral (RF-330SS) May 10, 2013 DOE referred the matter of Sunpentown-brand refrigerator, model RF-330SS, manufactured by Hefei Hualing Co., Ltd, to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Sunpentown: ENERGY STAR Referral (RF-330SS) (9.82 KB) More Documents & Publications

  6. Neutron stars as laboratories for gravity physics

    SciTech Connect (OSTI)

    Deliduman, Cemsinan

    2014-01-01

    We study the structure of neutron stars in R+?R gravity model with perturbative method. We obtain mass-radius relations for four representative equations of state (EoS). We find that, for |?|~10? cm, the results differ substantially from the results of general relativity. The effects of modified gravity are seen as mimicking a stiff or soft EoS for neutron stars depending upon whether ? is negative or positive, respectively. Some of the soft EoS that are excluded within the framework of general relativity can be reconciled for certain values of ? of this order with the 2 solar mass neutron star recently observed. Indeed, if the EoS is ever established to be soft, modified gravity of the sort studied here may be required to explain neutron star masses as large as 2 M{sub ?}. The associated length scale ?(?)~10? cm is of the order of the the typical radius of neutron stars implying that this is the smallest value we could find by using neutron stars as a probe. We thus conclude that the true value of ? is most likely much smaller than 10? cm.

  7. Storage and Assay of Tritium in STAR

    SciTech Connect (OSTI)

    Glen R. Longhurst; Robert A. Anderl; Robert J. Pawelko

    2004-09-01

    The Safety and Tritium Applied Research (STAR) facility has recently been commissioned to investigate tritium-related safety questions for fusion and other technologies. The authorized inventory of tritium is 1.6 grams, the threshold quantity for nuclear facility classification. A key capability in successful operation of the STAR facility is the ability to receive, inventory, and dispense tritium to the various experiments underway there. The system central to that function is the Tritium Storage and Assay System (SAS). The SAS has four major functions: (1) receiving and holding tritium from shipping containers brought into the STAR facility, (2) assaying the amount of tritium in the SAS, (3) dispensing tritium to secondary beds or containers used for transferring it to the experimental systems in the STAR facility, and (4) purifying hydrogen isotopes from non-hydrogen species. To that may be added a fifth, optional function, isotopic separation of hydrogen isotopes using bed-to-bed transfer techniques. This paper documents the design and operation of the STAR SAS and the procedures used for tritium accountancy in the STAR facility.

  8. TIME-VARYING DYNAMICAL STAR FORMATION RATE

    SciTech Connect (OSTI)

    Lee, Eve J.; Chang, Philip; Murray, Norman

    2015-02-10

    We present numerical evidence of dynamic star formation in which the accreted stellar mass grows superlinearly with time, roughly as t {sup 2}. We perform simulations of star formation in self-gravitating hydrodynamic and magnetohydrodynamic turbulence that is continuously driven. By turning the self-gravity of the gas in the simulations on or off, we demonstrate that self-gravity is the dominant physical effect setting the mass accretion rate at early times before feedback effects take over, contrary to theories of turbulence-regulated star formation. We find that gravitational collapse steepens the density profile around stars, generating the power-law tail on what is otherwise a lognormal density probability distribution function. Furthermore, we find turbulent velocity profiles to flatten inside collapsing regions, altering the size-line width relation. This local flattening reflects enhancements of turbulent velocity on small scales, as verified by changes to the velocity power spectra. Our results indicate that gas self-gravity dynamically alters both density and velocity structures in clouds, giving rise to a time-varying star formation rate. We find that a substantial fraction of the gas that forms stars arrives via low-density flows, as opposed to accreting through high-density filaments.

  9. Star formation relations in nearby molecular clouds

    SciTech Connect (OSTI)

    Evans, Neal J. II; Heiderman, Amanda; Vutisalchavakul, Nalin

    2014-02-20

    We test some ideas for star formation relations against data on local molecular clouds. On a cloud by cloud basis, the relation between the surface density of star formation rate and surface density of gas divided by a free-fall time, calculated from the mean cloud density, shows no significant correlation. If a crossing time is substituted for the free-fall time, there is even less correlation. Within a cloud, the star formation rate volume and surface densities increase rapidly with the corresponding gas densities, faster than predicted by models using the free-fall time defined from the local density. A model in which the star formation rate depends linearly on the mass of gas above a visual extinction of 8 mag describes the data on these clouds, with very low dispersion. The data on regions of very massive star formation, with improved star formation rates based on free-free emission from ionized gas, also agree with this linear relation.

  10. ENERGY STAR Webinar: Update on CREBs DATA and ENERGY STAR Score Development Process

    Broader source: Energy.gov [DOE]

    Hosted by the EPA's ENERGY STAR, this webinar will outline the schedule for ENERGY STAR 1-100 score development based on the 2012 Commercial Building Energy Consumption Survey data, provide a review of the types of properties covered, and a summary of new variables collected. This webinar runs from 2-3 p.m. Eastern Standard Time.

  11. ENERGY STAR Webinar: The Value of ENERGY STAR for Commercial Building Design

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will demonstrate the ENERGY STAR Target Finder and Portfolio Manager tools and show how they can be used to meet industry initiatives like the AIA 2030 Commitment and Architecture 2030 Challenge. This webinar will run from 2-3 p.m. Eastern Standard Time.

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

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) is hosting a webinar on how to apply 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 help your property get from application to award.

  13. Juno Beach, Florida: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Registered Energy Companies in Juno Beach, Florida Florida Power and Light Company Lone Star Transmission LLC NextEra Energy Resources formerly FPL Energy LLC References US...

  14. Quark matter symmetry energy and quark stars

    SciTech Connect (OSTI)

    Chu, Peng-Cheng; Chen, Lie-Wen

    2014-01-10

    We extend the confined-density-dependent-mass (CDDM) model to include isospin dependence of the equivalent quark mass. Within the confined-isospin-density-dependent-mass (CIDDM) model, we study the quark matter symmetry energy, the stability of strange quark matter, and the properties of quark stars. We find that including isospin dependence of the equivalent quark mass can significantly influence the quark matter symmetry energy as well as the properties of strange quark matter and quark stars. While the recently discovered large mass pulsars PSR J1614–2230 and PSR J0348+0432 with masses around 2 M {sub ☉} cannot be quark stars within the CDDM model, they can be well described by quark stars in the CIDDM model. In particular, our results indicate that the two-flavor u-d quark matter symmetry energy should be at least about twice that of a free quark gas or normal quark matter within the conventional Nambu-Jona-Lasinio model in order to describe PSR J1614–2230 and PSR J0348+0432 as quark stars.

  15. Magnetic fields and galactic star formation rates

    SciTech Connect (OSTI)

    Loo, Sven Van; Tan, Jonathan C.; Falle, Sam A. E. G.

    2015-02-10

    The regulation of galactic-scale star formation rates (SFRs) is a basic problem for theories of galaxy formation and evolution: which processes are responsible for making observed star formation rates so inefficient compared to maximal rates of gas content divided by dynamical timescale? Here we study the effect of magnetic fields of different strengths on the evolution of giant molecular clouds (GMCs) within a kiloparsec patch of a disk galaxy and resolving scales down to ?0.5 pc. Including an empirically motivated prescription for star formation from dense gas (n{sub H}>10{sup 5} cm{sup ?3}) at an efficiency of 2% per local free-fall time, we derive the amount of suppression of star formation by magnetic fields compared to the nonmagnetized case. We find GMC fragmentation, dense clump formation, and SFR can be significantly affected by the inclusion of magnetic fields, especially in our strongest investigated B-field case of 80 ?G. However, our chosen kiloparsec-scale region, extracted from a global galaxy simulation, happens to contain a starbursting cloud complex that is only modestly affected by these magnetic fields and likely requires internal star formation feedback to regulate its SFR.

  16. Haier: ENERGY STAR Referral (PRTS21SAC*) | Department of Energy

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

    PRTS21SAC*) Haier: ENERGY STAR Referral (PRTS21SAC*) September 20, 2011 DOE referred the matter of Haier refrigerator model PRTS21SAC* to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Haier: ENERGY STAR Referral (PRTS21SAC*) (77.61 KB) More Documents & Publications Haier: ENERGY STAR Referral (ESA408J) Haier: ENERGY STAR Referral (ESNCM053E)

  17. STARS MDT-II targets mission

    SciTech Connect (OSTI)

    Sims, B.A.; White, J.E.

    1997-08-01

    The Strategic Target System (STARS) was launched successfully on August 31, 1996 from the Kauai Test Facility (KTF) at the Pacific Missile Range Facility (PMRF). The STARS II booster delivered a payload complement of 26 vehicles atop a post boost vehicle. These targets were designed and the mission planning was achieved to provide for a dedicated mission for view by the Midcourse Space Experiment (MSX) Satellite Sensor Suite. Along with the MSX Satellite, other corollary sensors were involved. Included in these were the Airborne Surveillance Test Bed (AST) aircraft, the Cobra Judy sea based radar platform, Kwajalein Missile Range (KMR), and the Kiernan Reentry Measurements Site (KREMS). The launch was a huge success from all aspects. The STARS Booster flew a perfect mission from hardware, software and mission planning respects. The payload complement achieved its desired goals. All sensors (space, air, ship, and ground) attained excellent coverage and data recording.

  18. THE CLASSIFICATION OF KEPLER B-STAR VARIABLES

    SciTech Connect (OSTI)

    McNamara, Bernard J.; Jackiewicz, Jason; McKeever, Jean E-mail: jasonj@nmsu.edu

    2012-04-15

    The light curves of 252 B-star candidates in the Kepler database are analyzed in a similar fashion to that done by Balona et al. to further characterize B-star variability, increase the sample of variable B stars for future study, and to identify stars whose power spectra include particularly interesting features such as frequency groupings. Stars are classified as either constant light emitters, {beta} Cep stars, slowly pulsating B stars (SPBs), hybrid pulsators, binaries or stars whose light curves are dominated by rotation (Bin/Rot), hot subdwarfs, or white dwarfs. One-hundred stars in our sample were found to be either light constants or to be variable at a level of less than 0.02 mmag. We increase the number of candidate B-star variables found in the Kepler database by Balona et al. in the following fashion: {beta} Cep stars from 0 to 10, SPBs from eight to 54, hybrid pulsators from seven to 21, and Bin/Rot stars from 23 to 82. For comparison purposes, approximately 51 SPBs and six hybrids had been known prior to 2007. The number of {beta} Cep stars known prior to 2004 was 93. A secondary result of this study is the identification of an additional 11 pulsating white dwarf candidates, four of which possess frequency groupings.

  19. Integration and conventional systems at STAR

    SciTech Connect (OSTI)

    Matis, Howard S.; Brown, Ralph L.; Christie, William; Edwards, W.R.; Jared, Richard; Minor, Bob; Salz, Paul

    2002-02-20

    At the beginning of the design and construction of the STAR Detector, the collaboration assigned a team of physicists and engineers the responsibility of coordinating the construction of the detector. This group managed the general space assignments for each sub-system and coordinated the assembly and planning for the detector. Furthermore, as this group was the only STAR group with the responsibility of looking at the system as a whole, the collaboration assigned it several tasks that spanned the different sub-detectors. These items included grounding, rack layout, cable distribution, electrical, power and water, and safety systems. This paper describes these systems and their performance.

  20. When Stars Attack! In Search of

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

    Stars Attack! In Search of Near-Earth Supernova Explosions Brian Fields University of Illinois January 27, 2016 4:00 p.m. - Wilson Hall, One West The most massive stars are the celebrities of the cosmos: they are rare, but live extravagantly and die in spectacular and violent supernova explosions. These awesome events take a sinister shade when they occur close to home, because an explosion very nearby would pose a grave threat to Earthlings. We will discuss these cosmic insults to life, and

  1. Electrolux: ENERGY STAR Referral (FFN09M5HW*)

    Broader source: Energy.gov [DOE]

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

  2. Upper Bound on the First Star Formation History (Journal Article...

    Office of Scientific and Technical Information (OSTI)

    Upper Bound on the First Star Formation History Citation Details In-Document Search Title: Upper Bound on the First Star Formation History You are accessing a document from the ...

  3. The Energy of Star Wars: A Google+ Hangout

    Broader source: Energy.gov [DOE]

    Calling all Star Wars fans! Chat with our experts about energy in the Star Wars universe, from lightsabers to landspeeders, on a Google+ Hangout at 2 p.m. ET on Friday, June 12, 2015.

  4. Friedrich: ENERGY STAR Referral (YM18M34-A)

    Broader source: Energy.gov [DOE]

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

  5. Advanced Combustion Modeling with STAR-CD using Transient Flemelet...

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

    Modeling with STAR-CD using Transient Flemelet Models: TIF and TPV Advanced Combustion Modeling with STAR-CD using Transient Flemelet Models: TIF and TPV Presentation given at the ...

  6. On the Lack of Evolution in Galaxy Star Formation Efficiency...

    Office of Scientific and Technical Information (OSTI)

    On the Lack of Evolution in Galaxy Star Formation Efficiency Citation Details In-Document Search Title: On the Lack of Evolution in Galaxy Star Formation Efficiency You are ...

  7. Electrolux: ENERGY STAR Referral (EW26SS70I*)

    Broader source: Energy.gov [DOE]

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

  8. Perlick: ENERGY STAR Referral (HP72ROO-S)

    Broader source: Energy.gov [DOE]

    DOE referred Perlick refrigerator HP72ROO-S to EPA, brand manager of the ENERGY STAR program, for appropriate action after DOE testing revealed that the model does not meet ENERGY STAR requirements.

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

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

    following homes are eligible to earn the ENERGY STAR: Detached dwelling units 1 (e.g. ... Dwelling units 1 in multifamily buildings that are not eligible to earn the ENERGY STAR ...

  10. Energy Department Announces Partnership with CoStar Group, Inc...

    Energy Savers [EERE]

    Partnership with CoStar Group, Inc. to Expand Visibility of Energy-Efficient Buildings in U.S. Real Estate Marketplace Energy Department Announces Partnership with CoStar Group, ...

  11. ENERGY STAR Residential Water Heaters to Save Americans Up to...

    Energy Savers [EERE]

    STAR Residential Water Heaters to Save Americans Up to 823 Million in the Next Five Years ENERGY STAR Residential Water Heaters to Save Americans Up to 823 Million in the Next ...

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

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

    Home Performance with ENERGY STAR -- 10 Years of Continued Growth Home Performance with ENERGY STAR -- 10 Years of Continued Growth Provides an overview of the HPwES program, ...

  13. Perlick: ENERGY STAR Referral (HP48RO-S)

    Broader source: Energy.gov [DOE]

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

  14. DOE Energy Star Testing Reveals Inefficient ASKO Dishwasher

    Broader source: Energy.gov [DOE]

    DOE testing in support of the Energy Star program has revealed that an ASKO dishwasher (model D5122XXLB), which the company had claimed was Energy Star compliant, consumes more energy than...

  15. Duke Energy (Electric)- Energy Star Homes Rate Discount Program

    Broader source: Energy.gov [DOE]

    Duke Energy encourages residential customers to buy energy-efficient homes through the utility's Energy Star Homes Program, which awards a rate discount to customers living in Energy Star homes. To...

  16. Columbia Water & Light- New Home ENERGY STAR Rebate

    Broader source: Energy.gov [DOE]

    Columbia Water and Light offers a $1,000 rebate to customers for the construction of new homes that achieve certification as Energy Star homes. The Energy Star designation is given to homes that...

  17. Duke Energy Carolinas (Electric)- Energy Star Homes Rate Discount Program

    Broader source: Energy.gov [DOE]

    Duke Energy Carolinas encourages residential customers to buy energy-efficient homes through the utility's Energy Star Homes Program, which awards a rate discount to customers living in Energy Star...

  18. Duke Energy (Electric)- Energy Star Homes Rate Discount Program

    Broader source: Energy.gov [DOE]

    Duke Energy encourages residential customers to buy energy-efficient homes through the utility's Energy Star Homes Program, which awards a rate discount to customers living in Energy Star homes....

  19. ENERGY STAR Webinar: Portfolio Manager 301 | Department of Energy

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

    301 ENERGY STAR Webinar: Portfolio Manager 301 December 17, 2015 1:00PM to 2:00PM EST Online Hosted by the U.S. Environmental Protection Agency (EPA) ENERGY STAR, this webinar will...

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

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

    Appliance & Equipment Standards » ENERGY STAR » ENERGY STAR Test Procedures and Verification ENERGY STAR Test Procedures and Verification The Department of Energy (DOE) is the lead agency in the development and revision of all test procedures for products in the ENERGY STAR® program, including those products that are also subject to DOE's Energy Conservation Standards program. As specifications are updated and new products or metrics are added to the ENERGY STAR program, DOE is

  1. Kenmore: ENERGY STAR Referral (253.16582104) | Department of Energy

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

    253.16582104) Kenmore: ENERGY STAR Referral (253.16582104) April 18, 2012 DOE referred the matter of Kenmore-brand freezer model 253.16582104, which is manufactured by Electrolux Major Appliances North America ("Electrolux"), to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing raised issues regarding whether model 253.16582104 was properly qualified as an ENERGY STAR model. Kenmore: ENERGY STAR Referral

  2. ARM - Campaign Instrument - kandz-cm21-schenk-star

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

    -schenk-star Comments? We would love to hear from you! Send us a note below or call us at 1-888-ARM-DATA. Send Campaign Instrument : Kipp and Zonen-CM21 Schenk Star (KANDZ-CM21-SCHENK-STAR) Instrument Categories Radiometric Campaigns

  3. Star cell type core configuration for structural sandwich materials

    DOE Patents [OSTI]

    Christensen, Richard M.

    1995-01-01

    A new pattern for cellular core material used in sandwich type structural materials. The new pattern involves star shaped cells intermixed with hexagonal shaped cells. The new patterned cellular core material includes star shaped cells interconnected at points thereof and having hexagonal shape cells positioned adjacent the star points. The new pattern allows more flexibility and can conform more easily to curved shapes.

  4. Energy star compliant voice over internet protocol (VoIP) telecommunications network including energy star compliant VoIP devices

    DOE Patents [OSTI]

    Kouchri, Farrokh Mohammadzadeh

    2012-11-06

    A Voice over Internet Protocol (VoIP) communications system, a method of managing a communications network in such a system and a program product therefore. The system/network includes an ENERGY STAR (E-star) aware softswitch and E-star compliant communications devices at system endpoints. The E-star aware softswitch allows E-star compliant communications devices to enter and remain in power saving mode. The E-star aware softswitch spools messages and forwards only selected messages (e.g., calls) to the devices in power saving mode. When the E-star compliant communications devices exit power saving mode, the E-star aware softswitch forwards spooled messages.

  5. ENERGY STAR Webinar: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

    This webinar continues on the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR Portfolio Manager tool. Attendees will learn the more advanced functionalities, such as managing and tracking changes to your property uses over time, using spreadsheet templates to update property data, setting goals and targets to plan energy improvements for properties, generating and using custom reports, and using the Sustainable Buildings Checklist.

  6. ENERGY STAR Webinar: Portfolio Manager 301

    Broader source: Energy.gov [DOE]

    Hosted by the U.S. Environmental Protection Agency (EPA) ENERGY STAR, this webinar will show attendees how to upload templates to update property data, setting goals and targets to plan energy improvements for properties, creating custom reports, and using the Sustainable Buildings Checklist.

  7. The make-up of stars

    SciTech Connect (OSTI)

    Asplund, Martin

    2014-11-20

    The chemical composition of stars contain vital clues not only about the stars themselves but also about the conditions prevailing before their births. As such, stellar spectroscopy plays a key role in contemporary astrophysics and cosmology by probing cosmic, galactic, stellar and planetary evolution. In this review I will describe the theoretical foundations of quantitative stellar spectroscopy: stellar atmosphere models and spectral line formation. I will focus mainly on more recent advances in the field, in particular the advent of realistic time-dependent, 3D, (magneto-)hydrodynamical simulations of stellar surface convection and atmospheres and non-LTE radiative transfer relevant for stars like the Sun. I will also discuss some particular applications of this type of modelling which have resulted in some exciting break-throughs in our understanding and with wider implications: the solar chemical composition, the chemical signatures of planet formation imprinted in stellar abundances, the cosmological Li problem(s) and where the first stars may be residing today.

  8. SUPPRESSION OF STAR FORMATION IN NGC 1266

    SciTech Connect (OSTI)

    Alatalo, Katherine; Lanz, Lauranne; Bitsakis, Theodoros; Appleton, Philip N.; Ogle, Patrick M.; Lacy, Mark; Lonsdale, Carol J.; Nyland, Kristina; Meier, David S.; Cales, Sabrina L.; Chang, Philip; Davis, Timothy A.; De Zeeuw, P. T.; Martn, Sergio

    2015-01-01

    NGC 1266 is a nearby lenticular galaxy that harbors a massive outflow of molecular gas powered by the mechanical energy of an active galactic nucleus (AGN). It has been speculated that such outflows hinder star formation (SF) in their host galaxies, providing a form of feedback to the process of galaxy formation. Previous studies, however, indicated that only jets from extremely rare, high-power quasars or radio galaxies could impart significant feedback on their hosts. Here we present detailed observations of the gas and dust continuum of NGC 1266 at millimeter wavelengths. Our observations show that molecular gas is being driven out of the nuclear region at M-dot {sub out}?110 M{sub ?} yr{sup 1}, of which the vast majority cannot escape the nucleus. Only 2 M {sub ?} yr{sup 1} is actually capable of escaping the galaxy. Most of the molecular gas that remains is very inefficient at forming stars. The far-infrared emission is dominated by an ultra-compact (? 50 pc) source that could either be powered by an AGN or by an ultra-compact starburst. The ratio of the SF surface density (?{sub SFR}) to the gas surface density (?{sub H{sub 2}}) indicates that SF is suppressed by a factor of ?50 compared to normal star-forming galaxies if all gas is forming stars, and ?150 for the outskirt (98%) dense molecular gas if the central region is powered by an ultra-compact starburst. The AGN-driven bulk outflow could account for this extreme suppression by hindering the fragmentation and gravitational collapse necessary to form stars through a process of turbulent injection. This result suggests that even relatively common, low-power AGNs are able to alter the evolution of their host galaxies as their black holes grow onto the M-? relation.

  9. STAR FORMATION IN THE TAURUS FILAMENT L 1495: FROM DENSE CORES TO STARS

    SciTech Connect (OSTI)

    Schmalzl, Markus; Kainulainen, Jouni; Henning, Thomas; Launhardt, Ralf; Quanz, Sascha P.; Alves, Joao; Goodman, Alyssa A.; Pineda, Jaime E.; Roman-Zuniga, Carlos G.

    2010-12-10

    We present a study of dense structures in the L 1495 filament in the Taurus Molecular Cloud and examine its star-forming properties. In particular, we construct a dust extinction map of the filament using deep near-infrared observations, exposing its small-scale structure in unprecedented detail. The filament shows highly fragmented substructures and a high mass-per-length value of M{sub line} = 17 M{sub sun} pc{sup -1}, reflecting star-forming potential in all parts of it. However, a part of the filament, namely B 211, is remarkably devoid of young stellar objects. We argue that in this region the initial filament collapse and fragmentation is still taking place and star formation is yet to occur. In the star-forming part of the filament, we identify 39 cores with masses from 0.4 to 10 M{sub sun} and preferred separations in agreement with the local Jeans length. Most of these cores exceed the Bonnor-Ebert critical mass, and are therefore likely to collapse and form stars. The dense core mass function follows a power law with exponent {Gamma} = 1.2 {+-} 0.2, a form commonly observed in star-forming regions.

  10. Summit: ENERGY STAR Referral (F1112BL) | Department of Energy

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

    Summit: ENERGY STAR Referral (F1112BL) Summit: ENERGY STAR Referral (F1112BL) June 20, 2013 DOE referred the matter of Summit-brand refrigerator-freezer model F1112BL, which is manufactured by SANYO E&E (now Panasonic Appliances Refrigeration Systems Corporation of America), to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Summit: ENERGY STAR

  11. LITHIUM ABUNDANCES IN CARBON-ENHANCED METAL-POOR STARS

    SciTech Connect (OSTI)

    Masseron, Thomas; Johnson, Jennifer A.; Lucatello, Sara; Karakas, Amanda; Plez, Bertrand; Beers, Timothy C.; Christlieb, Norbert E-mail: jaj@astronomy.ohio-state.edu

    2012-05-20

    Carbon-enhanced metal-poor (CEMP) stars are believed to show the chemical imprints of more massive stars (M {approx}> 0.8 M{sub Sun }) that are now extinct. In particular, it is expected that the observed abundance of Li should deviate in these stars from the standard Spite lithium plateau. We study here a sample of 11 metal-poor stars and a double-lined spectroscopic binary with -1.8 < [Fe/H] < -3.3 observed with the Very Large Telescope/UVES spectrograph. Among these 12 metal-poor stars, there are 8 CEMP stars for which we measure or constrain the Li abundance. In contrast to previous arguments, we demonstrate that an appropriate regime of dilution permits the existence of 'Li-Spite plateau and C-rich' stars, whereas some of the 'Li-depleted and C-rich' stars call for an unidentified additional depletion mechanism that cannot be explained by dilution alone. We find evidence that rotation is related to the Li depletion in some CEMP stars. Additionally, we report on a newly recognized double-lined spectroscopic binary star in our sample. For this star, we develop a new technique from which estimates of stellar parameters and luminosity ratios can be derived based on a high-resolution spectrum alone, without the need for input from evolutionary models.

  12. NEW X-RAY DETECTIONS OF WNL STARS

    SciTech Connect (OSTI)

    Skinner, Stephen L.; Zhekov, Svetozar A.; Guedel, Manuel; Schmutz, Werner; Sokal, Kimberly R.

    2012-05-15

    Previous studies have demonstrated that putatively single nitrogen-type Wolf-Rayet stars (WN stars) without known companions are X-ray sources. However, almost all WN star X-ray detections so far have been of earlier WN2-WN6 spectral subtypes. Later WN7-WN9 subtypes (also known as WNL stars) have proved more difficult to detect, an important exception being WR 79a (WN9ha). We present here new X-ray detections of the WNL stars WR 16 (WN8h) and WR 78 (WN7h). These new results, when combined with previous detections, demonstrate that X-ray emission is present in WN stars across the full range of spectral types, including later WNL stars. The two WN8 stars observed to date (WR 16 and WR 40) show unusually low X-ray luminosities (L{sub x} ) compared to other WN stars, and it is noteworthy that they also have the lowest terminal wind speeds (v{sub {infinity}}). Existing X-ray detections of about a dozen WN stars reveal a trend of increasing L{sub x} with wind luminosity L{sub wind} = (1/2)M-dot v{sup 2}{sub {infinity}}, suggesting that wind kinetic energy may play a key role in establishing X-ray luminosity levels in WN stars.

  13. SPIN EVOLUTION OF ACCRETING YOUNG STARS. I. EFFECT OF MAGNETIC STAR-DISK COUPLING

    SciTech Connect (OSTI)

    Matt, Sean P.; Greene, Thomas P.; Pinzon, Giovanni; De la Reza, Ramiro E-mail: thomas.p.greene@nasa.go E-mail: delareza@on.b

    2010-05-10

    We present a model for the rotational evolution of a young, solar mass star interacting with an accretion disk. The model incorporates a description of the angular momentum transfer between the star and the disk due to a magnetic connection, and includes changes in the star's mass and radius and a decreasing accretion rate. The model also includes, for the first time in a spin evolution model, the opening of the stellar magnetic field lines, as expected to arise from twisting via star-disk differential rotation. In order to isolate the effect that this has on the star-disk interaction torques, we neglect the influence of torques that may arise from open field regions connected to the star or disk. For a range of magnetic field strengths, accretion rates, and initial spin rates, we compute the stellar spin rates of pre-main-sequence stars as they evolve on the Hayashi track to an age of 3 Myr. How much the field opening affects the spin depends on the strength of the coupling of the magnetic field to the disk. For the relatively strong coupling (i.e., high magnetic Reynolds number) expected in real systems, all models predict spin periods of less than {approx}3 days, in the age range of 1-3 Myr. Furthermore, these systems typically do not reach an equilibrium spin rate within 3 Myr, so that the spin at any given time depends upon the choice of initial spin rate. This corroborates earlier suggestions that, in order to explain the full range of observed rotation periods of approximately 1-10 days, additional processes, such as the angular momentum loss from powerful stellar winds, are necessary.

  14. Quantum liquid signatures in dwarf stars

    SciTech Connect (OSTI)

    Gabadadze, Gregory; Pirtskhalava, David E-mail: dmp371@nyu.edu

    2009-05-15

    We develop further the proposal of arXiv:0806.3692 that a new state of matter - charged condensate of spin-0 nuclei - may exist in helium-core dwarf stars. The charged condensate and its fluctuations are described by an effective field theory Lagrangian. The spectrum of bosonic fluctuations is gapped, while electrons, at temperatures of interest, give rise to gapless excitations near the Fermi surface. These properties determine the evolution of the dwarfs with condensed cores. In particular, we show that such dwarf stars would cool significantly faster than their crystallized counterparts. As a result, the luminosity function for the helium-core dwarfs will have a sharp drop-off after the condensation. It is tempting to interpret the recently discovered abrupt termination of a sequence of 24 helium-core dwarf candidates in NGC 6397 as a signature of the charged condensation.

  15. FAST FOSSIL ROTATION OF NEUTRON STAR CORES

    SciTech Connect (OSTI)

    Melatos, A.

    2012-12-10

    It is argued that the superfluid core of a neutron star super-rotates relative to the crust, because stratification prevents the core from responding to the electromagnetic braking torque, until the relevant dissipative (viscous or Eddington-Sweet) timescale, which can exceed {approx}10{sup 3} yr and is much longer than the Ekman timescale, has elapsed. Hence, in some young pulsars, the rotation of the core today is a fossil record of its rotation at birth, provided that magnetic crust-core coupling is inhibited, e.g., by buoyancy, field-line topology, or the presence of uncondensed neutral components in the superfluid. Persistent core super-rotation alters our picture of neutron stars in several ways, allowing for magnetic field generation by ongoing dynamo action and enhanced gravitational wave emission from hydrodynamic instabilities.

  16. Energy Star Concepts for Highway Vehicles

    SciTech Connect (OSTI)

    Greene, D.L.

    2003-06-24

    The authors of this report, under the sponsorship of the U.S. Department of Energy (DOE) Office of Energy Efficiency and Renewable Energy (EERE) Weatherization and Intergovernmental Program, have investigated the possible application of Energy Star ratings to passenger cars and light trucks. This study establishes a framework for formulating and evaluating Energy Star rating methods that is comprised of energy- and environmental-based metrics, potential vehicle classification systems, vehicle technology factors, and vehicle selection criteria. The study tests several concepts and Energy Star rating methods using model-year 2000 vehicle data--a spreadsheet model has been developed to facilitate these analyses. This study tests two primary types of rating systems: (1) an outcome-based system that rates vehicles based on fuel economy, GHG emissions, and oil use and (2) a technology-based system that rates vehicles based on the energy-saving technologies they use. Rating methods were evaluated based on their ability to select vehicles with high fuel economy, low GHG emissions, and low oil use while preserving a full range of service (size and acceleration) and body style choice. This study concludes that an Energy Star rating for passenger cars and light trucks is feasible and that several methods could be used to achieve reasonable tradeoffs between low energy use and emissions and diversity in size, performance, and body type. It also shows that methods that consider only fuel economy, GHG emissions, or oil use will not select a diverse mix of vehicles. Finally, analyses suggest that methods that encourage the use of technology only, may result in increases in acceleration power and weight rather than reductions in oil use and GHG emissions and improvements in fuel economy.

  17. All-Star Nanocrystals | The Ames Laboratory

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

    All-Star Nanocrystals Researchers discovered semiconducting nanocrystals that not only function as stellar light-to-energy converters but also as stable light emitters. Scientists synthesized a series of perovskite nanocrystals with different morphologies i.e., dots, rods, wires, plates, and sheets. Perovskite materials such as CH3NH3PbX3 (X = I, Br) are known to display many intriguing electronic light and chemical properties. Studies found that the rods and wires showed higher

  18. Observation of stars produced during cold fusion

    SciTech Connect (OSTI)

    Matsumoto, T. . Dept. of Nuclear Engineering)

    1992-12-01

    It has been indicated tht multiple-neutron nuclei such as quad-neutrons can be emitted during cold fusion. These multiple-neutrons might bombard the nuclei of materials outside a cold fusion cell to cause nuclear reactions. In this paper, observations of nuclear emulsions that were irradiated during a cold fusion experiment with heavy water and palladium foil are described. Various traces, like stars, showing nuclear reactions caused by the multiple-neutrons have been clearly observed.

  19. The H? profiles of Be shell stars

    SciTech Connect (OSTI)

    Silaj, J.; Jones, C. E.; Sigut, T. A. A.; Tycner, C.

    2014-11-01

    A new set of theoretical H? emission line profiles of Be stars has been computed using the code BERAY, which solves the transfer equation along a series of rays passing through the star+disk system, representing an improved treatment over earlier work done by the authors. The new profiles were compared with the previous work, and general trends (such as line profile shapes and correlations between line equivalent widths as a function of initial density ?{sub 0} and power law index n) were recovered. Additionally, BERAY was employed to model the spectra of eight well-known Be shell stars. Some degeneracy was found in the choice of model parameters, highlighting the need to employ alternate observables to constrain the models. However, the inclination angle of the model seemed relatively insensitive to the choices of other parameters, and we show that, with our models, only a very small range of inclination angles can adequately reproduce the observations. Five of our eight targets were found to have inclination angles of 70 or higher, and two more were found to have inclination angles of 67 and 65. The observation of one target4 Aquilaecould only be reproduced by models created at an inclination angle of approximately 45.

  20. Neutron-capture nucleosynthesis in the first stars

    SciTech Connect (OSTI)

    Roederer, Ian U.; Preston, George W.; Thompson, Ian B.; Shectman, Stephen A.; Sneden, Christopher

    2014-04-01

    Recent studies suggest that metal-poor stars enhanced in carbon but containing low levels of neutron-capture elements may have been among the first to incorporate the nucleosynthesis products of the first generation of stars. We have observed 16 stars with enhanced carbon or nitrogen using the MIKE Spectrograph on the Magellan Telescopes at Las Campanas Observatory and the Tull Spectrograph on the Smith Telescope at McDonald Observatory. We present radial velocities, stellar parameters, and detailed abundance patterns for these stars. Strontium, yttrium, zirconium, barium, europium, ytterbium, and other heavy elements are detected. In four stars, these heavy elements appear to have originated in some form of r-process nucleosynthesis. In one star, a partial s-process origin is possible. The origin of the heavy elements in the rest of the sample cannot be determined unambiguously. The presence of elements heavier than the iron group offers further evidence that zero-metallicity rapidly rotating massive stars and pair instability supernovae did not contribute substantial amounts of neutron-capture elements to the regions where the stars in our sample formed. If the carbon- or nitrogen-enhanced metal-poor stars with low levels of neutron-capture elements were enriched by products of zero-metallicity supernovae only, then the presence of these heavy elements indicates that at least one form of neutron-capture reaction operated in some of the first stars.

  1. DIRECT DETECTIONS OF YOUNG STARS IN NEARBY ELLIPTICAL GALAXIES

    SciTech Connect (OSTI)

    Ford, H. Alyson; Bregman, Joel N.

    2013-06-20

    Small amounts of star formation in elliptical galaxies are suggested by several results: surprisingly young ages from optical line indices, cooling X-ray gas, and mid-infrared dust emission. Such star formation has previously been difficult to directly detect, but using ultraviolet Hubble Space Telescope Wide Field Camera 3 imaging, we have identified individual young stars and star clusters in four nearby ellipticals. Ongoing star formation is detected in all galaxies, including three ellipticals that have previously exhibited potential signposts of star-forming conditions (NGC 4636, NGC 4697, and NGC 4374), as well as the typical ''red and dead'' NGC 3379. The current star formation in our closest targets, where we are most complete, is between 2.0 and 9.8 Multiplication-Sign 10{sup -5} M{sub Sun} yr{sup -1}. The star formation history was roughly constant from 0.5 to 1.5 Gyr (at (3-5) Multiplication-Sign 10{sup -4} M{sub Sun} yr{sup -1}), but decreased by a factor of several in the past 0.3 Gyr. Most star clusters have a mass between 10{sup 2} and 10{sup 4} M{sub Sun }. The specific star formation rates of {approx}10{sup -16} yr{sup -1} (at the present day) or {approx}10{sup -14} yr{sup -1} (when averaging over the past Gyr) imply that a fraction 10{sup -8} of the stellar mass is younger than 100 Myr and 10{sup -5} is younger than 1 Gyr, quantifying the level of frosting of recent star formation over the otherwise passive stellar population. There is no obvious correlation between either the presence or spatial distribution of postulated star formation indicators and the star formation we detect.

  2. THE MOST METAL-POOR STARS. II. CHEMICAL ABUNDANCES OF 190 METAL-POOR STARS INCLUDING 10 NEW STARS WITH [Fe/H] {<=} -3.5 , ,

    SciTech Connect (OSTI)

    Yong, David; Norris, John E.; Bessell, M. S.; Asplund, M.; Christlieb, N.; Beers, Timothy C.; Barklem, P. S.; Frebel, Anna; Ryan, S. G. E-mail: jen@mso.anu.edu.au E-mail: martin@mso.anu.edu.au E-mail: beers@pa.msu.edu E-mail: afrebel@mit.edu

    2013-01-01

    We present a homogeneous chemical abundance analysis of 16 elements in 190 metal-poor Galactic halo stars (38 program and 152 literature objects). The sample includes 171 stars with [Fe/H] {<=} -2.5, of which 86 are extremely metal poor, [Fe/H] {<=} -3.0. Our program stars include 10 new objects with [Fe/H] {<=} -3.5. We identify a sample of 'normal' metal-poor stars and measure the trends between [X/Fe] and [Fe/H], as well as the dispersion about the mean trend for this sample. Using this mean trend, we identify objects that are chemically peculiar relative to 'normal' stars at the same metallicity. These chemically unusual stars include CEMP-no objects, one star with high [Si/Fe], another with high [Ba/Sr], and one with unusually low [X/Fe] for all elements heavier than Na. The Sr and Ba abundances indicate that there may be two nucleosynthetic processes at lowest metallicity that are distinct from the main r-process. Finally, for many elements, we find a significant trend between [X/Fe] versus T {sub eff}, which likely reflects non-LTE and/or three-dimensional effects. Such trends demonstrate that care must be exercised when using abundance measurements in metal-poor stars to constrain chemical evolution and/or nucleosynthesis predictions.

  3. STAR FORMATION AROUND SUPERGIANT SHELLS IN THE LARGE MAGELLANIC CLOUD

    SciTech Connect (OSTI)

    Book, Laura G.; Chu Youhua; Gruendl, Robert A.; Fukui, Yasuo

    2009-03-15

    We examine the recent star formation associated with four supergiant shells in the Large Magellanic Cloud (LMC): LMC 1, 4, 5, and 6, which have been shown to have simple expanding-shell structures. H II regions and OB associations are used to infer star formation in the last few Myr, while massive young stellar objects reveal the current ongoing star formation. Distributions of ionized H I and molecular components of the interstellar gas are compared with the sites of recent and current star formation to determine whether triggering has taken place. We find that a great majority of the current star formation has occurred in gravitationally unstable regions, and that evidence of triggered star formation is prevalent at both large and local scales.

  4. [?/Fe]ABUNDANCES OF FOUR OUTER M31 HALO STARS

    SciTech Connect (OSTI)

    Vargas, Luis C.; Geha, Marla; Tollerud, Erik J. [Department of Astronomy, Yale University, 260 Whitney Avenue, New Haven, CT 06511 (United States); Gilbert, Karoline M. [Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States); Kirby, Evan N. [California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125 (United States); Guhathakurta, Puragra, E-mail: luis.vargas@yale.edu [UCO/Lick Observatory and Department of Astronomy and Astrophysics, University of California, 1156 High Street, Santa Cruz, CA 95064 (United States)

    2014-12-10

    We present alpha element to iron abundance ratios, [?/Fe], for four stars in the outer stellar halo of the Andromeda Galaxy (M31). The stars were identified as high-likelihood field halo stars by Gilbert et al. and lie at projected distances between 70 and 140 kpc from M31's center. These are the first alpha abundances measured for a halo star in a galaxy beyond the Milky Way. The stars range in metallicity between [Fe/H] = 2.2 and [Fe/H] = 1.4. The sample's average [?/Fe] ratio is +0.20 0.20. The best-fit average value is elevated above solar, which is consistent with rapid chemical enrichment from Type II supernovae. The mean [?/Fe] ratio of our M31 outer halo sample agrees (within the uncertainties) with that of Milky Way inner/outer halo stars that have a comparable range of [Fe/H].

  5. Continuous-time quantum walks on star graphs

    SciTech Connect (OSTI)

    Salimi, S.

    2009-06-15

    In this paper, we investigate continuous-time quantum walk on star graphs. It is shown that quantum central limit theorem for a continuous-time quantum walk on star graphs for N-fold star power graph, which are invariant under the quantum component of adjacency matrix, converges to continuous-time quantum walk on K{sub 2} graphs (complete graph with two vertices) and the probability of observing walk tends to the uniform distribution.

  6. Creating a Star on Earth | Department of Energy

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

    a Star on Earth Creating a Star on Earth March 5, 2014 - 11:45am Addthis In the video above, learn how scientists at the Princeton Plasma Physics Lab are creating a star on Earth in the National Spherical Torus Experiment (NSTX), a magnetic fusion device that is used to study the physics principles of spherically shaped plasmas. | Video by Matty Greene, Energy Department. Ben Dotson Ben Dotson Former Project Coordinator for Digital Reform, Office of Public Affairs Matty Greene Matty Greene

  7. NASA features LLNL star-formation simulations | National Nuclear Security

    National Nuclear Security Administration (NNSA)

    Administration | (NNSA) NASA features LLNL star-formation simulations Friday, January 29, 2016 - 5:56pm NNSA Blog These high performance computing (HPC) simulations of star formation account for a broad range of physical processes, including: gravity, supersonic turbulence, hydrodynamics, outflows, magnetic fields, chemistry and ionizing and non-ionizing radiation. Image courtesy of Pak Shing Li/ University of California, Berkeley High performance computing (HPC) simulations exploring star

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

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

    Requirements | Department of Energy National Program Requirements ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program Requirements ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program Requirements energy_star_v3_nat_program_rqmnts_reV07.pdf (217.46 KB) More Documents & Publications DOE Zero Energy Ready Home National Program Requirements (Rev. 05) DOE Zero Energy Ready Home National Program Requirements (Rev. 04) California DOE ZERH Program Requiremets

  9. ENERGY STAR Webinar: Portfolio Manager 101 | Department of Energy

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

    101 ENERGY STAR Webinar: Portfolio Manager 101 August 23, 2016 1:00PM to 2:00PM EDT Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will introduce and demonstrate the EPA's ENERGY STAR Portfolio Manager tool. Attendees will learn how to navigate Portfolio Manager, add a property and enter details about it, enter energy and water consumption data, and more.

  10. Los Alamos National Laboratory receives Star Status recognition for safety

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

    excellence from Department of Energy LANL receives recognition for safety excellence Los Alamos National Laboratory receives Star Status recognition for safety excellence from Department of Energy Los Alamos becomes the largest site in the DOE complex to receive VPP Star Status. October 8, 2014 Officials from the Department of Energy and the National Nuclear Security Administration joined Laboratory managers and employees at a VPP Star flag raising ceremony. Officials from the Department of

  11. Star cell type core configuration for structural sandwich materials

    DOE Patents [OSTI]

    Christensen, R.M.

    1995-08-01

    A new pattern for cellular core material used in sandwich type structural materials is disclosed. The new pattern involves star shaped cells intermixed with hexagonal shaped cells. The new patterned cellular core material includes star shaped cells interconnected at points thereof and having hexagonal shape cells positioned adjacent the star points. The new pattern allows more flexibility and can conform more easily to curved shapes. 3 figs.

  12. Bradbury Science Museum partnering in national Blue Star Museums program

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

    Blue Star Museums program Bradbury Science Museum partnering in national Blue Star Museums program Blue Star Museums program to host active duty military personnel and their families from Memorial Day, May 27, through Labor Day, Sept. 2. May 22, 2013 The museum is open daily except Thanksgiving, Christmas and New Year's Day. The museum is open daily except Thanksgiving, Christmas and New Year's Day. Contact Steve Sandoval Communications Office (505) 665-9206 Email The museum already has a

  13. Home Performance with ENERGY STAR | Department of Energy

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

    STAR Home Performance with ENERGY STAR Slides presented in the "What's Working in Residential Energy Efficiency Upgrade Programs Conference - Promising Approaches and Lessons Learned" on May 20, 2011 in Washington, D.C. Home Performance with ENERGY STAR (119.32 KB) More Documents & Publications Quality Control, Standardization of Upgrades, and Workforce Expectations Keys to Successful Quality Assurance and Quality Control Programs (101) EERE FY 2008-2012 Budget: Weatherization and

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

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

    ENERGY STAR Certified Homes, Version 3 (Rev. 07) National Program Requirements PDF icon energystarv3natprogramrqmntsreV07.pdf More Documents & Publications DOE Zero Energy ...

  15. The Energy of Star Wars: A Google+ Hangout

    Broader source: Energy.gov [DOE]

    On June 12, 2015, the Department of Energy hosted a live Google+ Hangout focusing on energy in the Star Wars movies.

  16. Pair instability supernovae of very massive population III stars...

    Office of Scientific and Technical Information (OSTI)

    strong reverse shock forms thatmore drives the growth of Rayleigh-Taylor instabilities. ... ANALYSIS; OXYGEN; QUASARS; RAYLEIGH-TAYLOR INSTABILITY; RED GIANT STARS; RED SHIFT; ...

  17. PEPCO- Home Performance with ENERGY STAR Incentive Program

    Broader source: Energy.gov [DOE]

    The Potomac Electric Power Company (PEPCO) offers the Home Performance with Energy Star Program which provides incentives for residential customers who have audits performed by participating...

  18. Scattering from Star Polymers including Excluded Volume Effects

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

    Li, Xin; Do, Changwoo; Liu, Yun; Hong, Kunlun; Smith, Greg; Chen, Wei-Ren

    2014-01-01

    In this work we present a new model for the form factor of a star polymer consisting of self-avoiding branches. This new model incorporates excluded volume effects and is derived from the two point correlation function for a star polymer.. We compare this model to small angle neutron scattering (SANS) measurements from polystyrene (PS) stars immersed in a good solvent, tetrahydrofuran (THF). It is shown that this model provides a good description of the scattering signature originating from the excluded volume effect and it explicitly elucidates the connection between the global conformation of a star polymer and the local stiffnessmore » of its constituent branch.« less

  19. Aircraft Integration and Flight Testing of 4STAR (Technical Report...

    Office of Scientific and Technical Information (OSTI)

    integrated the Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research (4STAR-Air) instrument for flight operation aboard Battelle's G-1 aircraft and conducted a ...

  20. DayStar Solar LLC formerly International Energy Trading LLC ...

    Open Energy Info (EERE)

    LLC formerly International Energy Trading LLC Jump to: navigation, search Name: DayStar Solar LLC (formerly International Energy Trading LLC) Place: Grass Valley, California Zip:...

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

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

    Comment submitted by Hoshizaki America, Inc. regarding the Energy Star Verification Testing Program Comment submitted by the North American Association of Food Equipment ...

  2. What do you get when two neutron stars merge?

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

    What do you get when two neutron stars merge? What do you get when two neutron stars merge? Led by Chris Fryer of the University of Arizona and the Los Alamos National Laboratory, a group of researchers undertook a highly collaborative study to better understand the fates of NS-NS mergers. November 8, 2015 Illustration of a binary neutron star system in the process of merging. The remnant formed by this merger could be either a neutron star or a black hole, determining whether it launches a

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

    Office of Legacy Management (LM)

    Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F23261 Sampling Date: 04... Test results contained within this data package meet the requirements of the National ...

  4. DOE Science Showcase - Startup Stars | OSTI, US Dept of Energy...

    Office of Scientific and Technical Information (OSTI)

    DOE Science Showcase - Startup Stars The Next Top Energy Innovator Iowa Powder Atomization ... Energy Department Technology Transfer Programs Visit the Science Showcase homepage. Last ...

  5. Delmarva Power- Home Performance with ENERGY STAR Incentive Program

    Broader source: Energy.gov [DOE]

    Delmarva Power and Light Company offers the Home Performance with Energy Star Program, which provides incentives for residential customers who have audits performed by participating contractors. ...

  6. MHK Technologies/CurrentStar | Open Energy Information

    Open Energy Info (EERE)

    Technology Profile Primary Organization Bourne Energy Technology Type Click here Axial Flow Turbine Technology Description The CurrentStar series is designed to harness the...

  7. STAR Images: Image gallery from the Solenoidal Tracker at RHIC

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

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

  8. ENERGY STAR Webinar: Energy Savings Plus Health: Indoor Air Quality...

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

    Energy Savings Plus Health: Indoor Air Quality Guidelines for School Building Upgrades ENERGY STAR Webinar: Energy Savings Plus Health: Indoor Air Quality Guidelines for School...

  9. EERE EnergyStar State Allocations | Department of Energy

    Energy Savers [EERE]

    Allocations PDF icon EEEnergyStarStateAllocations.pdf More Documents & Publications State Energy Efficient Appliance Rebate Program (SEEARP) American Recovery and...

  10. EPA, DOE Announce New Steps to Strengthen ENERGY STAR | Department...

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

    ... Independent Review Finds 98% Compliance Violations of the ENERGY STAR label tend to get big media attention, which is good - because it provides a strong disincentive for ...

  11. Scattering from Star Polymers including Excluded Volume Effects

    SciTech Connect (OSTI)

    Li, Xin [ORNL; Do, Changwoo [ORNL; Liu, Yun [National Institute of Standards and Technology (NIST); Sanchez-Diaz, Luis E [ORNL; Hong, Kunlun [ORNL; Smith, Greg [ORNL; Chen, Wei-Ren [ORNL

    2014-01-01

    In this work we present a new model for the form factor of a star polymer consisting of self-avoiding branches. This new model incorporates excluded volume effects and is derived from the two point correlation function for a star polymer.. We compare this model to small angle neutron scattering (SANS) measurements from polystyrene (PS) stars immersed in a good solvent, tetrahydrofuran (THF). It is shown that this model provides a good description of the scattering signature originating from the excluded volume effect and it explicitly elucidates the connection between the global conformation of a star polymer and the local stiffness of its constituent branch.

  12. NEW YOUNG STAR CANDIDATES IN CG4 AND Sa101

    SciTech Connect (OSTI)

    Rebull, L. M.; Laine, S.; Laher, R.; Legassie, M.; Hoette, V.; Kim, J. S.; Foster, M.; Mallory, C. R.; McCarron, K.; Sherry, W. H.

    2011-07-15

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

  13. Amplitude Variability in gamma Dor and delta Sct Stars Observed...

    Office of Scientific and Technical Information (OSTI)

    Title: Amplitude Variability in gamma Dor and delta Sct Stars Observed by Kepler The NASA ... Research Org: Los Alamos National Laboratory (LANL) Sponsoring Org: NASA Country of ...

  14. Energy Star Lighting Fixtures: How Does THAT Work?

    Broader source: Energy.gov [DOE]

    If you're considering replacing your indoor or outdoor home lighting, you might want to give an ENERGY STAR fixture a shot.

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

    Office of Legacy Management (LM)

    ... Technical Report for S M Stoller Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F23505 Sampling Dates: 041504 - 041604 Report to: S M Stoller ...

  16. UPPER BOUND ON THE FIRST STAR FORMATION HISTORY (Journal Article...

    Office of Scientific and Technical Information (OSTI)

    Citation Details In-Document Search Title: UPPER BOUND ON THE FIRST STAR FORMATION HISTORY Our understanding of the nature of the extragalactic background light (EBL) has improved ...

  17. DayStar Technologies Inc | Open Energy Information

    Open Energy Info (EERE)

    Technologies Inc Jump to: navigation, search Name: DayStar Technologies Inc Place: Santa Clara, California Zip: 95054 Product: US-based manufacturer of CIGS cells and modules....

  18. The Federal Guiding Principles Checklist in ENERGY STAR Portfolio

    Broader source: Energy.gov [DOE]

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

  19. Direct imaging of multiple planets orbiting the star HR 8799...

    Office of Scientific and Technical Information (OSTI)

    Direct imaging of multiple planets orbiting the star HR 8799 Citation Details In-Document ... Resource Type: Journal Article Resource Relation: Journal Name: Science, vol. 322, no. ...

  20. The evolutionary tracks of young massive star clusters

    SciTech Connect (OSTI)

    Pfalzner, S.; Steinhausen, M.; Vincke, K.; Menten, K.; Parmentier, G.

    2014-10-20

    Stars mostly form in groups consisting of a few dozen to several ten thousand members. For 30 years, theoretical models have provided a basic concept of how such star clusters form and develop: they originate from the gas and dust of collapsing molecular clouds. The conversion from gas to stars being incomplete, the leftover gas is expelled, leading to cluster expansion and stars becoming unbound. Observationally, a direct confirmation of this process has proved elusive, which is attributed to the diversity of the properties of forming clusters. Here we take into account that the true cluster masses and sizes are masked, initially by the surface density of the background and later by the still present unbound stars. Based on the recent observational finding that in a given star-forming region the star formation efficiency depends on the local density of the gas, we use an analytical approach combined with N-body simulations to reveal evolutionary tracks for young massive clusters covering the first 10 Myr. Just like the Hertzsprung-Russell diagram is a measure for the evolution of stars, these tracks provide equivalent information for clusters. Like stars, massive clusters form and develop faster than their lower-mass counterparts, explaining why so few massive cluster progenitors are found.

  1. North Star, Delaware: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Star, Delaware: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 39.7612226, -75.7191006 Show Map Loading map... "minzoom":false,"mappingservice...

  2. Home Performance with ENERGY STAR | Department of Energy

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

    by utilities or by NYSERDA, including and the NYSERDA Assisted Home Performance with ENERGY STAR. For further information on this program, please consult the program...

  3. Set and Save with Energy Star (Video) | Open Energy Information

    Open Energy Info (EERE)

    and Save with Energy Star (Video) Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Spain Installed Wind Capacity Website Focus Area: Renewable Energy Topics: Market...

  4. Energy Star Building Upgrade Value Calculator | Open Energy Informatio...

    Open Energy Info (EERE)

    Upgrade Value Calculator Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Energy Star Building Upgrade Value Calculator (for Office Properties) AgencyCompany...

  5. Blue Star Energy Services (Maryland) | Open Energy Information

    Open Energy Info (EERE)

    Maryland) Jump to: navigation, search Name: Blue Star Energy Services Place: Maryland References: EIA Form EIA-861 Final Data File for 2010 - File220101 EIA Form 861 Data...

  6. Fairbanks North Star Borough, Alaska: Energy Resources | Open...

    Open Energy Info (EERE)

    Fairbanks North Star Borough, Alaska: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 64.9526102, -146.4744155 Show Map Loading map......

  7. MHK Technologies/TidalStar | Open Energy Information

    Open Energy Info (EERE)

    search << Return to the MHK database homepage TidalStar.jpg Technology Profile Primary Organization Bourne Energy Technology Type Click here Axial Flow Turbine...

  8. Columbia Water & Light- Home Performance with ENERGY STAR Loan

    Office of Energy Efficiency and Renewable Energy (EERE)

    The Columbia Water & Light (CWL) Home Performance with ENERGY STAR program allows Columbia residents to finance energy efficiency improvements to homes with affordable, low-interest loans with...

  9. Evaluation Prompts ENERGY STAR Program to Replace Web Tool, Saving...

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

    Prompts ENERGY STAR Program to Replace Web Tool, Saving 90 Percent of Annual Costs A ... program managers decided to drop the web tool, eventually replacing it with a ...

  10. SIMILARITIES IN POPULATIONS OF STAR CLUSTERS

    SciTech Connect (OSTI)

    Fall, S. Michael; Chandar, Rupali E-mail: rupali.chandar@utoledo.edu

    2012-06-20

    We compare the observed mass functions and age distributions of star clusters in six well-studied galaxies: the Milky Way, Magellanic Clouds, M83, M51, and Antennae. In combination, these distributions span wide ranges of mass and age: 10{sup 2} {approx}< M/M{sub Sun} {approx}< 10{sup 6} and 10{sup 6} {approx}< {tau}/yr {approx}< 10{sup 9}. We confirm that the distributions are well represented by power laws: dN/dM{proportional_to}M{sup {beta}} with {beta} Almost-Equal-To -1.9 and dN/d{tau}{proportional_to}{tau}{sup {gamma}} with {gamma} Almost-Equal-To -0.8. The mass and age distributions are approximately independent of each other, ruling out simple models of mass-dependent disruption. As expected, there are minor differences among the exponents at a level close to the true uncertainties, {epsilon}{sub {beta}} {approx} {epsilon}{sub {gamma}} {approx} 0.1-0.2. However, the overwhelming impression is the similarity of the mass functions and age distributions of clusters in these different galaxies, including giant and dwarf, quiescent and interacting galaxies. This is an important empirical result, justifying terms such as 'universal' or 'quasi-universal'. We provide a partial theoretical explanation for these observations in terms of physical processes operating during the formation and disruption of the clusters, including star formation and feedback, subsequent stellar mass loss, and tidal interactions with passing molecular clouds. A full explanation will require additional information about the molecular clumps and star clusters in galaxies beyond the Milky Way.

  11. A-Power Energy | Open Energy Information

    Open Energy Info (EERE)

    Shenyang Power Group http:blogs.wsj.comenvironmentalcapital20091029lone-star-meet-red-star-chinas-15-billion-wind-power-deal-in-texas "About A-Power: A-Power Energy...

  12. The best and brightest metal-poor stars

    SciTech Connect (OSTI)

    Schlaufman, Kevin C.; Casey, Andrew R., E-mail: kschlauf@mit.edu, E-mail: arc@ast.cam.ac.uk [Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139 (United States)

    2014-12-10

    The chemical abundances of large samples of extremely metal-poor (EMP) stars can be used to investigate metal-free stellar populations, supernovae, and nucleosynthesis as well as the formation and galactic chemical evolution of the Milky Way and its progenitor halos. However, current progress on the study of EMP stars is being limited by their faint apparent magnitudes. The acquisition of high signal-to-noise spectra for faint EMP stars requires a major telescope time commitment, making the construction of large samples of EMP star abundances prohibitively expensive. We have developed a new, efficient selection that uses only public, all-sky APASS optical, 2MASS near-infrared, and WISE mid-infrared photometry to identify bright metal-poor star candidates through their lack of molecular absorption near 4.6 microns. We have used our selection to identify 11,916 metal-poor star candidates with V < 14, increasing the number of publicly available candidates by more than a factor of five in this magnitude range. Their bright apparent magnitudes have greatly eased high-resolution follow-up observations that have identified seven previously unknown stars with [Fe/H] ? 3.0. Our follow-up campaign has revealed that 3.8{sub ?1.1}{sup +1.3}% of our candidates have [Fe/H] ? 3.0 and 32.5{sub ?2.9}{sup +3.0}% have 3.0 ? [Fe/H] ? 2.0. The bulge is the most likely location of any existing Galactic Population III stars, and an infrared-only variant of our selection is well suited to the identification of metal-poor stars in the bulge. Indeed, two of our confirmed metal-poor stars with [Fe/H] ? 2.7 are within about 2 kpc of the Galactic center. They are among the most metal-poor stars known in the bulge.

  13. STAR FORMATION IN NUCLEAR RINGS OF BARRED GALAXIES

    SciTech Connect (OSTI)

    Seo, Woo-Young; Kim, Woong-Tae E-mail: wkim@astro.snu.ac.kr

    2013-06-01

    Nuclear rings in barred galaxies are sites of active star formation. We use hydrodynamic simulations to study the temporal and spatial behavior of star formation occurring in nuclear rings of barred galaxies where radial gas inflows are triggered solely by a bar potential. The star formation recipes include a density threshold, an efficiency, conversion of gas to star particles, and delayed momentum feedback via supernova explosions. We find that the star formation rate (SFR) in a nuclear ring is roughly equal to the mass inflow rate to the ring, while it has a weak dependence on the total gas mass in the ring. The SFR typically exhibits a strong primary burst followed by weak secondary bursts before declining to very small values. The primary burst is associated with the rapid gas infall to the ring due to the bar growth, while the secondary bursts are caused by re-infall of the ejected gas from the primary burst. While star formation in observed rings persists episodically over a few Gyr, the duration of active star formation in our models lasts for only about half of the bar growth time, suggesting that the bar potential alone is unlikely to be responsible for gas supply to the rings. When the SFR is low, most star formation occurs at the contact points between the ring and the dust lanes, leading to an azimuthal age gradient of young star clusters. When the SFR is large, on the other hand, star formation is randomly distributed over the whole circumference of the ring, resulting in no apparent azimuthal age gradient. Since the ring shrinks in size with time, star clusters also exhibit a radial age gradient, with younger clusters found closer to the ring. The cluster mass function is well described by a power law, with a slope depending on the SFR. Giant gas clouds in the rings have supersonic internal velocity dispersions and are gravitationally bound.

  14. Low-Interest Rates Entice Philadelphians to Reach for the Stars...

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

    For example, "Gold Star" projects, which are guided by an energy assessment and consist of ... As an alternative to the Gold Star level, the Silver Star allows homeowners to initiate ...

  15. Radial velocities of southern visual multiple stars

    SciTech Connect (OSTI)

    Tokovinin, Andrei; Pribulla, Theodor; Fischer, Debra E-mail: pribulla@ta3.sk

    2015-01-01

    High-resolution spectra of visual multiple stars were taken in 20082009 to detect or confirm spectroscopic subsystems and to determine their orbits. Radial velocities of 93 late-type stars belonging to visual multiple systems were measured by numerical cross-correlation. We provide the individual velocities, the width, and the amplitude of the Gaussians that approximate the correlations. The new information on the multiple systems resulting from these data is discussed. We discovered double-lined binaries in HD 41742B, HD 56593C, and HD 122613AB, confirmed several other known subsystems, and constrained the existence of subsystems in some visual binaries where both components turned out to have similar velocities. The orbits of double-lined subsystems with periods of 148 and 13 days are computed for HD 104471 Aa,Ab and HD 210349 Aa,Ab, respectively. We estimate individual magnitudes and masses of the components in these triple systems and update the outer orbit of HD 104471 AB.

  16. Star formation and substructure in galaxy clusters

    SciTech Connect (OSTI)

    Cohen, Seth A.; Hickox, Ryan C.; Wegner, Gary A.; Einasto, Maret; Vennik, Jaan

    2014-03-10

    We investigate the relationship between star formation (SF) and substructure in a sample of 107 nearby galaxy clusters using data from the Sloan Digital Sky Survey. Several past studies of individual galaxy clusters have suggested that cluster mergers enhance cluster SF, while others find no such relationship. The SF fraction in multi-component clusters (0.228 0.007) is higher than that in single-component clusters (0.175 0.016) for galaxies with M{sub r}{sup 0.1}star-forming galaxies increases with clustercentric distance and decreases with local galaxy number density, and multi-component clusters show a higher SF fraction than single-component clusters at almost all clustercentric distances and local densities. Comparing the SF fraction in individual clusters to several statistical measures of substructure, we find weak, but in most cases significant at greater than 2?, correlations between substructure and SF fraction. These results could indicate that cluster mergers may cause weak but significant SF enhancement in clusters, or unrelaxed clusters exhibit slightly stronger SF due to their less evolved states relative to relaxed clusters.

  17. HOT GAS LINES IN T TAURI STARS

    SciTech Connect (OSTI)

    Ardila, David R.; Herczeg, Gregory J.; Gregory, Scott G.; Hillenbrand, Lynne A.; Ingleby, Laura; Bergin, Edwin; Bethell, Thomas; Calvet, Nuria; France, Kevin; Brown, Alexander; Edwards, Suzan; Johns-Krull, Christopher; Linsky, Jeffrey L.; Yang, Hao; Valenti, Jeff A.; Abgrall, Herve; Alexander, Richard D.; Brown, Joanna M.; Espaillat, Catherine; Hussain, Gaitee; and others

    2013-07-01

    For Classical T Tauri Stars (CTTSs), the resonance doublets of N V, Si IV, and C IV, as well as the He II 1640 A line, trace hot gas flows and act as diagnostics of the accretion process. In this paper we assemble a large high-resolution, high-sensitivity data set of these lines in CTTSs and Weak T Tauri Stars (WTTSs). The sample comprises 35 stars: 1 Herbig Ae star, 28 CTTSs, and 6 WTTSs. We find that the C IV, Si IV, and N V lines in CTTSs all have similar shapes. We decompose the C IV and He II lines into broad and narrow Gaussian components (BC and NC). The most common (50%) C IV line morphology in CTTSs is that of a low-velocity NC together with a redshifted BC. For CTTSs, a strong BC is the result of the accretion process. The contribution fraction of the NC to the C IV line flux in CTTSs increases with accretion rate, from {approx}20% to up to {approx}80%. The velocity centroids of the BCs and NCs are such that V{sub BC} {approx}> 4 V{sub NC}, consistent with the predictions of the accretion shock model, in at most 12 out of 22 CTTSs. We do not find evidence of the post-shock becoming buried in the stellar photosphere due to the pressure of the accretion flow. The He II CTTSs lines are generally symmetric and narrow, with FWHM and redshifts comparable to those of WTTSs. They are less redshifted than the CTTSs C IV lines, by {approx}10 km s{sup -1}. The amount of flux in the BC of the He II line is small compared to that of the C IV line, and we show that this is consistent with models of the pre-shock column emission. Overall, the observations are consistent with the presence of multiple accretion columns with different densities or with accretion models that predict a slow-moving, low-density region in the periphery of the accretion column. For HN Tau A and RW Aur A, most of the C IV line is blueshifted suggesting that the C IV emission is produced by shocks within outflow jets. In our sample, the Herbig Ae star DX Cha is the only object for which we find a

  18. LITHIUM ABUNDANCES OF EXTREMELY METAL-POOR TURNOFF STARS

    SciTech Connect (OSTI)

    Aoki, Wako; Inoue, Susumu; Barklem, Paul S.; Beers, Timothy C.; Christlieb, Norbert; Perez, Ana E. GarcIa; Norris, John E.; Carollo, Daniela E-mail: Paul.Barklem@physics.uu.se E-mail: N.Christlieb@lsw.uni-heidelberg.de E-mail: jen@mso.anu.edu.au E-mail: inoue@tap.scphys.kyoto-u.ac.jp

    2009-06-20

    We have determined Li abundances for eleven metal-poor turnoff stars, among which eight have [Fe/H] <-3, based on LTE analyses of high-resolution spectra obtained with the High Dispersion Spectrograph on the Subaru Telescope. The Li abundances for four of these eight stars are determined for the first time by this study. Effective temperatures are determined by a profile analysis of H{alpha} and H{beta}. While seven stars have Li abundances as high as the Spite Plateau value, the remaining four objects with [Fe/H] <-3 have A(Li) =log (Li/H)+ 12 {approx}< 2.0, confirming the existence of extremely metal-poor (EMP) turnoff stars having low Li abundances, as reported by previous work. The average of the Li abundances for stars with [Fe/H]<-3 is lower by 0.2 dex than that of the stars with higher metallicity. No clear constraint on the metallicity dependence or scatter of the Li abundances is derived from our measurements for the stars with [Fe/H]<-3. Correlations of the Li abundance with effective temperatures, with abundances of Na, Mg, and Sr, and with the kinematical properties are investigated, but no clear correlation is seen in the EMP star sample.

  19. Overview of results from the STAR experiment at RHIC.

    SciTech Connect (OSTI)

    Filimonov, Kirill; STAR Collaboration

    2003-06-20

    The Relativistic Heavy-Ion Collider (RHIC) provides Au+Au collisions at energies up to {radical}s{sub NN} = 200 GeV. STAR experiment was designed and constructed to investigate the behavior of strongly interacting matter at high energy density. An overview of some of the recent results from the STAR collaboration is given.

  20. ENERGY STAR for Homes- Building America Top Innovation

    Broader source: Energy.gov [DOE]

    This Building America Innovations profile describes Building Americas technical support to ENERGY STAR for Homes, which has labeled more than 1.3 million ENERGY STAR homes that have delivered $23 billion in energy cost savings and avoided 210 million tons of green-house emissions.

  1. THE HABITABLE ZONES OF PRE-MAIN-SEQUENCE STARS

    SciTech Connect (OSTI)

    Ramirez, Ramses M.; Kaltenegger, Lisa

    2014-12-20

    We calculate the pre-main-sequence habitable zone (HZ) for stars of spectral classes F-M. The spatial distribution of liquid water and its change during the pre-main-sequence phase of protoplanetary systems is important for understanding how planets become habitable. Such worlds are interesting targets for future missions because the coolest stars could provide habitable conditions for up to 2.5 billion years post-accretion. Moreover, for a given star type, planetary systems are more easily resolved because of higher pre-main-sequence stellar luminosities, resulting in larger planet-star separation for cool stars than is the case for the traditional main-sequence (MS) HZ. We use one-dimensional radiative-convective climate and stellar evolutionary models to calculate pre-main-sequence HZ distances for F1-M8 stellar types. We also show that accreting planets that are later located in the traditional MS HZ orbiting stars cooler than a K5 (including the full range of M stars) receive stellar fluxes that exceed the runaway greenhouse threshold, and thus may lose substantial amounts of water initially delivered to them. We predict that M-star planets need to initially accrete more water than Earth did, or, alternatively, have additional water delivered later during the long pre-MS phase to remain habitable. Our findings are also consistent with recent claims that Venus lost its water during accretion.

  2. Building America Top Innovations 2012: ENERGY STAR for Homes Support

    SciTech Connect (OSTI)

    none,

    2013-01-01

    This Building America Top Innovations profile describes Building Americas technical support to ENERGY STAR for Homes, which has labeled more than 1.3 million ENERGY STAR homes that have delivered $23 billion in energy cost savings and avoided 210 million tons of green-house emissions.

  3. STAR (Solenoidal Tracker at RHIC) Figures and Data

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

    The STAR Collaboration

    The primary physics task of STAR is to study the formation and characteristics of the quark-gluon plasma (QGP), a state of matter believed to exist at sufficiently high energy densities. STAR consists of several types of detectors, each specializing in detecting certain types of particles or characterizing their motion. These detectors work together in an advanced data acquisition and subsequent physics analysis that allows final statements to be made about the collision. The STAR Publications page provides access to all published papers by the STAR Collaboration, and many of them have separate links to the figures and data found in or supporting the paper. See also the data-rich summaries of the research at http://www.star.bnl.gov/central/physics/results/. [See also DDE00230

  4. INTERNAL GRAVITY WAVES IN MASSIVE STARS: ANGULAR MOMENTUM TRANSPORT

    SciTech Connect (OSTI)

    Rogers, T. M.; Lin, D. N. C.; McElwaine, J. N.; Lau, H. H. B. E-mail: lin@ucolick.org E-mail: hblau@astro.uni-bonn.de

    2013-07-20

    We present numerical simulations of internal gravity waves (IGW) in a star with a convective core and extended radiative envelope. We report on amplitudes, spectra, dissipation, and consequent angular momentum transport by such waves. We find that these waves are generated efficiently and transport angular momentum on short timescales over large distances. We show that, as in Earth's atmosphere, IGW drive equatorial flows which change magnitude and direction on short timescales. These results have profound consequences for the observational inferences of massive stars, as well as their long term angular momentum evolution. We suggest IGW angular momentum transport may explain many observational mysteries, such as: the misalignment of hot Jupiters around hot stars, the Be class of stars, Ni enrichment anomalies in massive stars, and the non-synchronous orbits of interacting binaries.

  5. THE STRUCTURE OF THE STAR-FORMING CLUSTER RCW 38

    SciTech Connect (OSTI)

    Winston, E.; Wolk, S. J.; Bourke, T. L.; Spitzbart, B.; Megeath, S. T.; Gutermuth, R.

    2011-12-20

    We present a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 {mu}m) is combined with Two Micron All Sky Survey near-IR data to identify young stellar objects (YSOs) by IR-excess emission from their circumstellar material. Chandra X-ray data are used to identify class III pre-main-sequence stars lacking circumstellar material. We identify 624 YSOs: 23 class 0/I and 90 flat spectrum protostars, 437 class II stars, and 74 class III stars. We also identify 29 (27 new) O star candidates over the IRAC field. Seventy-two stars exhibit IR-variability, including 7 class 0/I and 12 flat spectrum YSOs. A further 177 tentative candidates are identified by their location in the IRAC [3.6] versus [3.6]-[5.8] color-magnitude diagram. We find strong evidence of subclustering in the region. Three subclusters were identified surrounding the central cluster, with massive and variable stars in each subcluster. The central region shows evidence of distinct spatial distributions of the protostars and pre-main-sequence stars. A previously detected IR cluster, DB2001{sub O}bj36, has been established as a subcluster of RCW 38. This suggests that star formation in RCW 38 occurs over a more extended area than previously thought. The gas-to-dust ratio is examined using the X-ray derived hydrogen column density, N{sub H} and the K-band extinction, and found to be consistent with the diffuse interstellar medium, in contrast with Serpens and NGC 1333. We posit that the high photoionizing flux of massive stars in RCW 38 affects the agglomeration of the dust grains.

  6. STAR-FORMING GALAXY EVOLUTION IN NEARBY RICH CLUSTERS

    SciTech Connect (OSTI)

    Tyler, K. D.; Rieke, G. H.; Bai, L.

    2013-08-20

    Dense environments are known to quench star formation in galaxies, but it is still unknown what mechanism(s) are directly responsible. In this paper, we study the star formation of galaxies in A2029 and compare it to that of Coma, combining indicators at 24 {mu}m, H{alpha}, and UV down to rates of 0.03 M{sub Sun} yr{sup -1}. We show that A2029's star-forming galaxies follow the same mass-SFR relation as the field. The Coma cluster, on the other hand, has a population of galaxies with star formation rates (SFRs) significantly lower than the field mass-SFR relation, indicative of galaxies in the process of being quenched. Over half of these galaxies also host active galactic nuclei. Ram-pressure stripping and starvation/strangulation are the most likely mechanisms for suppressing the star formation in these galaxies, but we are unable to disentangle which is dominating. The differences we see between the two clusters' populations of star-forming galaxies may be related to their accretion histories, with A2029 having accreted its star-forming galaxies more recently than Coma. Additionally, many early-type galaxies in A2029 are detected at 24 {mu}m and/or in the far-UV, but this emission is not directly related to star formation. Similar galaxies have probably been classified as star forming in previous studies of dense clusters, possibly obscuring some of the effects of the cluster environment on true star-forming galaxies.

  7. A RAPIDLY EVOLVING REGION IN THE GALACTIC CENTER: WHY S-STARS THERMALIZE AND MORE MASSIVE STARS ARE MISSING

    SciTech Connect (OSTI)

    Chen, Xian; Amaro-Seoane, Pau E-mail: Pau.Amaro-Seoane@aei.mpg.de

    2014-05-10

    The existence of ''S-stars'' within a distance of 1'' from Sgr A* contradicts our understanding of star formation, due to Sgr A* 's forbiddingly violent environment. A suggested possibility is that they form far away and were brought in by some fast dynamical process, since they are young. Nonetheless, all conjectured mechanisms either fail to reproduce their eccentricities—without violating their young age—or cannot explain the problem of {sup i}nverse mass segregation{sup :} the fact that lighter stars (the S-stars) are closer to Sgr A* and more massive ones, Wolf-Rayet (WR) and O-stars, are farther out. In this Letter we propose that the mechanism responsible for both the distribution of the eccentricities and the paucity of massive stars is the Kozai-Lidov-like resonance induced by a sub-parsec disk recently discovered in the Galactic center. Considering that the disk probably extended to a smaller radius in the past, we show that in as short as (a few) 10{sup 6} yr, the stars populating the innermost 1'' region would redistribute in angular-momentum space and recover the observed ''super-thermal'' distribution. Meanwhile, WR and O-stars in the same region intermittently attain ample eccentricities that will lead to their tidal disruptions by the central massive black hole. Our results provide new evidences that Sgr A* was powered several millions years ago by an accretion disk as well as by tidal stellar disruptions.

  8. KNOW THE STAR, KNOW THE PLANET. II. SPECKLE INTERFEROMETRY OF EXOPLANET HOST STARS

    SciTech Connect (OSTI)

    Mason, Brian D.; Hartkopf, William I.; Raghavan, Deepak; Subasavage, John P.; Roberts, Lewis C.; Turner, Nils H.; Ten Brummelaar, Theo A. E-mail: wih@usno.navy.mil E-mail: jsubasavage@ctio.noao.edu E-mail: nils@chara-array.org

    2011-11-15

    A study of the host stars to exoplanets is important for understanding their environment. To that end, we report new speckle observations of a sample of exoplanet host primaries. The bright exoplanet host HD 8673 (= HIP 6702) is revealed to have a companion, although at this time we cannot definitively establish the companion as physical or optical. The observing lists for planet searches and for these observations have for the most part been pre-screened for known duplicity, so the detected binary fraction is lower than what would otherwise be expected. Therefore, a large number of double stars were observed contemporaneously for verification and quality control purposes, to ensure that the lack of detection of companions for exoplanet hosts was valid. In these additional observations, 10 pairs are resolved for the first time and 60 pairs are confirmed. These observations were obtained with the USNO speckle camera on the NOAO 4 m telescopes at both KPNO and CTIO from 2001 to 2010.

  9. STAR CLUSTERS IN A NUCLEAR STAR FORMING RING: THE DISAPPEARING STRING OF PEARLS

    SciTech Connect (OSTI)

    Visnen, Petri; Barway, Sudhanshu; Randriamanakoto, Zara

    2014-12-20

    An analysis of the star cluster population in a low-luminosity early-type galaxy, NGC2328, is presented. The clusters are found in a tight star forming nuclear spiral/ring pattern and we also identify a bar from structural two-dimensional decomposition. These massive clusters are forming very efficiently in the circumnuclear environment and they are young, possibly all less than 30 Myr of age. The clusters indicate an azimuthal age gradient, consistent with a ''pearls-on-a-string'' formation scenario, suggesting bar-driven gas inflow. The cluster mass function has a robust down turn at low masses at all age bins. Assuming clusters are born with a power-law distribution, this indicates extremely rapid disruption at timescales of just several million years. If found to be typical, it means that clusters born in dense circumnuclear rings do not survive to become old globular clusters in non-interacting systems.

  10. CIRCUMSTELLAR STRUCTURE AROUND EVOLVED STARS IN THE CYGNUS-X STAR FORMATION REGION

    SciTech Connect (OSTI)

    Kraemer, Kathleen E.; Price, Stephan D.

    2010-06-15

    We present observations of newly discovered 24 {mu}m circumstellar structures detected with MIPS around three evolved stars in the Cygnus-X star-forming region. One of the objects, BD+43 3710, has a bipolar nebula, possibly due to an outflow or a torus of material. A second, HBHA 4202-22, a Wolf-Rayet candidate, shows a circular shell of 24 {mu}m emission suggestive of either a limb-brightened shell or disk seen face-on. No diffuse emission was detected around either of these two objects in the Spitzer 3.6-8 {mu}m IRAC bands. The third object is the luminous blue variable candidate G79.29+0.46. We resolved the previously known inner ring in all four IRAC bands. The 24 {mu}m emission from the inner ring extends {approx}1.'2 beyond the shorter wavelength emission, well beyond what can be attributed to the difference in resolutions between MIPS and IRAC. Additionally, we have discovered an outer ring of 24 {mu}m emission, possibly due to an earlier episode of mass loss. For the two shell stars, we present the results of radiative transfer models, constraining the stellar and dust shell parameters. The shells are composed of amorphous carbon grains, plus polycyclic aromatic hydrocarbons in the case of G79.29+0.46. Both G79.29+0.46 and HBHA 4202-22 lie behind the main Cygnus-X cloud. Although G79.29+0.46 simply may be on the far side of the cloud, HBHA 4202-22 is unrelated to the Cygnus-X star formation region.

  11. Status and future directions of the ENERGY STAR program

    SciTech Connect (OSTI)

    Brown, Richard E.; Webber, Carrie A.; Koomey, Jonathan G.

    2000-06-19

    In 1992 the U.S. Environmental Protection Agency (EPA) introduced ENERGY STAR (registered trademark), a voluntary labeling program designed to identify and promote energy-efficient products, in order to reduce carbon dioxide emissions. Since then EPA, now in partnership with the U.S. Department of Energy (DOE), has expanded the program to cover nearly the entire buildings sector, spanning new homes, commercial buildings, residential heating and cooling equipment, major appliances, office equipment, commercial and residential lighting, and home electronics. This paper provides a snapshot of the ENERGY STAR program in the year 2000, including a general overview of the program, its accomplishments, and the possibilities for future development. First, we describe the products that are currently eligible for the ENERGY STAR label and the program mechanisms that EPA and DOE are using to promote these products. Second, we illustrate selected milestones achieved in some markets, and ways that EPA and DOE are responding to challenges or changes in certain markets. Third, we discuss the evolving ENERGY STAR brand strategy. Next, we explore ways in which ENERGY STAR interacts with and enhances other policies, such as appliance standards and regional market transformation collaboratives. We then discuss evaluation studies that EPA and DOE are undertaking to quantify the impact of the ENERGY STAR program. Finally, we discuss future areas of expansion for the ENERGY STAR program, including labeling of new products and integrated programs for commercial and existing residential buildings.

  12. Further stable neutron star models from f(R) gravity

    SciTech Connect (OSTI)

    Astashenok, Artyom V.; Capozziello, Salvatore; Odintsov, Sergei D. E-mail: capozziello@na.infn.it

    2013-12-01

    Neutron star models in perturbative f(R) gravity are considered with realistic equations of state. In particular, we consider the FPS, SLy and other equations of state and a case of piecewise equation of state for stars with quark cores. The mass-radius relations for f(R) = R+R(e{sup ?R/R{sub 0}}?1) model and for R{sup 2} models with logarithmic and cubic corrections are obtained. In the case of R{sup 2} gravity with cubic corrections, we obtain that at high central densities (? > 10?{sub ns}, where ?{sub ns} = 2.7 10{sup 14} g/cm{sup 3} is the nuclear saturation density), stable star configurations exist. The minimal radius of such stars is close to 9 km with maximal mass ? 1.9M{sub ?} (SLy equation). A similar situation takes place for AP4 and BSK20 EoS. Such an effect can give rise to more compact stars than in General Relativity. If observationally identified, such objects could constitute a formidable signature for modified gravity at astrophysical level. Another interesting result can be achieved in modified gravity with only a cubic correction. For some EoS, the upper limit of neutron star mass increases and therefore these EoS can describe realistic star configurations (although, in General Relativity, these EoS are excluded by observational constraints)

  13. Strategic Target Systems (STARS) environmental assessment. Supplement. Final report

    SciTech Connect (OSTI)

    Not Available

    1991-07-01

    The Strategic Target System program (STARS) uses a three-stage solid propellant guided missile. The missile integrates selected parts of the Navy retired Polaris A3 fleet ballistic missile with a substantial number of newly developed subsystems. STARS will be used for testing various developmental elements of the Strategic Defense Initiative System. STARS will fly a payload of either single or multiple reentry vehicles to the Broad Ocean Area or will be targeted for impact or for reentry. As part of the STARS development process, an EA was prepared. It concluded with a finding of no significant impact (FNSI). The Army determined that the STARS program would have no significant environmental impacts and that any potential impacts could be mitigated. However, as a result of lawsuits the court ordered that a supplemental study be conducted of the potential effects on the Kauai environment from hydrogen chloride released during STARS launches and that a determination be made as to whether the release of freon from the second stage of the STARS would violate the Hawaii Ozone Layer Protection Statute.

  14. RED CLUMP STARS IN THE SAGITTARIUS TIDAL STREAMS

    SciTech Connect (OSTI)

    Carrell, Kenneth; Chen Yuqin; Wilhelm, Ronald

    2012-07-15

    We have probed a section (l {approx} 150, b {approx} -60) of the trailing tidal arm of the Sagittarius dwarf spheroidal galaxy by identifying a sample of Red Clump (RC) stream stars. RC stars are not generally found in the halo field, but are found in significant numbers in both the Sagittarius galaxy and its tidal streams, making them excellent probes of stream characteristics. Our target sample was selected using photometric data from the Sloan Digital Sky Survey, Data Release 6, which was constrained in color to match the Sagittarius RC stars. Spectroscopic observations of the target stars were conducted at Kitt Peak National Observatory using the WIYN telescope. The resulting spectroscopic sample is magnitude limited and contains both main-sequence disk stars and evolved RC stars. We have developed a method to systematically separate these two stellar classes using kinematic information and a Bayesian approach for surface gravity determination. The resulting RC sample allows us to determine an absolute stellar density of {rho} = 2.7 {+-} 0.5 RC stars kpc{sup -3} at this location in the stream. Future measurements of stellar densities for a variety of populations and at various locations along the streams will lead to a much improved understanding of the original nature of the Sagittarius galaxy and the physical processes controlling its disruption and subsequent stream generation.

  15. THE STAR FORMATION HISTORY AND CHEMICAL EVOLUTION OF STAR-FORMING GALAXIES IN THE NEARBY UNIVERSE

    SciTech Connect (OSTI)

    Torres-Papaqui, J. P.; Coziol, R.; Ortega-Minakata, R. A.; Neri-Larios, D. M. E-mail: rcoziol@astro.ugto.mx E-mail: daniel@astro.ugto.mx

    2012-08-01

    We have determined the metallicity (O/H) and nitrogen abundance (N/O) of a sample of 122,751 star-forming galaxies (SFGs) from the Data Release 7 of the Sloan Digital Sky Survey. For all these galaxies we have also determined their morphology and obtained a comprehensive picture of their star formation history (SFH) using the spectral synthesis code STARLIGHT. The comparison of the chemical abundance with the SFH allows us to describe the chemical evolution of the SFGs in the nearby universe (z {<=} 0.25) in a manner consistent with the formation of their stellar populations and morphologies. A high fraction (45%) of the SFGs in our sample show an excess abundance of nitrogen relative to their metallicity. We also find this excess to be accompanied by a deficiency of oxygen, which suggests that this could be the result of effective starburst winds. However, we find no difference in the mode of star formation of the nitrogen-rich and nitrogen-poor SFGs. Our analysis suggests that they all form their stars through a succession of bursts of star formation extended over a period of few Gyr. What produces the chemical differences between these galaxies seems therefore to be the intensity of the bursts: the galaxies with an excess of nitrogen are those that are presently experiencing more intense bursts or have experienced more intense bursts in their past. We also find evidence relating the chemical evolution process to the formation of the galaxies: the galaxies with an excess of nitrogen are more massive, and have more massive bulges and earlier morphologies than those showing no excess. Contrary to expectation, we find no evidence that the starburst wind efficiency decreases with the mass of the galaxies. As a possible explanation we propose that the loss of metals consistent with starburst winds took place during the formation of the galaxies, when their potential wells were still building up, and consequently were weaker than today, making starburst winds more

  16. The era of star formation in galaxy clusters

    SciTech Connect (OSTI)

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

    2013-12-20

    We analyze the star formation properties of 16 infrared-selected, spectroscopically confirmed galaxy clusters at 1 < z < 1.5 from the Spitzer/IRAC Shallow Cluster Survey (ISCS). We present new spectroscopic confirmation for six of these high-redshift clusters, five of which are at z > 1.35. Using infrared luminosities measured with deep Spitzer/Multiband Imaging Photometer for Spitzer observations at 24 μm, along with robust optical + IRAC photometric redshifts and spectral-energy-distribution-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 ∼ 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. By combining these observations with complementary studies showing a rapid increase in the active galactic nucleus (AGN) fraction, a stochastic star formation history, and a major merging episode at the same epoch in this cluster sample, we suggest that the starburst activity is likely merger-driven and that the subsequent quenching is due to feedback from merger-fueled AGNs. The totality of the evidence suggests we are witnessing the final quenching period that brings an end to the era of star formation in galaxy clusters and initiates the era of passive evolution.

  17. GAMMA RAYS FROM STAR FORMATION IN CLUSTERS OF GALAXIES

    SciTech Connect (OSTI)

    Storm, Emma M.; Jeltema, Tesla E.; Profumo, Stefano

    2012-08-20

    Star formation in galaxies is observed to be associated with gamma-ray emission, presumably from non-thermal processes connected to the acceleration of cosmic-ray nuclei and electrons. The detection of gamma rays from starburst galaxies by the Fermi Large Area Telescope (LAT) has allowed the determination of a functional relationship between star formation rate and gamma-ray luminosity. Since star formation is known to scale with total infrared (8-1000 {mu}m) and radio (1.4 GHz) luminosity, the observed infrared and radio emission from a star-forming galaxy can be used to quantitatively infer the galaxy's gamma-ray luminosity. Similarly, star-forming galaxies within galaxy clusters allow us to derive lower limits on the gamma-ray emission from clusters, which have not yet been conclusively detected in gamma rays. In this study, we apply the functional relationships between gamma-ray luminosity and radio and IR luminosities of galaxies derived by the Fermi Collaboration to a sample of the best candidate galaxy clusters for detection in gamma rays in order to place lower limits on the gamma-ray emission associated with star formation in galaxy clusters. We find that several clusters have predicted gamma-ray emission from star formation that are within an order of magnitude of the upper limits derived in Ackermann et al. based on non-detection by Fermi-LAT. Given the current gamma-ray limits, star formation likely plays a significant role in the gamma-ray emission in some clusters, especially those with cool cores. We predict that both Fermi-LAT over the course of its lifetime and the future Cerenkov Telescope Array will be able to detect gamma-ray emission from star-forming galaxies in clusters.

  18. The decay of debris disks around solar-type stars

    SciTech Connect (OSTI)

    Sierchio, J. M.; Rieke, G. H.; Su, K. Y. L.; Gspr, Andras, E-mail: sierchio@mit.edu [Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)

    2014-04-10

    We present a Spitzer MIPS study of the decay of debris disk excesses at 24 and 70 ?m for 255 stars of types F4-K2. We have used multiple tests, including consistency between chromospheric and X-ray activity and placement on the H-R diagram, to assign accurate stellar ages. Within this spectral type range, at 24 ?m, 13.6% 2.8% of the stars younger than 1 Gyr have excesses at the 3? level or more, whereas none of the older stars do, confirming previous work. At 70 ?m, 22.5% 3.6% of the younger stars have excesses at ?3? significance, whereas only 4.7{sub ?2.2}{sup +3.7}% of the older stars do. To characterize the far-infrared behavior of debris disks more robustly, we doubled the sample by including stars from the DEBRIS and DUNES surveys. For the F4-K4 stars in this combined sample, there is only a weak (statistically not significant) trend in the incidence of far-infrared excess with spectral type (detected fractions of 21.9{sub ?4.3}{sup +4.8}%, late F; 16.5{sub ?3.3}{sup +3.9}%, G; and 16.9{sub ?5.0}{sup +6.3}%, early K). Taking this spectral type range together, there is a significant decline between 3 and 4.5 Gyr in the incidence of excesses, with fractional luminosities just under 10{sup 5}. There is an indication that the timescale for decay of infrared excesses varies roughly inversely with the fractional luminosity. This behavior is consistent with theoretical expectations for passive evolution. However, more excesses are detected around the oldest stars than are expected from passive evolution, suggesting that there is late-phase dynamical activity around these stars.

  19. Groundbreaking Partnership with CoStar Adds Visibility to Energy

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

    Performance | Department of Energy Groundbreaking Partnership with CoStar Adds Visibility to Energy Performance Groundbreaking Partnership with CoStar Adds Visibility to Energy Performance June 13, 2016 - 1:18pm Addthis bto_uptakepost_062216.png by Andrew Burr, U.S. Department of Energy On May 26, Better Buildings announced an historic partnership with The CoStar Group, one of the largest providers of information to real estate decision-makers in the country, to increase the visibility of

  20. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    9.1.4 Market Premiums for ENERGY STAR-Labeled Commercial Buildings in Six Studies (1) CoStar Group/USD CB Richard Ellis/USD Eichholtz/Kok/Quigley Fuerst/McCallister Pivo/Fisher Wiley/Johnson Note(s): Source(s): 1) All studies were conducted in 2008 and 2009 and compared ENERGY STAR-labeled buildings in the United States with similar non-labeled buildings. More information at http://www.imt.org/rating-value. 2) Lower vacancy rates. 3) Not reported. Institute for Market Tranformation,

  1. Comment submitted by Whirlpool Corporation regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Whirlpool Corporation regarding the Energy Star Verification Testing Program

  2. Comment submitted by Consumers Union regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Consumers Union regarding the Energy Star Verification Testing Program

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

    Broader source: Energy.gov [DOE]

    This document is ENERGY STAR Appliance Verification Testing - Pilot Program Summary Report dated February 3, 2012

  4. FAQ's for: ENERGY STAR Verification Testing Pilot Program dated December 2010

    Office of Energy Efficiency and Renewable Energy (EERE)

    This document is the FAQ's for the ENERGY STAR Verification Testing Pilot Program dated December 2010

  5. Comment submitted by Traulsen regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Traulsen regarding the Energy Star Verification Testing Program

  6. Comment submitted by Earthjustice regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Earthjustice regarding the Energy Star Verification Testing Program

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

    Office of Energy Efficiency and Renewable Energy (EERE)

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

  8. American Samoa's Rebate Program Brings ENERGY STAR to Island

    Office of Energy Efficiency and Renewable Energy (EERE)

    Thanks to a grant through the American Recovery and Reinvestment Act, residents of American Samoa are able for the first time to purchase ENERGY STAR air conditioners – and for 30 percent off - through the Island's first appliance rebate program.

  9. ENERGY STAR CERTIFIED HOMES, VERSION 3 (REV. 08) NATIONAL PROGRAM...

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

    process, making it easier to certify a home under v3 or v3.1. PDF icon energystarv3natprogramrqmntsrev08.pdf More Documents & Publications ENERGY STAR Certified Homes, ...

  10. Snohomish County PUD No 1- Build with Energy Star Program

    Broader source: Energy.gov [DOE]

    The Build with Energy Star Program from Snohomish County PUD No 1 is designed to encourage builders to include energy-efficient measures in new homes being built in Snohomish County and on Camano...

  11. Friedrich: ENERGY STAR Referral (SM18M30)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Friedrich room air conditioner model SM18M30 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  12. Friedrich: ENERGY STAR Referral (SS12M30)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Friedrich room air conditioner model SS12M30 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  13. Five ENERGY STAR Room Air Conditioners Fail Testing

    Broader source: Energy.gov [DOE]

    The U.S. Department of Energy's Office of Enforcement announced today that DOE testing has identified five Friedrich room air conditioners that do not meet the ENERGY STAR Program’s energy...

  14. Friedrich: ENERGY STAR Referral (SS14L10-E)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Friedrich room air conditioner SS14L10-E to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  15. Electrolux: ENERGY STAR Referral (GAH105Q2T1)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Electrolux room air conditioner model GAH105Q2T1 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  16. General Electric: ENERGY STAR Referral (PFSF5NFZ****)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of General Electric refrigerator-freezer basic model PFSF5NFZ**** to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  17. NineStar Connect- Residential Energy Efficient Equipment Rebate Program

    Office of Energy Efficiency and Renewable Energy (EERE)

    Nine Star Connect (Greenfield and Maxwell, IN) offers residential customers an incentive to buy energy efficient air-source heat pumps, geothermal heat pumps, heat p[ump water heaters and lighting....

  18. Columbia Water & Light- Home Performance with ENERGY STAR Rebates

    Broader source: Energy.gov [DOE]

    Columbia Water and Light, a municipal utility, offers rebates to its residential customers who make certain energy efficient improvements to the home. Under the Home Performance with Energy Star...

  19. Equator Appliance: ENERGY STAR Referral (EZ 3720 CEE)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Equator clothes washer model EZ 3720 CEE to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  20. Groundbreaking Partnership with CoStar Adds Visibility to Energy...

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

    of the largest providers of information to real estate decision-makers in the country, to increase the visibility of energy performance data in CoStar's online property database. ...

  1. MHK Technologies/OceanStar | Open Energy Information

    Open Energy Info (EERE)

    energy efficient process to smooth out the pulse characteristics common to wave energy in order to be electrical grid friendly The OceanStars high level of scalability is...

  2. Maytag: ENERGY STAR Referral (MVWC6ESWW1)

    Office of Energy Efficiency and Renewable Energy (EERE)

    DOE referred the matter of Maytag clothes washer model MVWC6ESWW1 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  3. Missouri Gas Energy (MGE)- Home Performance with ENERGY STAR

    Broader source: Energy.gov [DOE]

    Missouri Gas Energy (MGE) offers rebates to its residential customers towards the cost of an ENERGY STAR Home Energy Assessment and a portion of the installed efficiency improvements. Home...

  4. South River EMC- Energy Star Homes Rebate Program

    Broader source: Energy.gov [DOE]

    South River EMC offers incentives to home buyers and builders who purchase or construct Energy Star certified single-family site built homes, manufactured homes, and multi-family dwellings. Energy...

  5. What do you get when two neutron stars merge?

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

    What do you get when two neutron stars merge? Led by Chris Fryer of the University of ... Led by Chris Fryer of the University of Arizona and the Los Alamos National Laboratory, a ...

  6. The chemical abundances of the Ap star HD94660

    SciTech Connect (OSTI)

    Giarrusso, M. [Universit di Catania, Dipartimento di Fisica e Astronomia, Sezione Astrofisica, Via S. Sofia 78, 95123 Catania (Italy); INAF - Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123 Catania (Italy); INFN - Laboratori Nazionali del Sud (Italy)

    2014-05-09

    In this work I present the determination of chemical abundances of the Ap star HD94660, a possible rapid oscillating star. As all the magnetic chemically peculiar objects, it presents CNO underabundance and overabundance of iron peak elements of ?100 times and of rare earths up to 4 dex with respect to the Sun. The determination was based on the conversion of the observed equivalent widths into abundances simultaneously to the determination of effective temperature and gravity. Since the Balmer lines of early type stars are very sensitive to the surface gravity while the flux distribution is sensitive to the effective temperature, I have adopted an iterative procedure to match the H{sub ?} line profile and the observed UV-Vis-NIR magnitudes of HD94660 looking for a consistency between the metallicity of the atmosphere model and the derived abundances. From my spectroscopic analysis, this star belongs to the no-rapid oscillating class.

  7. Avanti: ENERGY STAR Referral (BCA4560W-2)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Avanti refrigerator model BCA4560W-2 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  8. Kansas City Power & Light- Home Performance with ENERGY STAR

    Broader source: Energy.gov [DOE]

    Kansas City Power & Light (KCP&L) offers rebates to residential customers of KCP&L's Greater Missouri Operations towards the cost of an ENERGY STAR Home Energy Assessment and a portion...

  9. Kansas City Power & Light- Home Performance Rebate with ENERGY STAR

    Broader source: Energy.gov [DOE]

    Kansas City Power and Light (KCP&L) offers rebates to residential customers towards the cost of an ENERGY STAR Home Energy Assessment and a portion of the installed efficiency improvements....

  10. Magnetohydrodynamical turbulence in Star and Planet Formation | Princeton

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

    Plasma Physics Lab March 7, 2007, 4:15pm to 5:15pm Colloquia Magnetohydrodynamical turbulence in Star and Planet Formation Dr. Mordecai-Mark Mac Low, Department of Astrophysics American Museum of Natural History

  11. VEE-0040- In the Matter of Western Star Propane, Inc.

    Broader source: Energy.gov [DOE]

    On February 18, 1997, Western Star Propane, Inc. (Western) filed an Application for Exception with the Office of Hearings and Appeals (OHA) of the Department of Energy (DOE). In its application,...

  12. PrimeStar Solar Inc | Open Energy Information

    Open Energy Info (EERE)

    PrimeStar Solar Inc Place: Longmont, Colorado Zip: 80504 Product: Intends to produce CdTe thin film PV modules using technology licensed by the NREL. Coordinates: 40.16394,...

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

    Office of Legacy Management (LM)

    ... F25982 4 4.1 102504 Technical Report for S M Stoller Star Center-WWNA Monthly; Largo, FL 110406202 Accutest Job Number: F26616 Sampling Date: 090904 Report to: S M Stoller ...

  14. Electrolux: ENERGY STAR Referral (FRA256ST2)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Electrolux room air conditioner model FRA256ST2 to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  15. Reading Municipal Light Department- Residential Energy Star Appliance Rebate Program

    Broader source: Energy.gov [DOE]

    Reading Municipal Light Department (RMLD) offers rebates to residential customers who install Energy Star appliances in eligible homes. The offer is limited to one rebate per appliance, or a...

  16. Haier: ENERGY STAR Referral (ESNCM053E) | Department of Energy

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

    DOE referred the matter of Haier freezer model ESNCM053E to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE ...

  17. North Star Refrigerator: Proposed Penalty (2013-CE-5355)

    Broader source: Energy.gov [DOE]

    DOE alleged in a Notice of Proposed Civil Penalty that North Star Refrigerator Co., Inc. failed to certify a variety of walk-in cooler or freezer components as compliant with the applicable energy conservation standards.

  18. Support for ENERGY STAR Enforcement | Department of Energy

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

    a means for consumers to buy products more energy-efficient than required by law, ENERGY STAR has huge potential to save money for consumers by offering buyers more options...

  19. ENERGY STAR Webinar: Portfolio Manager 201 | Department of Energy

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

    201 ENERGY STAR Webinar: Portfolio Manager 201 December 16, 2015 1:00PM to 2:00PM EST Online This webinar continues on the U.S. Environmental Protection Agency's (EPA's) ENERGY...

  20. NNSA Congratulates Pantex for Earning STAR in DOE's Voluntary...

    National Nuclear Security Administration (NNSA)

    B&W Pantex is also the proud recipient of the DOE's Voluntary Protection Program STAR status for safety excellence. The company was also named one of America's safest...

  1. Support for ENERGY STAR Enforcement | Department of Energy

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

    into a Consent Decree with Haier America Trading, L.L.C., after DOE testing in the Energy Star Verification Testing Pilot Program showed Haier's freezer model HUF138EA, not...

  2. Home Performance with ENERGY STAR Program | Department of Energy

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

    available until June 30, 2015 or until the funds are exhausted. NJ Home Performance with ENERGY STAR program includes both rebate and loan as incentives. This program is listed...

  3. Progress Energy Carolinas - Rate Discount for Energy Star Homes...

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

    qualify, the home must meet the standards of the U.S. Environmental Protection Agency's Energy Star-labeled home program and be verified by a registered third party. The...

  4. Home Performance with ENERGY STAR (WPS Customers Only) | Department...

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

    Energy-saving products and installation: Free Summary Through the Home Performance with Energy Star program, Focus on Energy offers in-home energy audits and cash incentives for...

  5. NJ Clean Energy- ENERGY STAR Appliance Rebate program

    Broader source: Energy.gov [DOE]

    When mail-in rebates are active, as a general rule, all appliances must be ENERGY STAR rated; however, additional requirements may apply to different types of appliances. Rebate requests must...

  6. Upper Bound on the First Star Formation History (Journal Article...

    Office of Scientific and Technical Information (OSTI)

    Upper Bound on the First Star Formation History Citation Details ... Publication Date: 2014-11-20 OSTI Identifier: 1165908 Report Number(s): SLAC-PUB-16151 Journal ID: ISSN ...

  7. Upper Bound on the First Star Formation History (Journal Article...

    Office of Scientific and Technical Information (OSTI)

    Upper Bound on the First Star Formation History Citation Details ... Publication Date: 2014-01-09 OSTI Identifier: 1114151 Report Number(s): SLAC-PUB-15885 Journal ID: ISSN ...

  8. ENERGY STAR for Homes - Building America Top Innovation | Department...

    Energy Savers [EERE]

    Cumulatively, more than 1.3 million ENERGY STAR certified homes have delivered 23 billion in energy cost savings and avoided 210 million tons of green-house emissions. Strong ...

  9. DOE Recognizes Top ENERGY STAR Partners | Department of Energy

    Office of Environmental Management (EM)

    ... ENERGY STAR is a joint DOE-EPA program, formed in 1992 as a voluntary, market-based partnership that seeks to reduce air pollution through increased energy efficiency. DOE and ...

  10. Draft Environmental Assessment for NorthStar | National Nuclear Security

    National Nuclear Security Administration (NNSA)

    Administration | (NNSA) Draft Environmental Assessment for NorthStar ENVIRONMENTAL ASSESSMENT FOR NORTHSTAR MEDICAL TECHNOLOGIES LLC COMMERCIAL DOMESTIC PRODUCTION OF THE MEDICAL ISOTOPE MOLYBDENUM-99 Proposed Action: The Department of Energy (DOE) National Nuclear Security Administration (NNSA) proposes to provide funding to NorthStar to accelerate the establishment of the commercial production of the medical isotope molybdenum-99 using accelerator technology. Report Designation: Draft

  11. The domains of instability for the pulsating PG1159 stars.

    SciTech Connect (OSTI)

    Quirion, P.-O.; Fontaine, Gilles.; Brassard, Pierre; Herwig, F. H.

    2004-01-01

    The fact that we find pulsating and nonpulsating stars mixed together in the PG 1159 region of the log g - T{sub eff} diagram has been a long standing puzzle. The poor understanding of the driving mechanism in those stars has been the reason why it has taken so long to address properly this problem. Following the work of Saio (1996) and Gautschy (1997) based on the OPAL opacities, Quirion, Fontaine, & Brassard (2004) recently showed that we are now able to understand and reproduce the ranges of observed periods in the pulsating PG 1159 stars in terms of the original {kappa}-mechanism associated with the partial ionization of the K-shell electrons of C and O which, along with He, make up the composition of the envelope of those stars. Contrary to others, those three studies agree in that no composition gradients are needed between the atmospheric layers and the driving region. Furthermore, the cohabitation of pulsating and nonpulsating PG 1159 stars is naturally explained in terms of a dispersion in atmospheric parameters and in terms of a variation in surface composition from star to star. In particular, the most He-rich stars tend to be stable. We go beyond the findings discussed by Quirion et al. (2004) in this paper, and present the results of additional calculations aimed at describing better the role of the chemical composition (in particular the role of metallicity) as well as that of the stellar mass on the boundaries of the instability domain in the log g - T{sub eff} plane.

  12. Calendar Year 2008 Program Benefits for ENERGY STAR Labeled Products

    SciTech Connect (OSTI)

    Homan, GregoryK; Sanchez, Marla; Brown, RichardE; Lai, Judy

    2010-08-24

    This paper presents current and projected savings for ENERGY STAR labeled products, and details the status of the model as implemented in the September 2009 spreadsheets. ENERGY STAR is a voluntary energy efficiency labeling program operated jointly by the Environmental Protection Agency (US EPA) and the U.S. Department of Energy (US DOE), designed to identify and promote energy-efficient products, buildings and practices. Since the program inception in 1992, ENERGY STAR has become a leading international brand for energy efficient products, and currently labels more than thirty products, spanning office equipment, heating, cooling and ventilation equipment, commercial and residential lighting, home electronics, and major appliances. ENERGY STAR's central role in the development of regional, national and international energy programs necessitates an open process whereby its program achievements to date as well as projected future savings are shared with stakeholders. This report presents savings estimates for ENERGY STAR labeled products. We present estimates of energy, dollar, and carbon savings achieved by the program in the year 2008, annual forecasts for 2009 and 2010, and cumulative savings estimates for the period 1993 through 2008 and cumulative forecasts for the period 2009 through 2015. Through 2008 the program saved 8.8 Quads of primary energy and avoided the equivalent of 158 metric tones carbon (MtC). The forecast for the period 2009-2015 is 18.1 Quads or primary energy saved and 316 MtC emissions avoided. The sensitivity analysis bounds the best estimate of carbon avoided between 104 MtC and 213 MtC (1993 to 2008) and between 206 MtC and 444 MtC (2009 to 2015). In this report we address the following questions for ENERGY STAR labeled products: (1) How are ENERGY STAR impacts quantified; (2) What are the ENERGY STAR achievements; and (3) What are the limitations to our method?

  13. Hans Bethe, Powering the Stars, and Nuclear Physics

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

    Hans Bethe, Energy Production in Stars, and Nuclear Physics Awards and Tributes * Resources with Additional Information Hans Bethe Courtesy of Cornell University "Hans Bethe was one of the great physicists not only of the twentieth century, but of all time. During his long life, he uncovered the secrets powering the stars, published the standard work on nuclear physics, built atomic weapons, and called for a halt to their proliferation. Bethe's dual legacy is one of genius and

  14. ENERGY STAR Webinar: Portfolio Manager 301 | Department of Energy

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

    Webinar: Portfolio Manager 301 ENERGY STAR Webinar: Portfolio Manager 301 August 25, 2016 1:00PM to 2:00PM EDT Hosted by the U.S. Environmental Protection Agency (EPA) ENERGY STAR, this webinar will show attendees how to upload templates to update property data, setting goals and targets to plan energy improvements for properties, creating custom reports, and using the Sustainable Buildings Checklist. Register for this webinar

  15. ENERGY STAR Webinar: Portfolio Manager 201 | Department of Energy

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

    201 ENERGY STAR Webinar: Portfolio Manager 201 August 24, 2016 1:00PM to 2:00PM EDT This webinar continues on the U.S. Environmental Protection Agency's (EPA's) new ENERGY STAR Portfolio Manager tool. Attendees will learn the more advanced functionalities, such as managing and tracking changes to your property uses over time, using spreadsheet templates to update property data, setting goals and targets to plan energy improvements for properties, generating and using custom reports, and using

  16. DOE Headquarters Receives Energy Star Recognition from EPA | Department of

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

    Energy Headquarters Receives Energy Star Recognition from EPA DOE Headquarters Receives Energy Star Recognition from EPA July 9, 2008 - 2:15pm Addthis WASHINGTON - U.S. Secretary of Energy Samuel W. Bodman today accepted a plaque from the U.S. Environmental Protection Agency (EPA) certifying the Department of Energy's (DOE) James Forrestal Headquarters Building as an ENERGY STAR® building. The Forrestal building uses 40 percent less energy than the average office building, saving taxpayers

  17. DOE Honors Safety Star: Department's Program Honors Portsmouth Site

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

    Contractor Employee for Promoting Safety Excellence | Department of Energy Honors Safety Star: Department's Program Honors Portsmouth Site Contractor Employee for Promoting Safety Excellence DOE Honors Safety Star: Department's Program Honors Portsmouth Site Contractor Employee for Promoting Safety Excellence September 11, 2012 - 12:00pm Addthis Wastren-EnergX Mission Support (WEMS) Senior Safety Engineer Marsha Bevins, left, stands with DOE Director of Worker Safety and Health Brad Davy

  18. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    2010 ENERGY STAR Qualified New Single-Family Homes, by Selected State Market Hawaii Nevada Iowa Arizona Ohio Colorado Texas Maryland Oklahoma New Jersey Delaware Utah Kentucky Rhode Island New Mexico Vermont District of Columbia Wisconsin New York Michigan United States Note(s): Source(s): The States listed are the top 20 by ENERGY STAR market penetration. Personal communication, Zachary Shadid, U.S. EPA, February 9, 2012; DOC/Census Bureau, Building Permits Survey, 2010, "New Privately

  19. SHEDDING NEW LIGHT ON EXPLODING STARS: TERASCALE SIMULATIONS OF

    Office of Scientific and Technical Information (OSTI)

    NEUTRINO-DRIVEN SUPERNOVAE AND THEIR NUCLEOSYNTHESIS (Technical Report) | SciTech Connect SHEDDING NEW LIGHT ON EXPLODING STARS: TERASCALE SIMULATIONS OF NEUTRINO-DRIVEN SUPERNOVAE AND THEIR NUCLEOSYNTHESIS Citation Details In-Document Search Title: SHEDDING NEW LIGHT ON EXPLODING STARS: TERASCALE SIMULATIONS OF NEUTRINO-DRIVEN SUPERNOVAE AND THEIR NUCLEOSYNTHESIS This project was focused on simulations of core-collapse supernovae on parallel platforms. The intent was to address a number of

  20. DOE - Office of Legacy Management -- Star Cutter Corp - MI 15

    Office of Legacy Management (LM)

    Star Cutter Corp - MI 15 FUSRAP Considered Sites Site: STAR CUTTER CORP. (MI.15) Eliminated from consideration under FUSRAP Designated Name: Not Designated Alternate Name: None Location: Farmington , Michigan MI.15-1 Evaluation Year: 1991 MI.15-2 Site Operations: Performed a one time uranium slug drilling operation test in 1956. MI.15-3 MI.15-1 Site Disposition: Eliminated - Potential for contamination considered remote based on limited scope and quantity of materials handled MI.15-2 Radioactive

  1. Bradbury Science Museum participates in Blue Star Museums program

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

    Museum participates in Blue Star Museums program Bradbury Science Museum participates in Blue Star Museums program Museum to host active duty military personnel and their families from Memorial Day, May 25, through Labor Day, Sept. 7. May 21, 2015 Bradbury Science Museum, los Alamos, New Mexico Bradbury Science Museum, Los Alamos, New Mexico Contact Los Alamos National Laboratory Steve Sandoval Communications Office (505) 665 9206 Email "The museum already has a free-admission policy, but

  2. Home Performance with ENERGY STAR Webinar (text version)

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

    5, 2010 - Home Performance with ENERGY STAR Webinar (text version) Erin Jackson: Okay, hi, everybody. This is Erin Jackson with the Department of Energy, and we welcome you to today's webinar about the EPA's Home Performance with ENERGY STAR Program. I am very excited to introduce our speakers today. The first person we have online is Chandler von Schrader - am I saying that correctly? Chandler von Schrader: Yes. Erin Jackson: Good, good. Hi, welcome, Chandler. He has been in the energy

  3. ON STAR FORMATION RATES AND STAR FORMATION HISTORIES OF GALAXIES OUT TO z {approx} 3

    SciTech Connect (OSTI)

    Wuyts, Stijn; Foerster Schreiber, Natascha M.; Lutz, Dieter; Nordon, Raanan; Berta, Stefano; Genzel, Reinhard; Magnelli, Benjamin; Poglitsch, Albrecht; Altieri, Bruno; Andreani, Paola; Aussel, Herve; Daddi, Emanuele; Elbaz, David; Cimatti, Andrea; Koekemoer, Anton M.; Maiolino, Roberto; McGrath, Elizabeth J.

    2011-09-01

    We compare multi-wavelength star formation rate (SFR) indicators out to z {approx} 3 in the GOODS-South field. Our analysis uniquely combines U to 8 {mu}m photometry from FIREWORKS, MIPS 24 {mu}m and PACS 70, 100, and 160 {mu}m photometry from the PEP, and H{alpha} spectroscopy from the SINS survey. We describe a set of conversions that lead to a continuity across SFR indicators. A luminosity-independent conversion from 24 {mu}m to total infrared luminosity yields estimates of L{sub IR} that are in the median consistent with the L{sub IR} derived from PACS photometry, albeit with significant scatter. Dust correction methods perform well at low-to-intermediate levels of star formation. They fail to recover the total amount of star formation in systems with large SFR{sub IR}/SFR{sub UV} ratios, typically occuring at the highest SFRs (SFR{sub UV+IR} {approx}> 100 M{sub sun} yr{sup -1}) and redshifts (z {approx}> 2.5) probed. Finally, we confirm that H{alpha}-based SFRs at 1.5 < z < 2.6 are consistent with SFR{sub SED} and SFR{sub UV+IR} provided extra attenuation toward H II regions is taken into account (A{sub V,neb} = A{sub V,continuum}/0.44). With the cross-calibrated SFR indicators in hand, we perform a consistency check on the star formation histories inferred from spectral energy distribution (SED) modeling. We compare the observed SFR-M relations and mass functions at a range of redshifts to equivalents that are computed by evolving lower redshift galaxies backward in time. We find evidence for underestimated stellar ages when no stringent constraints on formation epoch are applied in SED modeling. We demonstrate how resolved SED modeling, or alternatively deep UV data, may help to overcome this bias. The age bias is most severe for galaxies with young stellar populations and reduces toward older systems. Finally, our analysis suggests that SFHs typically vary on timescales that are long (at least several 100 Myr) compared to the galaxies' dynamical time.

  4. Magnetic Fields in Population III Star Formation

    SciTech Connect (OSTI)

    Turk, Matthew J.; Oishi, Jeffrey S.; Abel, Tom; Bryan, Greg

    2012-02-22

    We study the buildup of magnetic fields during the formation of Population III star-forming regions, by conducting cosmological simulations from realistic initial conditions and varying the Jeans resolution. To investigate this in detail, we start simulations from identical initial conditions, mandating 16, 32 and 64 zones per Jeans length, and studied the variation in their magnetic field amplification. We find that, while compression results in some amplification, turbulent velocity fluctuations driven by the collapse can further amplify an initially weak seed field via dynamo action, provided there is sufficient numerical resolution to capture vortical motions (we find this requirement to be 64 zones per Jeans length, slightly larger than, but consistent with previous work run with more idealized collapse scenarios). We explore saturation of amplification of the magnetic field, which could potentially become dynamically important in subsequent, fully-resolved calculations. We have also identified a relatively surprising phenomena that is purely hydrodynamic: the higher-resolved simulations possess substantially different characteristics, including higher infall-velocity, increased temperatures inside 1000 AU, and decreased molecular hydrogen content in the innermost region. Furthermore, we find that disk formation is suppressed in higher-resolution calculations, at least at the times that we can follow the calculation. We discuss the effect this may have on the buildup of disks over the accretion history of the first clump to form as well as the potential for gravitational instabilities to develop and induce fragmentation.

  5. Angular momentum transport via internal gravity waves in evolving stars

    SciTech Connect (OSTI)

    Fuller, Jim; Lecoanet, Daniel; Cantiello, Matteo; Brown, Ben

    2014-11-20

    Recent asteroseismic advances have allowed for direct measurements of the internal rotation rates of many subgiant and red giant stars. Unlike the nearly rigidly rotating Sun, these evolved stars contain radiative cores that spin faster than their overlying convective envelopes, but slower than they would in the absence of internal angular momentum transport. We investigate the role of internal gravity waves in angular momentum transport in evolving low-mass stars. In agreement with previous results, we find that convectively excited gravity waves can prevent the development of strong differential rotation in the radiative cores of Sun-like stars. As stars evolve into subgiants, however, low-frequency gravity waves become strongly attenuated and cannot propagate below the hydrogen-burning shell, allowing the spin of the core to decouple from the convective envelope. This decoupling occurs at the base of the subgiant branch when stars have surface temperatures of T ? 5500 K. However, gravity waves can still spin down the upper radiative region, implying that the observed differential rotation is likely confined to the deep core near the hydrogen-burning shell. The torque on the upper radiative region may also prevent the core from accreting high angular momentum material and slow the rate of core spin-up. The observed spin-down of cores on the red giant branch cannot be totally attributed to gravity waves, but the waves may enhance shear within the radiative region and thus increase the efficacy of viscous/magnetic torques.

  6. Extreme neutron stars from Extended Theories of Gravity

    SciTech Connect (OSTI)

    Astashenok, Artyom V.; Capozziello, Salvatore; Odintsov, Sergei D. E-mail: capozziello@na.infn.it

    2015-01-01

    We discuss neutron stars with strong magnetic mean fields in the framework of Extended Theories of Gravity. In particular, we take into account models derived from f(R) and f(G) extensions of General Relativity where functions of the Ricci curvature invariant R and the Gauss-Bonnet invariant G are respectively considered. Dense matter in magnetic mean field, generated by magnetic properties of particles, is described by assuming a model with three meson fields and baryons octet. As result, the considerable increasing of maximal mass of neutron stars can be achieved by cubic corrections in f(R) gravity. In principle, massive stars with M>4M{sub ?} can be obtained. On the other hand, stable stars with high strangeness fraction (with central densities ?{sub c}?1.52.0 GeV/fm{sup 3}) are possible considering quadratic corrections of f(G) gravity. The magnetic field strength in the star center is of order 68נ10{sup 18} G. In general, we can say that other branches of massive neutron stars are possible considering the extra pressure contributions coming from gravity extensions. Such a feature can constitute both a probe for alternative theories and a way out to address anomalous self-gravitating compact systems.

  7. ChemLabBox for SnifferStars

    Energy Science and Technology Software Center (OSTI)

    2002-01-24

    The software entitled "ChemLabBox for SnifferStars" is used to collect, display, and save data from the Sandia National Laboratories chemical analysis system dubbed SnifferStar. Sensor data is streamed from a SnifferStar unit into a computer thru RS-232 in a manner that is not amendable to plotting. Also, there is no direct way to start and stop the unit as is. This software rearranges the data into something that can be easily plotted in real-time thenmore » saves the data into a text fild. In addition, this software provides the users a means to start and stop the hardware. This software was written specifically for SnifferStar. SnifferStar data is delivered at a very fast rate but for a short period of time. This software is written around that premise. It is written for Pentium or higher machines running Windows 95/98/ME/NT/2000/XP. Lockheed Martin is interested in using it for testing SnifferStar units before deployment. To date they have not indicated their intent to deliver the code either in part or whole as part of their product.« less

  8. Relativistic structure, stability, and gravitational collapse of charged neutron stars

    SciTech Connect (OSTI)

    Ghezzi, Cristian R.

    2005-11-15

    Charged stars have the potential of becoming charged black holes or even naked singularities. We present a set of numerical solutions of the Tolman-Oppenheimer-Volkov equations that represents spherical charged compact stars in hydrostatic equilibrium. The stellar models obtained are evolved forward in time integrating the Einstein-Maxwell field equations. We assume an equation of state of a neutron gas at zero temperature. The charge distribution is taken as being proportional to the rest mass density distribution. The set of solutions present an unstable branch, even with charge-to-mass ratios arbitrarily close to the extremum case. We perform a direct check of the stability of the solutions under strong perturbations and for different values of the charge-to-mass ratio. The stars that are in the stable branch oscillate and do not collapse, while models in the unstable branch collapse directly to form black holes. Stars with a charge greater than or equal to the extreme value explode. When a charged star is suddenly discharged, it does not necessarily collapse to form a black hole. A nonlinear effect that gives rise to the formation of a shell of matter (in supermassive stars), is negligible in the present simulations. The results are in agreement with the third law of black hole thermodynamics and with the cosmic censorship conjecture.

  9. PULSATION PERIOD VARIATIONS IN THE RRc LYRAE STAR KIC 5520878

    SciTech Connect (OSTI)

    Hippke, Michael; Learned, John G.; Zee, A.; Edmondson, William H.; Lindner, John F.; Kia, Behnam; Ditto, William L.; Stevens, Ian R. E-mail: jgl@phys.hawaii.edu E-mail: w.h.edmondson@bham.ac.uk E-mail: wditto@hawaii.edu E-mail: irs@star.sr.bham.ac.uk

    2015-01-01

    Learned et al. proposed that a sufficiently advanced extra-terrestrial civilization may tickle Cepheid and RR Lyrae variable stars with a neutrino beam at the right time, thus causing them to trigger early and jogging the otherwise very regular phase of their expansion and contraction. This would turn these stars into beacons to transmit information throughout the galaxy and beyond. The idea is to search for signs of phase modulation (in the regime of short pulse duration) and patterns, which could be indicative of intentional, omnidirectional signaling. We have performed such a search among variable stars using photometric data from the Kepler space telescope. In the RRc Lyrae star KIC 5520878, we have found two such regimes of long and short pulse durations. The sequence of period lengths, expressed as time series data, is strongly autocorrelated, with correlation coefficients of prime numbers being significantly higher (p = 99.8%). Our analysis of this candidate star shows that the prime number oddity originates from two simultaneous pulsation periods and is likely of natural origin. Simple physical models elucidate the frequency content and asymmetries of the KIC 5520878 light curve. Despite this SETI null result, we encourage testing of other archival and future time-series photometry for signs of modulated stars. This can be done as a by-product to the standard analysis, and can even be partly automated.

  10. CENSUS OF BLUE STARS IN SDSS DR8

    SciTech Connect (OSTI)

    Scibelli, Samantha; Newberg, Heidi Jo; Carlin, Jeffrey L.; Yanny, Brian

    2015-01-01

    We present a census of the 12,060 spectra of blue objects ((g – r){sub 0} < –0.25) in the Sloan Digital Sky Survey (SDSS) Data Release 8 (DR8). As part of the data release, all of the spectra were cross-correlated with 48 template spectra of stars, galaxies, and QSOs to determine the best match. We compared the blue spectra by eye to the templates assigned in SDSS DR8. 10,856 of the objects matched their assigned template, 170 could not be classified due to low signal-to-noise ratio, and 1034 were given new classifications. We identify 7458 DA white dwarfs, 1145 DB white dwarfs, 273 rarer white dwarfs (including carbon, DZ, DQ, and magnetic), 294 subdwarf O stars, 648 subdwarf B stars, 679 blue horizontal branch stars, 1026 blue stragglers, 13 cataclysmic variables, 129 white dwarf-M dwarf binaries, 36 objects with spectra similar to DO white dwarfs, 179, quasi-stellar objects (QSOs), and 10 galaxies. We provide two tables of these objects, sample spectra that match the templates, figures showing all of the spectra that were grouped by eye, and diagnostic plots that show the positions, colors, apparent magnitudes, proper motions, etc., for each classification. Future surveys will be able to use templates similar to stars in each of the classes we identify to automatically classify blue stars, including rare types.

  11. Delayed star formation in isolated dwarf galaxies: Hubble space telescope star formation history of the Aquarius dwarf irregular

    SciTech Connect (OSTI)

    Cole, Andrew A.; Weisz, Daniel R.; Dolphin, Andrew E.; Skillman, Evan D.; McConnachie, Alan W.; Brooks, Alyson M.; Leaman, Ryan E-mail: drw@ucsc.edu E-mail: skillman@astro.umn.edu E-mail: abrooks@physics.rutgers.edu

    2014-11-01

    We have obtained deep images of the highly isolated (d = 1 Mpc) Aquarius dwarf irregular galaxy (DDO 210) with the Hubble Space Telescope Advanced Camera for Surveys. The resulting color-magnitude diagram (CMD) reaches more than a magnitude below the oldest main-sequence turnoff, allowing us to derive the star formation history (SFH) over the entire lifetime of the galaxy with a timing precision of ?10% of the lookback time. Using a maximum likelihood fit to the CMD we find that only ?10% of all star formation in Aquarius took place more than 10 Gyr ago (lookback time equivalent to redshift z ? 2). The star formation rate increased dramatically ?6-8 Gyr ago (z ? 0.7-1.1) and then declined until the present time. The only known galaxy with a more extreme confirmed delay in star formation is Leo A, a galaxy of similar M {sub H} {sub I}/M {sub *}, dynamical mass, mean metallicity, and degree of isolation. The delayed stellar mass growth in these galaxies does not track the mean dark matter accretion rate from CDM simulations. The similarities between Leo A and Aquarius suggest that if gas is not removed from dwarf galaxies by interactions or feedback, it can linger for several gigayears without cooling in sufficient quantity to form stars efficiently. We discuss possible causes for the delay in star formation including suppression by reionization and late-time mergers. We find reasonable agreement between our measured SFHs and select cosmological simulations of isolated dwarfs. Because star formation and merger processes are both stochastic in nature, delayed star formation in various degrees is predicted to be a characteristic (but not a universal) feature of isolated small galaxies.

  12. The RR Lyrae stars: New perspectives

    SciTech Connect (OSTI)

    McNamara, D. H.; Barnes, J. E-mail: jonathan.barnes@slcc.edu

    2014-02-01

    We demonstrate that the Oosterhoff II (Oo II) RR Lyrae ab variables are hotter by ?270 K, at the same period, than Oo I variables. Or, at the same ((B) (V)){sub 0} value the Oo II variables have larger radii than Oo I variables. This accounts for the reason Oo II variables are brighter (0.12-0.20 mag) than Oo I variables. The dependence of the light amplitude of RR Lyrae variables on temperature is independent of Oo type. This makes it possible to derive an accurate set of equations to relate intrinsic (B V){sub 0} color indices to light amplitudes, which in turn can be used to determine the interstellar reddening (E (B V)). With just a few variables (?5), it is possible to determine the E (B V) to an accuracy of <0.01 mag in the absence of systematic photometric errors. We discuss the errors introduced in color excess determinations by including the Blazhko stars in a solution. A comparison of color excess values of 23 globular clusters and two regions of the Large Magellanic Cloud (LMC), determined with the aid of our newly developed equations, are found to compare favorably (?0.01 mag) with color excess values found in the literature. Four new Oo III variables, some found in metal-poor clusters, are discussed. An analysis of the galactic-field variables indicates the majority are Oo I and Oo II variables, but a few short-period (log P < 0.36) metal-strong variables, so far not found in galactic globular clusters are evidently ?0.30 mag fainter than Oo I variables. Oo III variables may also be present in the field. We conclude that the RR Lyrae ab variables are primarily restricted to four sequences or groups. If we assume that the Oo I variables' mean absolute magnitude is Mv = 0.61, the mean absolute magnitudes of the other three sequences are: short-period variables Mv ? 0.89 mag, Oo II Mv ? 0.43 mag, and Oo III Mv ? 0.29 mag. The Oo I fundamental RR Lyrae ab red edge (FRE) and fundamental blue edge (FBE) occur at approximately the following

  13. THE CATALINA SURVEYS PERIODIC VARIABLE STAR CATALOG

    SciTech Connect (OSTI)

    Drake, A. J.; Graham, M. J.; Djorgovski, S. G.; Mahabal, A. A.; Donalek, C.; Williams, R.; Catelan, M.; Torrealba, G.; García-Álvarez, D.; Prieto, J. L.; Beshore, E.; Larson, S.; Christen sen, E.; Boattini, A.; Gibbs, A.; Hill, R.; Kowalski, R.; Johnson, J.; Belokurov, V.; Koposov, S. E.; and others

    2014-07-01

    We present ∼47,000 periodic variables found during the analysis of 5.4 million variable star candidates within a 20,000 deg{sup 2} region covered by the Catalina Surveys Data Release-1 (CSDR1). Combining these variables with type ab RR Lyrae from our previous work, we produce an online catalog containing periods, amplitudes, and classifications for ∼61,000 periodic variables. By cross-matching these variables with those from prior surveys, we find that >90% of the ∼8000 known periodic variables in the survey region are recovered. For these sources, we find excellent agreement between our catalog and prior values of luminosity, period, and amplitude as well as classification. We investigate the rate of confusion between objects classified as contact binaries and type c RR Lyrae (RRc's) based on periods, colors, amplitudes, metallicities, radial velocities, and surface gravities. We find that no more than a few percent of the variables in these classes are misidentified. By deriving distances for this clean sample of ∼5500 RRc's, we trace the path of the Sagittarius tidal streams within the Galactic halo. Selecting 146 outer-halo RRc's with SDSS radial velocities, we confirm the presence of a coherent halo structure that is inconsistent with current N-body simulations of the Sagittarius tidal stream. We also find numerous long-period variables that are very likely associated within the Sagittarius tidal stream system. Based on the examination of 31,000 contact binary light curves we find evidence for two subgroups exhibiting irregular light curves. One subgroup presents significant variations in mean brightness that are likely due to chromospheric activity. The other subgroup shows stable modulations over more than a thousand days and thereby provides evidence that the O'Connell effect is not due to stellar spots.

  14. X-RAY EMISSION FROM MAGNETIC MASSIVE STARS

    SciTech Connect (OSTI)

    Naz, Yal; Petit, Vronique; Rinbrand, Melanie; Owocki, Stan; Cohen, David; Ud-Doula, Asif; Wade, Gregg A.

    2014-11-01

    Magnetically confined winds of early-type stars are expected to be sources of bright and hard X-rays. To clarify the systematics of the observed X-ray properties, we have analyzed a large series of Chandra and XMM-Newton observations, corresponding to all available exposures of known massive magnetic stars (over 100 exposures covering ?60% of stars compiled in the catalog of Petit et al.). We show that the X-ray luminosity is strongly correlated with the stellar wind mass-loss rate, with a power-law form that is slightly steeper than linear for the majority of the less luminous, lower- M-dot B stars and flattens for the more luminous, higher- M-dot O stars. As the winds are radiatively driven, these scalings can be equivalently written as relations with the bolometric luminosity. The observed X-ray luminosities, and their trend with mass-loss rates, are well reproduced by new MHD models, although a few overluminous stars (mostly rapidly rotating objects) exist. No relation is found between other X-ray properties (plasma temperature, absorption) and stellar or magnetic parameters, contrary to expectations (e.g., higher temperature for stronger mass-loss rate). This suggests that the main driver for the plasma properties is different from the main determinant of the X-ray luminosity. Finally, variations of the X-ray hardnesses and luminosities, in phase with the stellar rotation period, are detected for some objects and they suggest that some temperature stratification exists in massive stars' magnetospheres.

  15. Modeling jet and outflow feedback during star cluster formation

    SciTech Connect (OSTI)

    Federrath, Christoph; Schrn, Martin; Banerjee, Robi; Klessen, Ralf S.

    2014-08-01

    Powerful jets and outflows are launched from the protostellar disks around newborn stars. These outflows carry enough mass and momentum to transform the structure of their parent molecular cloud and to potentially control star formation itself. Despite their importance, we have not been able to fully quantify the impact of jets and outflows during the formation of a star cluster. The main problem lies in limited computing power. We would have to resolve the magnetic jet-launching mechanism close to the protostar and at the same time follow the evolution of a parsec-size cloud for a million years. Current computer power and codes fall orders of magnitude short of achieving this. In order to overcome this problem, we implement a subgrid-scale (SGS) model for launching jets and outflows, which demonstrably converges and reproduces the mass, linear and angular momentum transfer, and the speed of real jets, with ?1000 times lower resolution than would be required without the SGS model. We apply the new SGS model to turbulent, magnetized star cluster formation and show that jets and outflows (1) eject about one-fourth of their parent molecular clump in high-speed jets, quickly reaching distances of more than a parsec, (2) reduce the star formation rate by about a factor of two, and (3) lead to the formation of ?1.5 times as many stars compared to the no-outflow case. Most importantly, we find that jets and outflows reduce the average star mass by a factor of ? three and may thus be essential for understanding the characteristic mass of the stellar initial mass function.

  16. SS 383: A NEW S-TYPE YELLOW SYMBIOTIC STAR?

    SciTech Connect (OSTI)

    Baella, N. O.; Pereira, C. B.; Miranda, L. F.

    2013-11-01

    Symbiotic stars are key objects in understanding the formation and evolution of interacting binary systems, and are probably the progenitors of Type Ia supernovae. However, the number of known symbiotic stars is much lower than predicted. We aim to search for new symbiotic stars, with particular emphasis on the S-type yellow symbiotic stars, in order to determine their total population, evolutionary timescales, and physical properties. The Two Micron All Sky Survey (2MASS) (J H) versus (H K {sub s}) color-color diagram has been previously used to identify new symbiotic star candidates and show that yellow symbiotics are located in a particular region of that diagram. Candidate symbiotic stars are selected on the basis of their locus in the 2MASS (J H) versus (H K {sub s}) diagram and the presence of H? line emission in the Stephenson and Sanduleak H? survey. This diagram separates S-type yellow symbiotic stars from the rest of the S-type symbiotic stars, allowing us to select candidate yellow symbiotics. To establish the true nature of the candidates, intermediate-resolution spectroscopy is obtained. We have identified the H? emission line source SS 383 as an S-type yellow symbiotic candidate by its position in the 2MASS color-color diagram. The optical spectrum of SS 383 shows Balmer, He I, He II, and [O III] emission lines, in combination with TiO absorption bands that confirm its symbiotic nature. The derived electron density (?10{sup 8-9} cm{sup 3}), He I emission line intensity ratios, and position in the [O III] ?5007/H? versus [O III] ?4363/H? diagram indicate that SS 383 is an S-type symbiotic star, with a probable spectral type of K7-M0 deduced for its cool component based on TiO indices. The spectral type and the position of SS 383 (corrected for reddening) in the 2MASS color-color diagram strongly suggest that SS 383 is an S-type yellow symbiotic. Our result points out that the 2MASS color-color diagram is a powerful tool in identifying new S

  17. A search for stars of very low metal abundance. VI. Detailed abundances of 313 metal-poor stars

    SciTech Connect (OSTI)

    Roederer, Ian U.; Preston, George W.; Thompson, Ian B.; Shectman, Stephen A.; Burley, Gregory S.; Kelson, Daniel D.; Sneden, Christopher

    2014-06-01

    We present radial velocities, equivalent widths, model atmosphere parameters, and abundances or upper limits for 53 species of 48 elements derived from high resolution optical spectroscopy of 313 metal-poor stars. A majority of these stars were selected from the metal-poor candidates of the HK Survey of Beers, Preston, and Shectman. We derive detailed abundances for 61% of these stars for the first time. Spectra were obtained during a 10 yr observing campaign using the Magellan Inamori Kyocera Echelle spectrograph on the Magellan Telescopes at Las Campanas Observatory, the Robert G. Tull Coudé Spectrograph on the Harlan J. Smith Telescope at McDonald Observatory, and the High Resolution Spectrograph on the Hobby-Eberly Telescope at McDonald Observatory. We perform a standard LTE abundance analysis using MARCS model atmospheres, and we apply line-by-line statistical corrections to minimize systematic abundance differences arising when different sets of lines are available for analysis. We identify several abundance correlations with effective temperature. A comparison with previous abundance analyses reveals significant differences in stellar parameters, which we investigate in detail. Our metallicities are, on average, lower by ≈0.25 dex for red giants and ≈0.04 dex for subgiants. Our sample contains 19 stars with [Fe/H] ≤–3.5, 84 stars with [Fe/H] ≤–3.0, and 210 stars with [Fe/H] ≤–2.5. Detailed abundances are presented here or elsewhere for 91% of the 209 stars with [Fe/H] ≤–2.5 as estimated from medium resolution spectroscopy by Beers, Preston, and Shectman. We will discuss the interpretation of these abundances in subsequent papers.

  18. FORMATION AND EVOLUTION OF NUCLEAR STAR CLUSTERS WITH IN SITU STAR FORMATION: NUCLEAR CORES AND AGE SEGREGATION

    SciTech Connect (OSTI)

    Aharon, Danor; Perets, Hagai B.

    2015-02-01

    Nuclear stellar cluster (NSCs) are known to exist around massive black holes (MBHs) in galactic nuclei. Two formation scenarios were suggested for their origin: (1) buildup of NSCs from consecutive infall of stellar clusters and (2) continuous in situ star formation. Though the cluster infall scenario has been extensively studied, the in situ formation scenario has been hardly explored. Here we use Fokker-Planck (FP) calculations to study the effects of star formation on the buildup of NSCs and its implications for their long-term evolution and their resulting structure. We use the FP equation to describe the evolution of stellar populations and add appropriate source terms to account for the effects of newly formed stars. We show that continuous star formation even 1-2 pc away from the MBH can lead to the buildup of an NSC with properties similar to those of the Milky Way NSC. We find that the structure of the old stellar population in the NSC with in situ star formation could be very similar to the steady-state Bahcall-Wolf cuspy structure. However, its younger populations do not yet achieve a steady state. In particular, formed/evolved NSCs with in situ star formation contain differential age-segregated stellar populations that are not yet fully mixed. Younger stellar populations formed in the outer regions of the NSC have a cuspy structure toward the NSC outskirts, while showing a core-like distribution inward, with younger populations having larger core sizes. In principal, such a structure can give rise to an apparent core-like radial distribution of younger stars, as observed in the Galactic center.

  19. The interstellar medium and star formation in local galaxies: Variations of the star formation law in simulations

    SciTech Connect (OSTI)

    Becerra, Fernando; Escala, Andrés

    2014-05-01

    We use the adaptive mesh refinement code Enzo to model the interstellar medium (ISM) in isolated local disk galaxies. The simulation includes a treatment for star formation and stellar feedback. We get a highly supersonic turbulent disk, which is fragmented at multiple scales and characterized by a multi-phase ISM. We show that a Kennicutt-Schmidt relation only holds when averaging over large scales. However, values of star formation rates and gas surface densities lie close in the plot for any averaging size. This suggests an intrinsic relation between stars and gas at cell-size scales, which dominates over the global dynamical evolution. To investigate this effect, we develop a method to simulate the creation of stars based on the density field from the snapshots, without running the code again. We also investigate how the star formation law is affected by the characteristic star formation timescale, the density threshold, and the efficiency considered in the recipe. We find that the slope of the law varies from ∼1.4 for a free-fall timescale, to ∼1.0 for a constant depletion timescale. We further demonstrate that a power law is recovered just by assuming that the mass of the new stars is a fraction of the mass of the cell m {sub *} = ερ{sub gas}Δx {sup 3}, with no other physical criteria required. We show that both efficiency and density threshold do not affect the slope, but the right combination of them can adjust the normalization of the relation, which in turn could explain a possible bi-modality in the law.

  20. On the onset of secondary stellar generations in giant star-forming regions and massive star clusters

    SciTech Connect (OSTI)

    Palou, J.; Wnsch, R.; Tenorio-Tagle, G.

    2014-09-10

    Here we consider the strong evolution experienced by the matter reinserted by massive stars, both in giant star-forming regions driven by a constant star formation rate and in massive and coeval superstar clusters. In both cases we take into consideration the changes induced by stellar evolution on the number of massive stars, the number of ionizing photons, and the integrated mechanical luminosity of the star-forming regions. The latter is at all times compared with the critical luminosity that defines, for a given size, the lower mechanical luminosity limit above which the matter reinserted via strong winds and supernova explosions suffers frequent and recurrent thermal instabilities that reduce its temperature and pressure and inhibit its exit as part of a global wind. Instead, the unstable reinserted matter is compressed by the pervasive hot gas, and photoionization maintains its temperature at T ? 10{sup 4} K. As the evolution proceeds, more unstable matter accumulates and the unstable clumps grow in size. Here we evaluate the possible self-shielding of thermally unstable clumps against the UV radiation field. Self-shielding allows for a further compression of the reinserted matter, which rapidly develops a high-density neutral core able to absorb in its outer skin the incoming UV radiation. Under such conditions the cold (T ? 10 K) neutral cores soon surpass the Jeans limit and become gravitationally unstable, creating a new stellar generation with the matter reinserted by former massive stars. We present the results of several calculations of this positive star formation feedback scenario promoted by strong radiative cooling and mass loading.

  1. NEW UBVRI PHOTOMETRY OF 234 M33 STAR CLUSTERS

    SciTech Connect (OSTI)

    Ma Jun

    2013-04-15

    This is the second paper of our series. In this paper, we present UBVRI photometry for 234 star clusters in the field of M33. For most of these star clusters, there is photometry in only two bands in previous studies. The photometry of these star clusters is performed using archival images from the Local Group Galaxies Survey, which covers 0.8 deg{sup 2} along the major axis of M33. Detailed comparisons show that, in general, our photometry is consistent with previous measurements, and in particular that our photometry is in good agreement with that of Zloczewski and Kaluzny. Combined with star cluster photometry in previous studies, we present some results: none of the M33 youngest clusters ({approx}10{sup 7} yr) have masses approaching 10{sup 5} M{sub Sun }, and comparisons with models of simple stellar populations suggest a large range of ages for M33 star clusters and some as old as the Galactic globular clusters.

  2. ELEVEN NEW HEAVILY REDDENED FIELD WOLF-RAYET STARS

    SciTech Connect (OSTI)

    Smith, J. D. T.; Cushing, Michael; Barletta, Anthony; McCarthy, Don; Kulesa, Craig; Van Dyk, Schuyler D.

    2012-12-01

    We report the results of a medium-narrowband 2 {mu}m line survey covering 5.8 deg{sup 2} near the Galactic plane. We confirm 11 new field Wolf-Rayet stars along three lines of sight probing the inner Galaxy, demonstrating the capability to uncover distant and highly reddened populations of Galactic wind-borne emission-line stars suffering extinction as high as A{sub V} {approx} 40 and as distant as 9 kpc down to modest magnitude limits of K{sub s} {approx} 12.5. All stars are of subtype WC7-8, with median distance d = 6 kpc and median extinction A{sub K{sub s}} = 2.5. Over the fields surveyed, the density of Wolf-Rayet stars to limiting magnitude K{sub s} {approx} 12.5 was found to be 1.9 deg{sup -2}. We compare this to models which predict their distribution within the Galaxy and find that, even neglecting survey and subtype incompleteness, they consistently underpredict the number of newly discovered stars along the surveyed lines of sight.

  3. SPINDOWN OF ISOLATED NEUTRON STARS: GRAVITATIONAL WAVES OR MAGNETIC BRAKING?

    SciTech Connect (OSTI)

    Staff, Jan E.; Jaikumar, Prashanth; Chan, Vincent; Ouyed, Rachid

    2012-05-20

    We study the spindown of isolated neutron stars from initially rapid rotation rates, driven by two factors: (1) gravitational wave emission due to r-modes and (2) magnetic braking. In the context of isolated neutron stars, we present the first study including self-consistently the magnetic damping of r-modes in the spin evolution. We track the spin evolution employing the RNS code, which accounts for the rotating structure of neutron stars for various equations of state. We find that, despite the strong damping due to the magnetic field, r-modes alter the braking rate from pure magnetic braking for B {<=} 10{sup 13} G. For realistic values of the saturation amplitude {alpha}{sub sat}, the r-mode can also decrease the time to reach the threshold central density for quark deconfinement. Within a phenomenological model, we assess the gravitational waveform that would result from r-mode-driven spindown of a magnetized neutron star. To contrast with the persistent signal during the spindown phase, we also present a preliminary estimate of the transient gravitational wave signal from an explosive quark-hadron phase transition, which can be a signal for the deconfinement of quarks inside neutron stars.

  4. Spin-down dynamics of magnetized solar-type stars

    SciTech Connect (OSTI)

    Oglethorpe, R. L. F.; Garaud, P.

    2013-12-01

    It has long been known that solar-type stars undergo significant spin-down, via magnetic braking, during their main-sequence lifetimes. However, magnetic braking only operates on the surface layers; it is not yet completely understood how angular momentum is transported within the star and how rapidly the spin-down information is communicated to the deep interior. In this work, we use insight from recent progress in understanding internal solar dynamics to model the interior of other solar-type stars. We assume, following Gough and McIntyre, that the bulk of the radiation zone of these stars is held in uniform rotation by the presence of an embedded large-scale primordial field, confined below a stably stratified, magnetic-free tachocline by large-scale meridional flows downwelling from the convection zone. We derive simple equations to describe the response of this model interior to spin-down of the surface layers, which are identical to the two-zone model of MacGregor and Brenner, with a coupling timescale proportional to the local Eddington-Sweet timescale across the tachocline. This timescale depends both on the rotation rate of the star and on the thickness of the tachocline, and it can vary from a few hundred thousand years to a few Gyr, depending on stellar properties. Qualitative predictions of the model appear to be consistent with observations, although they depend sensitively on the assumed functional dependence of the tachocline thickness on the stellar rotation rate.

  5. Effects of intermediate mass black holes on nuclear star clusters

    SciTech Connect (OSTI)

    Mastrobuono-Battisti, Alessandra; Perets, Hagai B.; Loeb, Abraham

    2014-11-20

    Nuclear star clusters (NSCs) are dense stellar clusters observed in galactic nuclei, typically hosting a central massive black hole. Here we study the possible formation and evolution of NSCs through the inspiral of multiple star clusters hosting intermediate mass black holes (IMBHs). Using an N-body code, we examine the dynamics of the IMBHs and their effects on the NSC. We find that IMBHs inspiral to the core of the newly formed NSC and segregate there. Although the IMBHs scatter each other and the stars, none of them is ejected from the NSC. The IMBHs are excited to high eccentricities and their radial density profile develops a steep power-law cusp. The stars also develop a power-law cusp (instead of the central core that forms in their absence), but with a shallower slope. The relaxation rate of the NSC is accelerated due to the presence of IMBHs, which act as massive perturbers. This in turn fills the loss cone and boosts the tidal disruption rate of stars both by the MBH and the IMBHs to a value excluded by rate estimates based on current observations. Rate estimates of tidal disruptions can therefore provide a cumulative constraint on the existence of IMBHs in NSCs.

  6. The Fate of the Compact Remnant in Neutron Star Mergers

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

    Fryer, Chris L.; Belczynski, Krzysztoff; Ramirez-Ruiz, Enrico; Rosswog, Stephan; Shen, Gang; Steiner, Andrew W.

    2015-10-06

    Neutron star (binary neutron star and neutron star - black hole) mergers are believed to produce short-duration gamma-ray bursts. They are also believed to be the dominant source of gravitational waves to be detected by the advanced LIGO and the dominant source of the heavy r-process elements in the universe. Whether or not these mergers produce short-duration GRBs depends sensitively on the fate of the core of the remnant (whether, and how quickly, it forms a black hole). In this paper, we combine the results of merger calculations and equation of state studies to determine the fate of the coresmore » of neutron star mergers. Using population studies, we can determine the distribution of these fates to compare to observations. We find that black hole cores form quickly only for equations of state that predict maximum non-rotating neutron star masses below 2.3-2.4 solar masses. If quick black hole formation is essential in producing gamma-ray bursts, LIGO observed rates compared to GRB rates could be used to constrain the equation of state for dense nuclear matter.« less

  7. Stellar signatures of AGN-jet-triggered star formation

    SciTech Connect (OSTI)

    Dugan, Zachary; Silk, Joseph; Bryan, Sarah; Gaibler, Volker; Haas, Marcel

    2014-12-01

    To investigate feedback between relativistic jets emanating from active galactic nuclei and the stellar population of the host galaxy, we analyze the long-term evolution of the orbits of the stars formed in the galaxy-scale simulations by Gaibler et al. of jets in massive, gas-rich galaxies at z ? 2-3. We find strong, jet-induced differences in the resulting stellar populations of galaxies that host relativistic jets and galaxies that do not, including correlations in stellar locations, velocities, and ages. Jets are found to generate distributions of increased radial and vertical velocities that persist long enough to effectively augment the stellar structure of the host. The jets cause the formation of bow shocks that move out through the disk, generating rings of star formation within the disk. The bow shock often accelerates pockets of gas in which stars form, yielding populations of stars with significant radial and vertical velocities, some of which have large enough velocities to escape the galaxy. These stellar population signatures can serve to identify past jet activity as well as jet-induced star formation.

  8. Friedrich: ENERGY STAR Referral (CP15F10) | Department of Energy

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

    CP15F10) Friedrich: ENERGY STAR Referral (CP15F10) August 18, 2011 DOE referred the matter of Friedrich room air conditioner model CP15F10 to the U.S. Environmental Protection Agency, brand manager for the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. Friedrich: ENERGY STAR Referral (CP15F10) (89.48 KB) More Documents & Publications Friedrich: ENERGY STAR Referral (CP15F10) Friedrich: ENERGY STAR Referral

  9. Lone Tree, Colorado: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Tree, Colorado: Energy Resources Jump to: navigation, search Equivalent URI DBpedia Coordinates 39.5360997, -104.8963682 Show Map Loading map... "minzoom":false,"mappingservic...

  10. Overview of Silicon Detectors in STAR: Present and Future

    SciTech Connect (OSTI)

    Kabana, Sonia; Collaboration: The SVT, SSD and HFT detector groups of the STAR experiment at RHIC

    2011-12-13

    The STAR experiment at RHIC aims to study the QCD phase transition and the origin of the spin of the proton. Its main detector for charged particle track reconstruction is a Time Projection Chamber, which has been supplemented with a silicon detector involving two different technologies, in particular double-sided silicon strip and silicon drift technology. STAR is preparing now for a new Silicon Vertex Detector, using double-sided silicon strip, single-sided silicon strip-pads, and CMOS monolithic active pixel sensors technology, planned to take data in 2014. We give an overview of the design, calibration and performances of the silicon detectors used by the STAR experiment in the past and the expected performances of the future silicon detector upgrade.

  11. IDENTIFYING BLUE HORIZONTAL BRANCH STARS USING THE z FILTER

    SciTech Connect (OSTI)

    Vickers, John J.; Grebel, Eva K.; Huxor, Avon P.

    2012-04-15

    In this paper we present a new method for selecting blue horizontal branch (BHB) candidates based on color-color photometry. We make use of the Sloan Digital Sky Survey z band as a surface gravity indicator and show its value for selecting BHB stars from quasars, white dwarfs, and main-sequence A-type stars. Using the g, r, i, and z bands, we demonstrate that extraction accuracies on a par with more traditional u, g, and r photometric selection methods may be achieved. We also show that the completeness necessary to probe major Galactic structure may be maintained. Our new method allows us to efficiently select BHB stars from photometric sky surveys that do not include a u-band filter such as the Panoramic Survey Telescope and Rapid Response System.

  12. Mass radius relation of compact stars in the braneworld

    SciTech Connect (OSTI)

    Castro, Luis B.; Menezes, Dbora P.; Alloy, Marcelo D. E-mail: alloy@uffs.edu.br

    2014-08-01

    The braneworld scenario, based on the fact that the four dimension space-time is a hyper-surface of a five dimensional manifold, was shown to deal in a satisfactory way with the hierarchy problem. In this work we study macroscopic stellar properties of compact stars from the braneworld point of view. Using neutron star equations of state, we test the possibility of extra dimensions by solving the brane Tolman-Oppenheimer-Volkoff equations obtained for three kinds of possible compact objects: hadronic, hybrid and quark stars. By comparing the macroscopic solutions with observational constraints, we establish a brane tension lower limit and the value for which the Tolman-Oppenheimer-Volkoff equations in the braneworld converge to the usual Tolman-Oppenheimer-Volkoff equations.

  13. DOUBLE STARS IN THE USNO CCD ASTROGRAPHIC CATALOG

    SciTech Connect (OSTI)

    Hartkopf, William I.; Mason, Brian D.; Finch, Charlie T.; Zacharias, Norbert; Wycoff, Gary L.; Hsu, Danley E-mail: bdm@usno.navy.mil E-mail: nz@usno.navy.mil

    2013-10-01

    The newly completed Fourth USNO CCD Astrographic Catalog (UCAC4) has proven to be a rich source of double star astrometry and photometry. Following initial comparisons of UCAC4 results against those obtained by speckle interferometry, the UCAC4 catalog was matched against known double stars in the Washington Double Star Catalog in order to provide additional differential astrometry and photometry for these pairs. Matches to 58,131 pairs yielded 61,895 astrometric and 68,935 photometric measurements. Finally, a search for possible new common proper motion (CPM) pairs was made using new UCAC4 proper motion data; this resulted in 4755 new potential CPM doubles (and an additional 27,718 astrometric and photometric measures from UCAC and other sources)

  14. The origin of the most iron-poor star

    SciTech Connect (OSTI)

    Marassi, S.; Schneider, R.; Limongi, M. [INAF/Osservatorio Astronomico di Roma, Via di Frascati 33, I-00040 Monteporzio (Italy); Chiaki, G.; Yoshida, N. [Department of Physics, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033 (Japan); Omukai, K. [Astronomical Institute, Tohoku University, Sendai 980-8578 (Japan); Nozawa, T. [National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588 (Japan); Chieffi, A., E-mail: stefania.marassi@oa-roma.inaf.it [INAF/IASF, Via Fosso del Cavaliere 100, I-00133 Roma (Italy)

    2014-10-20

    We investigate the origin of carbon-enhanced metal-poor (CEMP) stars starting from the recently discovered [Fe/H] < -7.1 star SMSS J031300. We show that the elemental abundances observed on the surface of SMSS J031300 can be well fit by the yields of faint, metal-free, supernovae (SNe). Using properly calibrated faint SN explosion models, we study, for the first time, the formation of dust grains in such carbon-rich, iron-poor SN ejecta. Calculations are performed assuming both unmixed and uniformly mixed ejecta and taking into account the partial destruction by the SN reverse shock. We find that, due to the paucity of refractory elements beside carbon, amorphous carbon is the only grain species to form, with carbon condensation efficiencies that range between (0.15 and 0.84), resulting in dust yields in the range (0.025-2.25) M {sub ?}. We follow the collapse and fragmentation of a star-forming cloud enriched by the products of these faint SN explosions and we explore the role played by fine structure line cooling and dust cooling. We show that even if grain growth during the collapse has a minor effect of the dust-to-gas ratio, due to C depletion into CO molecules at an early stage of the collapse, the formation of CEMP low-mass stars, such as SMSS J031300, could be triggered by dust cooling and fragmentation. A comparison between model predictions and observations of a sample of C-normal and C-rich metal-poor stars supports the idea that a single common pathway may be responsible for the formation of the first low-mass stars.

  15. Clementine Star Tracker Stellar Compass: Final report part 1

    SciTech Connect (OSTI)

    Priest, R.E.; Kordas, J.F.; Lewis, I.T.

    1995-07-01

    The Clementine mission provided the first ever complete, systematic surface mapping of the moon from the ultra-violet to the near-infrared regions. More than 1.7 million images of the moon, earth and space were returned from this mission. Two star stracker stellar compasses (star tracker camera + stellar compass software) were included on the spacecraft, serving a primary function of providing angle updates to the guidance and navigation system. These cameras served a secondary function by providing a wide field of view imaging capability for lunar horizon glow and other dark-side imaging data. This 290 g camera using a 576 x 384 focal plane array and a 17 mm entrance pupil, detected and centroided stars as dim and dimmer than 4.5 m{sub v}, providing rms pointing accuracy of better than 100 {mu}rad pitch and yaw and 450 {mu}rad roll. A description of this light-weight, low power star tracker camera along with a summary of lessons learned is presented. Design goals and preliminary on-orbit performance estimates are addressed in terms of meeting the mission`s primary objective for flight qualifying the sensors for future Department of Defense flights. Documentation generated during the design, analysis, build, test and characterization of the star tracker cameras are presented. Collectively, this documentation represents a small library of information for this camera, and may be used as a framework for producing copy units by commercial enterprises, and therefore satisfies a Department of Defense and Department of Energy goal to transfer technology to industry. However, the considerable knowledge gained from the experience of the individuals involved in the system trades, design, analysis, production, testing and characterization of the star tracker stellar compass is not contained in this documentation.

  16. AN ULTRAVIOLET INVESTIGATION OF ACTIVITY ON EXOPLANET HOST STARS

    SciTech Connect (OSTI)

    Shkolnik, Evgenya L.

    2013-03-20

    Using the far-UV (FUV) and near-UV (NUV) photometry from the NASA Galaxy Evolution Explorer (GALEX), we searched for evidence of increased stellar activity due to tidal and/or magnetic star-planet interactions (SPI) in the 272 known FGK planetary hosts observed by GALEX. With the increased sensitivity of GALEX, we are able probe systems with lower activity levels and at larger distances than what has been done to date with X-ray satellites. We compared samples of stars with close-in planets (a < 0.1 AU) to those with far-out planets (a > 0.5 AU) and looked for correlations of excess activity with other system parameters. This statistical investigation found no clear correlations with a, M{sub p} , or M{sub p} /a, in contrast to some X-ray and Ca II studies. However, there is tentative evidence (at a level of 1.8{sigma}) that stars with radial-velocity-(RV)-detected close-in planets are more FUV-active than stars with far-out planets, in agreement with several published X-ray and Ca II results. The case is strengthened to a level of significance to 2.3{sigma} when transit-detected close-in planets are included. This is most likely because the RV-selected sample of stars is significantly less active than the field population of comparable stars, while the transit-selected sample is similarly active. Given the factor of 2-3 scatter in fractional FUV luminosity for a given stellar effective temperature, it is necessary to conduct a time-resolved study of the planet hosts in order to better characterize their UV variability and generate a firmer statistical result.

  17. ORIGIN OF THE GALAXY MASS-METALLICITY-STAR FORMATION RELATION

    SciTech Connect (OSTI)

    Harwit, Martin; Brisbin, Drew

    2015-02-20

    We describe an equilibrium model that links the metallicity of low-redshift galaxies to stellar evolution models. It enables the testing of different stellar initial mass functions and metal yields against observed galaxy metallicities. We show that the metallicities of more than 80,000 Sloan Digital Sky Survey galaxies in the low-redshift range 0.07 ? z ? 0.3 considerably constrain stellar evolution models that simultaneously relate galaxy stellar mass, metallicity, and star formation rates to the infall rate of low-metallicity extragalactic gas and outflow of enriched matter. A feature of our model is that it encompasses both the active star forming phases of a galaxy and epochs during which the same galaxy may lie fallow. We show that the galaxy mass-metallicity-star formation relation can be traced to infall of extragalactic gas mixing with native gas from host galaxies to form stars of observed metallicities, the most massive of which eject oxygen into extragalactic space. Most consequential among our findings is that, on average, extragalactic infall accounts for one half of the gas required for star formation, a ratio that is remarkably constant across galaxies with stellar masses ranging at least from M* = 2 10{sup 9} to 6 10{sup 10} M {sub ?}. This leads us to propose that star formation is initiated when extragalactic infall roughly doubles the mass of marginally stable interstellar clouds. The processes described may also account quantitatively for the metallicity of extragalactic space, though to check this the fraction of extragalactic baryons will need to be more firmly established.

  18. Tierra Concrete Homes Honored with Energy Star Award

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

    Tierra Concrete Homes Honored with Energy Star Award For more information contact: Sarah Holmes Barba, 303-275-3023 email: Sarah Homes Barba Golden, Colo., August 8, 2001 - Tierra Concrete Homes, Inc. of Pueblo, Colo., has been recognized as a leader in energy-efficient home building by Energy Star, a national program that develops energy-saving partnerships with the home building industry. The first-ever "Most Energy-Efficient Homes of the New Millennium" award was presented to

  19. The Many Faces - and Phases - of Neutron Stars

    SciTech Connect (OSTI)

    Piekarewicz, J.

    2007-10-26

    Understanding the equation of state (EOS) of nuclear matter 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 EOS of cold baryonic matter with special emphasis on its impact on the structure and dynamics of neutron stars. In particular, I will discuss the many fascinating phases that one encounters as one travels from the low-density crust to the high-density core.

  20. 3.17 The Stars Above Us, Govern Our Conditions

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

    2 6/1/2011 3.17 The Stars Above Us, Govern Our Conditions The origins of chemical elements found on Earth-nuclear reactions that take place in stars-were discovered and confirmed by researchers supported by the Office of Science and predecessor agencies. The late William Fowler of the California Institute of Technology won half of the 1983 Nobel Prize in physics for his work in elucidating this process of nucleosynthesis. Fowler carried out experimental studies of nuclear reactions of

  1. A star harbouring a wormhole at its core

    SciTech Connect (OSTI)

    Dzhunushaliev, Vladimir; Folomeev, Vladimir; Kleihaus, Burkhard; Kunz, Jutta E-mail: vfolomeev@mail.ru E-mail: kunz@theorie.physik.uni-oldenburg.de

    2011-04-01

    We consider a configuration consisting of a wormhole filled by a perfect fluid. Such a model can be applied to describe stars as well as neutron stars with a nontrivial topology. The presence of a tunnel allows for motion of the fluid, including oscillations near the core of the system. Choosing the polytropic equation of state for the perfect fluid, we obtain static regular solutions. Based on these solutions, we consider small radial oscillations of the configuration and show that the solutions are stable with respect to linear perturbations in the external region.

  2. ENERGY STAR Webinar: Introducing Waste & Materials Tracking in Portfolio

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

    Manager | Department of Energy Introducing Waste & Materials Tracking in Portfolio Manager ENERGY STAR Webinar: Introducing Waste & Materials Tracking in Portfolio Manager August 18, 2016 2:00PM to 3:30PM EDT Hosted by the U.S. Environmental Protection Agency's (EPA's) ENERGY STAR, this webinar will show how to track your building's waste and materials management. It will introduce the types of waste and disposal methods attendees can track, new metrics and reports, and how you can

  3. All Stars of the Better Buildings Summit | Department of Energy

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

    All Stars of the Better Buildings Summit All Stars of the Better Buildings Summit June 15, 2016 - 4:04pm Addthis BetterBuildingsLogo.png By Monica Kanojia This year's Better Buildings Summit was filled with the announcement of several exceptional milestones and Partner achievements. U.S. Energy Secretary Ernest Moniz lauded the initiative's $1.3 billion in energy cost savings coupled with the avoidance of 10 million tons of harmful carbon emissions, as well as the Challenge Partners that

  4. STARS A Two Stage High Gain Harmonic Generation FEL Demonstrator

    SciTech Connect (OSTI)

    M. Abo-Bakr; W. Anders; J. Bahrdt; P. Budz; K.B. Buerkmann-Gehrlein; O. Dressler; H.A. Duerr; V. Duerr; W. Eberhardt; S. Eisebitt; J. Feikes; R. Follath; A. Gaupp; R. Goergen; K. Goldammer; S.C. Hessler; K. Holldack; E. Jaeschke; Thorsten Kamps; S. Klauke; J. Knobloch; O. Kugeler; B.C. Kuske; P. Kuske; A. Meseck; R. Mitzner; R. Mueller; M. Neeb; A. Neumann; K. Ott; D. Pfluckhahn; T. Quast; M. Scheer; Th. Schroeter; M. Schuster; F. Senf; G. Wuestefeld; D. Kramer; Frank Marhauser

    2007-08-01

    BESSY is proposing a demonstration facility, called STARS, for a two-stage high-gain harmonic generation free electron laser (HGHG FEL). STARS is planned for lasing in the wavelength range 40 to 70 nm, requiring a beam energy of 325 MeV. The facility consists of a normal conducting gun, three superconducting TESLA-type acceleration modules modified for CW operation, a single stage bunch compressor and finally a two-stage HGHG cascaded FEL. This paper describes the faciliy layout and the rationale behind the operation parameters.

  5. DOE Testing Reveals Samsung Refrigerator Does Not Meet Energy Star Requirements

    Broader source: Energy.gov [DOE]

    DOE-initiated testing has revealed that a Samsung refrigerator (model RF26VAB), which the company had claimed was Energy Star compliant, consumed more energy than permitted by the Energy Star...

  6. THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY...

    Office of Scientific and Technical Information (OSTI)

    NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION Citation Details In-Document Search Title: THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY...

  7. Energy All-Stars Shine Bright at Inaugural Lecture Series | Department...

    Office of Environmental Management (EM)

    All-Stars Shine Bright at Inaugural Lecture Series Energy All-Stars Shine Bright at Inaugural Lecture Series January 22, 2013 - 3:38pm Addthis Energy Secretary Steven Chu talks about ...

  8. Department of Energy to Take Steps to Remove ENERGY STAR Label...

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

    As a result, effective January 2, 2010, certain LG French-door refrigerators are no longer eligible to carry the ENERGY STAR label. ENERGY STAR is a voluntary program sponsored ...

  9. DOE Refers Two ENERGY STAR Models to EPA for Potential De-Listing...

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

    Two ENERGY STAR Models to EPA for Potential De-Listing DOE Refers Two ENERGY STAR Models to EPA for Potential De-Listing January 11, 2012 - 11:00am Addthis U.S. Department of...

  10. Evaluation Prompts ENERGY STAR Program to Replace Web Tool, Saving 90 Percent of Annual Costs

    Office of Energy Efficiency and Renewable Energy (EERE)

    This document, from the U.S. Environmental Protection Agency's ENERGY STAR Residential Program, is part of the Case Study Series, highlighting how "Evaluation Prompts ENERGY STAR Program to Replace Web Tool, Saving 90 Percent of Annual Costs."

  11. Comment submitted by InterMetro Industries Corp. regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by InterMetro Industries Corp. regarding the Energy Star Verification Testing Program

  12. Comment submitted by Hobart/ITW Food Equipment Group regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Hobart/ITW Food Equipment Group regarding the Energy Star Verification Testing Program

  13. Comment submitted by Hoshizaki America, Inc. regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Hoshizaki America, Inc. regarding the Energy Star Verification Testing Program

  14. Comment submitted by Ingersoll Rand Residential Solutions regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Ingersoll Rand Residential Solutions regarding the Energy Star Verification Testing Program

  15. Comment submitted by United Lighting, Inc. regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by United Lighting, Inc. regarding the Energy Star Verification Testing Program

  16. Comment submitted by BSH Home Appliances Corporation regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by BSH Home Appliances Corporation regarding the Energy Star Verification Testing Program

  17. Comment submitted by the Natural Resources Defense Council (NRDC) regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by the Natural Resources Defense Council (NRDC) regarding the Energy Star Verification Testing Program

  18. DOE Verification Testing in Support of ENERGY STAR, April 22, 2011 |

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

    Department of Energy 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 testing process, dated April 22, 2011 estar_verification_process.pdf (368.74 KB) More Documents & Publications Comment submitted by Hoshizaki America, Inc. regarding the Energy Star Verification Testing Program Comment submitted by the North American Association of Food Equipment

  19. Comment submitted by CertainTeed Corporation regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by CertainTeed Corporation regarding the Energy Star Verification Testing Program

  20. Comment submitted by the Bradford White Corporation (BWC) regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by the Bradford White Corporation (BWC) regarding the Energy Star Verification Testing Program

  1. Comment submitted by Energizer Battery Manufacturing, Inc. regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by Energizer Battery Manufacturing, Inc. regarding the Energy Star Verification Testing Program

  2. Comment submitted by the Alliance for Water Efficiency (AWE) regarding the Energy Star Verification Testing Program

    Broader source: Energy.gov [DOE]

    This document is a comment submitted by the Alliance for Water Efficiency (AWE) regarding the Energy Star Verification Testing Program

  3. Comment submitted by A. O. Smith Corporation regarding the Energy Star Verification Testing Program

    Office of Energy Efficiency and Renewable Energy (EERE)

    This document is a comment submitted by A. O. Smith Corporation regarding the Energy Star Verification Testing Program

  4. Absolute properties of the eclipsing binary star V501 Herculis

    SciTech Connect (OSTI)

    Lacy, Claud H. Sandberg; Fekel, Francis C. E-mail: fekel@evans.tsuniv.edu

    2014-10-01

    V501 Her is a well detached G3 eclipsing binary star with a period of 8.597687 days for which we have determined very accurate light and radial-velocity curves using robotic telescopes. Results of these data indicate that the component stars have masses of 1.269 ± 0.004 and 1.211 ± 0.003 solar masses, radii of 2.001 ± 0.003 and 1.511 ± 0.003 solar radii, and temperatures of 5683 ± 100 K and 5720 ± 100 K, respectively. Comparison with the Yonsei-Yale series of evolutionary models results in good agreement at an age of about 5.1 Gyr for a somewhat metal-rich composition. Those models indicate that the more massive, larger, slightly cooler star is just beyond core hydrogen exhaustion while the less massive, smaller, slightly hotter star has not quite reached core hydrogen exhaustion. The orbit is not yet circularized, and the components are rotating at or near their pseudosynchronous velocities. The distance to the system is 420 ± 30 pc.

  5. Gluon Vortices and Induced Magnetic Field in Compact Stars

    SciTech Connect (OSTI)

    Ferrer, Efrain J.

    2007-10-26

    The natural candidates for the realization of color superconductivity are the extremely dense cores of compact stars, many of which have very large magnetic fields, especially the so called magnetars. In this paper we discuss how a color superconducting core can serve to generate and enhance the stellar magnetic field without appealing to a magnetohydrodynamic dynamo mechanism.

  6. THE INFRARED TELESCOPE FACILITY (IRTF) SPECTRAL LIBRARY: COOL STARS

    SciTech Connect (OSTI)

    Rayner, John T.; Cushing, Michael C.; Vacca, William D. E-mail: michael.cushing@gmail.com

    2009-12-01

    We present a 0.8-5 {mu}m spectral library of 210 cool stars observed at a resolving power of R {identical_to} {lambda}/{delta}{lambda} {approx} 2000 with the medium-resolution infrared spectrograph, SpeX, at the 3.0 m NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii. The stars have well-established MK spectral classifications and are mostly restricted to near-solar metallicities. The sample not only contains the F, G, K, and M spectral types with luminosity classes between I and V, but also includes some AGB, carbon, and S stars. In contrast to some other spectral libraries, the continuum shape of the spectra is measured and preserved in the data reduction process. The spectra are absolutely flux calibrated using the Two Micron All Sky Survey photometry. Potential uses of the library include studying the physics of cool stars, classifying and studying embedded young clusters and optically obscured regions of the Galaxy, evolutionary population synthesis to study unresolved stellar populations in optically obscured regions of galaxies and synthetic photometry. The library is available in digital form from the IRTF Web site.

  7. Calendar Year 2009 Program Benefits for ENERGY STAR Labeled Products

    SciTech Connect (OSTI)

    Homan, Gregory K; Sanchez, Marla C.; Brown, Richard E.

    2010-11-15

    ENERGY STAR is a voluntary energy efficiency labeling program operated jointly by the Environmental Protection Agency (US EPA) and the U.S. Department of Energy (US DOE), designed to identify and promote energy-efficient products, buildings and practices. Since the program inception in 1992, ENERGY STAR has become a leading international brand for energy efficient products, and currently labels more than thirty products, spanning office equipment, heating, cooling and ventilation equipment, commercial and residential lighting, home electronics, and major appliances. ENERGY STAR's central role in the development of regional, national and international energy programs necessitates an open process whereby its program achievements to date as well as projected future savings are shared with stakeholders. This report presents savings estimates from the use ENERGY STAR labeled products. We present estimates of energy, dollar, and carbon savings achieved by the program in the year 2009, annual forecasts for 2010 and 2011, and cumulative savings estimates for the period 1993 through 2009 and cumulative forecasts for the period 2010 through 2015. Through 2009 the program saved 9.5 Quads of primary energy and avoided the equivalent of 170 million metric tons carbon (MMTC). The forecast for the period 2009-2015 is 11.5 Quads or primary energy saved and 202 MMTC emissions avoided. The sensitivity analysis bounds the best estimate of carbon avoided between 110 MMTC and 231 MMTC (1993 to 2009) and between 130 MMTC and 285 MMTC (2010 to 2015).

  8. HOW CAN NEWLY BORN RAPIDLY ROTATING NEUTRON STARS BECOME MAGNETARS?

    SciTech Connect (OSTI)

    Cheng, Quan; Yu, Yun-Wei

    2014-05-10

    In a newly born (high-temperature and Keplerian rotating) neutron star, r-mode instability can lead to stellar differential rotation, which winds the seed poloidal magnetic field (∼10{sup 11} G) to generate an ultra-high (∼10{sup 17} G) toroidal field component. Subsequently, by succumbing to the Tayler instability, the toroidal field could be partially transformed into a new poloidal field. Through such dynamo processes, the newly born neutron star with sufficiently rapid rotation could become a magnetar on a timescale of ∼10{sup 2} {sup –} {sup 3} s, with a surface dipolar magnetic field of ∼10{sup 15} G. Accompanying the field amplification, the star could spin down to a period of ∼5 ms through gravitational wave radiation due to the r-mode instability and, in particular, the non-axisymmetric stellar deformation caused by the toroidal field. This scenario provides a possible explanation for why the remnant neutron stars formed in gamma-ray bursts and superluminous supernovae could be millisecond magnetars.

  9. Pair instability supernovae of very massive population III stars

    SciTech Connect (OSTI)

    Chen, Ke-Jung; Woosley, Stan; Heger, Alexander; Almgren, Ann; Whalen, Daniel J.

    2014-09-01

    Numerical studies of primordial star formation suggest that the first stars in the universe may have been very massive. Stellar models indicate that non-rotating Population III stars with initial masses of 140-260 M {sub ☉} die as highly energetic pair-instability supernovae. We present new two-dimensional simulations of primordial pair-instability supernovae done with the CASTRO code. Our simulations begin at earlier times than previous multidimensional models, at the onset of core contraction, to capture any dynamical instabilities that may be seeded by core contraction and explosive burning. Such instabilities could enhance explosive yields by mixing hot ash with fuel, thereby accelerating nuclear burning, and affect the spectra of the supernova by dredging up heavy elements from greater depths in the star at early times. Our grid of models includes both blue supergiants and red supergiants over the range in progenitor mass expected for these events. We find that fluid instabilities driven by oxygen and helium burning arise at the upper and lower boundaries of the oxygen shell ∼20-100 s after core bounce. Instabilities driven by burning freeze out after the SN shock exits the helium core. As the shock later propagates through the hydrogen envelope, a strong reverse shock forms that drives the growth of Rayleigh-Taylor instabilities. In red supergiant progenitors, the amplitudes of these instabilities are sufficient to mix the supernova ejecta.

  10. PROTOSTELLAR OUTFLOWS AND RADIATIVE FEEDBACK FROM MASSIVE STARS

    SciTech Connect (OSTI)

    Kuiper, Rolf; Yorke, Harold W.; Turner, Neal J. E-mail: Harold.W.Yorke@jpl.nasa.gov

    2015-02-20

    We carry out radiation hydrodynamical simulations of the formation of massive stars in the super-Eddington regime including both their radiative feedback and protostellar outflows. The calculations start from a prestellar core of dusty gas and continue until the star stops growing. The accretion ends when the remnants of the core are ejected, mostly by the force of the direct stellar radiation in the polar direction and elsewhere by the reradiated thermal infrared radiation. How long the accretion persists depends on whether the protostellar outflows are present. We set the mass outflow rate to 1% of the stellar sink particle's accretion rate. The outflows open a bipolar cavity extending to the core's outer edge, through which the thermal radiation readily escapes. The radiative flux is funneled into the polar directions while the core's collapse proceeds near the equator. The outflow thus extends the ''flashlight effect'', or anisotropic radiation field, found in previous studies from the few hundred AU scale of the circumstellar disk up to the 0.1 parsec scale of the core. The core's flashlight effect allows core gas to accrete on the disk for longer, in the same way that the disk's flashlight effect allows disk gas to accrete on the star for longer. Thus although the protostellar outflows remove material near the core's poles, causing slower stellar growth over the first few free-fall times, they also enable accretion to go on longer in our calculations. The outflows ultimately lead to stars of somewhat higher mass.

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

    Office of Legacy Management (LM)

    ... F30885 4 4.1 F30885: Chain of Custody Page 2 of 2 18 of 18 F30885 4 4.1 071505 Technical Report for S M Stoller Star Center-WWNA Monthly; Largo, FL 7030-226 Accutest Job Number: ...

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

    Office of Legacy Management (LM)

    ... F28014 4 4.1 F28014: Chain of Custody Page 2 of 2 12 of 12 F28014 4 4.1 122704 Technical Report for S M Stoller Star Center-WWNA Monthly; Largo, FL 7030-226 Accutest Job Number: ...

  13. Comet Riders--Nuclear nomads to the stars

    SciTech Connect (OSTI)

    Angelo, J.A. Jr. ); Buden, D. )

    1991-01-01

    This paper describes the potential role of an evolutionary family of advanced space nuclear power systems (solid core reactor, gas core reactor, and thermonulcear fusion systems) in the detailed exploration of Solar System comets and in the use of interstellar comes to support migratory journeys to the stars by both human beings and their smart robot systems. 14 refs., 5 figs., 2 tabs.

  14. ENERGY STAR Webinar: Zero Energy Ready Home Program

    Broader source: Energy.gov [DOE]

    Once a home is as good as ENERGY STAR, the modest added “lift” to bring a home up to DOE’s Zero Energy Ready specs unleashes a wave of powerful value messages.  DOE Zero Energy Ready Homes live...

  15. The massive star population in M101. II. Spatial variations in the recent star formation history

    SciTech Connect (OSTI)

    Grammer, Skyler; Humphreys, Roberta M. E-mail: roberta@umn.edu

    2014-09-01

    We investigate star formation history (SFH) as a function of radius in M101 using archival Hubble Space Telescope Advanced Camera for Surveys photometry. We derive the SFH from the resolved stellar populations in five 2' wide annuli. Binning the SFH into time frames corresponding to stellar populations traced by Hα, far-ultraviolet, and near-ultraviolet emission, we find that the fraction of stellar populations young enough to contribute in Hα is 15%-35% in the inner regions, compared to less than 5% in the outer regions. This provides a sufficient explanation for the lack of Hα emission at large radii. We also model the blue to red supergiant ratio in our five annuli, examine the effects that a metallicity gradient and variable SFH have on the predicted ratios, and compare to the observed values. We find that the radial behavior of our modeled blue to red supergiant ratios is highly sensitive to both spatial variations in the SFH and metallicity. Incorporating the derived SFH into modeled ratios, we find that we are able to reproduce the observed values at large radii (low metallicity), but at small radii (high metallicity) the modeled and observed ratios are discrepant.

  16. LANL/Green Star Tests of the Green Star SBS-60 Spectrometer

    SciTech Connect (OSTI)

    T. E. Sampson; D. T. Vo; T. L. Cremers; P. A. Hypes; Y. P. Seldiakov; A. B. Dorin; M. V. Kondrashov; V. I. Timoshin

    2001-06-01

    We report on joint testing of the Russian-designed and manufactured single board spectrometer SBS-60 from Green Star Ltd. of Moscow. The SBS-60 will be used to make material control and accountability measurements on plutonium in the Russian plutonium disposition program. We compared three SBS-60 units of two different designs with three commonly used commercial US data acquisition systems by making measurements with three different HPGe detector systems. The measurements were performed to test if the gamma-ray spectral data of plutonium samples from the SBS-60 was suitable for analysis for the isotopic composition of plutonium using the Los Alamos FRAM isotopic analysis software. Each detector fed its signal to two data acquisition systems, one SBS-60 and one commercial US system. The data from the two systems were analyzed by FRAM and compared. In addition, we characterized the throughput, resolution, and stability of the SBS-60 data acquisition system in comparison with the commercial US systems. This report presents detailed results of all the tests performed.

  17. Resolved star formation on sub-galactic scales in a merger at z = 1.7

    SciTech Connect (OSTI)

    Whitaker, Katherine E.; Rigby, Jane R.; Teng, Stacy H.; Brammer, Gabriel B.; Gladders, Michael D.; Sharon, Keren; Wuyts, Eva

    2014-08-01

    We present a detailed analysis of Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) G141 grism spectroscopy for seven star-forming regions of the highly magnified lensed starburst galaxy RCSGA 032727-132609 at z = 1.704. We measure the spatial variations of the extinction in RCS0327 through the observed H?/H? emission line ratios, finding a constant average extinction of E(B V){sub gas} = 0.40 0.07. We infer that the star formation is enhanced as a result of an ongoing interaction, with measured star formation rates derived from demagnified, extinction-corrected H? line fluxes for the individual star-forming clumps falling >1-2 dex above the star formation sequence. When combining the HST/WFC3 [O III] ?5007/H? emission line ratio measurements with [N II]/H? line ratios from Wuyts et al., we find that the majority of the individual star-forming regions fall along the local 'normal' abundance sequence. With the first detections of the He I ?5876 and He II ?4686 recombination lines in a distant galaxy, we probe the massive-star content of the star-forming regions in RCS0327. The majority of the star-forming regions have a He I ?5876 to H? ratio consistent with the saturated maximum value, which is only possible if they still contain hot O-stars. Two regions have lower ratios, implying that their last burst of new star formation ended ?5 Myr ago. Together, the He I ?5876 and He II ?4686 to H? line ratios provide indirect evidence for the order in which star formation is stopping in individual star-forming knots of this high-redshift merger. We place the spatial variations of the extinction, star formation rate and ionization conditions in the context of the star formation history of RCS0327.

  18. Luminous and variable stars in M31 and M33. II. Luminous blue variables, candidate LBVs, Fe II emission line stars, and other supergiants

    SciTech Connect (OSTI)

    Humphreys, Roberta M.; Davidson, Kris; Weis, Kerstin; Bomans, D. J.; Burggraf, Birgitta E-mail: kweis@astro.rub.de

    2014-07-20

    An increasing number of non-terminal eruptions are being found in the numerous surveys for optical transients. Very little is known about these giant eruptions, their progenitors and their evolutionary state. A greatly improved census of the likely progenitor class, including the most luminous evolved stars, the luminous blue variables (LBVs), and the warm and cool hypergiants is now needed for a complete picture of the final pre-supernova stages of very massive stars. We have begun a survey of the evolved and unstable luminous star populations in several nearby resolved galaxies. In this second paper on M31 and M33, we review the spectral characteristics, spectral energy distributions, circumstellar ejecta, and evidence for mass loss for 82 luminous and variable stars. We show that many of these stars have warm circumstellar dust including several of the Fe II emission line stars, but conclude that the confirmed LBVs in M31 and M33 do not. The confirmed LBVs have relatively low wind speeds even in their hot, quiescent or visual minimum state compared to the B-type supergiants and Of/WN stars which they spectroscopically resemble. The nature of the Fe II emission line stars and their relation to the LBV state remains uncertain, but some have properties in common with the warm hypergiants and the sgB[e] stars. Several individual stars are discussed in detail. We identify three possible candidate LBVs and three additional post-red supergiant candidates. We suggest that M33-013406.63 (UIT301,B416) is not an LBV/S Dor variable, but is a very luminous late O-type supergiant and one of the most luminous stars or pair of stars in M33.

  19. DB-6 Precedent Transactions.xlsx

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

    Aug-11 Wind Energy Transmission Texas CREZ Rate Recovery Debt Mitsubishi UFJ, Deutsche Bank 500,000,000 Nov-11 Lone Star CREZ Rate Recovery Debt Mitsubishi UFJ, Mizuho, Credit ...

  20. Whole-House Systems Approach | Department of Energy

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

    Design Design for Efficiency Whole-House Systems Approach Whole-House Systems Approach The whole-house systems approach used to design this ultra-efficient home at Lone Star ...

  1. Palm Beach County, Florida: Energy Resources | Open Energy Information

    Open Energy Info (EERE)

    Power and Light Company Hydro Alternative Energy Kitson Partners LPG Electrical, Inc Lone Star Transmission LLC NextEra Energy Resources formerly FPL Energy LLC Power Tree Corp RAM...

  2. Florida's 22nd congressional district: Energy Resources | Open...

    Open Energy Info (EERE)

    Energy 5 0 Energy 5 0 LLC Enerize Corp Florida Power and Light Company Hydro Alternative Energy Kitson Partners Lone Star Transmission LLC NanoEner Technologies NextEra Energy...

  3. Y-12 now a DOE-VPP Star site | Y-12 National Security Complex

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

    now a DOE-VPP Star ... Y-12 now a DOE-VPP Star site Posted: June 6, 2012 - 2:00pm B&W Y-12 Senior Vice President and Deputy General Manager of Operations Bill Klemm (center) and Atomic Trades and Labor Council President Steve Jones (right) raise the DOE-VPP Star flag as Dan Hoag, NNSA acting site manager, looks on. The Y-12 National Security Complex now flies the VPP Star flag after a ceremony held Tuesday morning, June 5. The flag signifies Y-12's recent achievement of DOE-VPP Star status,

  4. THE HOT R CORONAE BOREALIS STAR DY CENTAURI IS A BINARY

    SciTech Connect (OSTI)

    Kameswara Rao, N.; Lambert, David L.; McArthur, Barbara; Garcia-Hernandez, D. A.; Woolf, Vincent M. E-mail: dll@astro.as.utexas.edu

    2012-11-20

    The remarkable hot R Coronae Borealis (RCB) star DY Cen is revealed to be the first and only binary system to be found among the RCB stars and their likely relatives, including the extreme helium stars and the hydrogen-deficient carbon stars. Radial velocity determinations from 1982 to 2010 have shown that DY Cen is a single-lined spectroscopic binary in an eccentric orbit with a period of 39.67 days. It is also one of the hottest and most H-rich member of the class of RCB stars. The system may have evolved from a common envelope to its current form.

  5. KitchenAid: ENERGY STAR Referral (KSRG25FVMS*) | Department of Energy

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

    KSRG25FVMS*) KitchenAid: ENERGY STAR Referral (KSRG25FVMS*) September 13, 2011 DOE referred the matter of Whirlpool's KitchenAid refrigerator model KSRG25FVMS* to the U.S. Environmental Protection Agency, brand manager of the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. KitchenAid: ENERGY STAR Referral (KSRG25FVMS*) (58.79 KB) More Documents & Publications KitchenAid: ENERGY STAR Referral (KSRS25RV*) Maytag:

  6. KitchenAid: ENERGY STAR Referral (KSRS25RV*) | Department of Energy

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

    KSRS25RV*) KitchenAid: ENERGY STAR Referral (KSRS25RV*) September 6, 2011 DOE referred the matter of Whirlpool's KitchenAid refrigerator model KSRS25RV* to the U.S. Environmental Protection Agency, brand manager of the ENERGY STAR Program, for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification. KitchenAid: ENERGY STAR Referral (KSRS25RV*) (35.25 KB) More Documents & Publications KitchenAid: ENERGY STAR Referral (KSRG25FVMS*) Whirlpool:

  7. A NEAR-INFRARED SURVEY OF THE INNER GALACTIC PLANE FOR WOLF-RAYET STARS. II. GOING FAINTER: 71 MORE NEW W-R STARS

    SciTech Connect (OSTI)

    Shara, Michael M.; Faherty, Jacqueline K.; Zurek, David; Moffat, Anthony F. J.; Doyon, Rene; Gerke, Jill; Artigau, Etienne; Drissen, Laurent E-mail: jfaherty@amnh.org E-mail: moffat@astro.umontreal.ca E-mail: gerke@astronomy.ohio-state.edu E-mail: ldrissen@phy.ulaval.ca

    2012-06-15

    We are continuing a J, K and narrowband imaging survey of 300 deg{sup 2} of the plane of the Galaxy, searching for new Wolf-Rayet (W-R) stars. Our survey spans 150 Degree-Sign in Galactic longitude and reaches 1 Degree-Sign above and below the Galactic plane. The survey has a useful limiting magnitude of K = 15 over most of the observed Galactic plane, and K = 14 (due to severe crowding) within a few degrees of the Galactic center. Thousands of emission-line candidates have been detected. In spectrographic follow-ups of 146 relatively bright W-R star candidates, we have re-examined 11 previously known WC and WN stars and discovered 71 new W-R stars, 17 of type WN and 54 of type WC. Our latest image analysis pipeline now picks out W-R stars with a 57% success rate. Star subtype assignments have been confirmed with the K-band spectra and distances approximated using the method of spectroscopic parallax. Some of the new W-R stars are among the most distant known in our Galaxy. The distribution of these new W-R stars is beginning to trace the locations of massive stars along the distant spiral arms of the Milky Way.

  8. The identification of RR Lyrae and δ Scutti stars from variable galaxy evolution explorer ultraviolet sources

    SciTech Connect (OSTI)

    Kinman, T. D.; Brown, Warren R.

    2014-12-01

    We identify the RR Lyrae and δ Scuti stars in three catalogs of Galaxy Evolution Explorer (GALEX) variable sources. The NUV amplitude of RR Lyrae stars is about twice that in V, so we find a larger percentage of low-amplitude variables than catalogs such as Abbas et al. Interestingly, the (NUV – V){sub 0} color is sensitive to metallicity and can be used to distinguish between variables of the same period but differing [Fe/H]. This color is also more sensitive to T {sub eff} than optical colors and can be used to identify the red edge of the instability gap. We find 8 δ Scuti stars, 17 RRc stars, 1 RRd star, and 84 RRab stars in the GALEX variable catalogs of Welsh et al. and Wheatley et al. We also classify 6 δ Scuti stars, 5 RRc stars, and 18 RRab stars among the 55 variable GALEX sources identified as 'stars' or RR Lyrae stars in the catalog of Gezari et al. We provide ephemerides and light curves for the 26 variables that were not previously known.

  9. Precise rotation rates for five slowly rotating A stars

    SciTech Connect (OSTI)

    Gray, David F.

    2014-04-01

    Projected rotation rates of five early A-type slowly rotating stars are measured spectroscopically to a precision of 0.2 km s{sup 1}. A detailed Fourier analysis is done, as well as a comparison of profiles directly. Macroturbulence is needed in addition to rotation to reproduce the profile shapes. An upper limit of ?2 km s{sup 1} is placed on the microturbulence dispersion. Small unexplained differences between the models and the observations are seen in the sidelobe structure of the transforms. The v sin i results are: ? Dra, 26.2; ? Leo, 22.5; ? CMa A, 16.7; ? Gem A, 10.7; o Peg, 6.0 km s{sup 1}. These stars are suitable as standards for measuring rotation using less fundamental methods.

  10. The Safety and Tritium Applied Research (STAR) Facility: Status-2004

    SciTech Connect (OSTI)

    Anderl, R.A.; Longhurst, G.R.; Pawelko, R.J.; Sharpe, J.P.; Schuetz, S.T.; Petti, D.A.

    2005-07-15

    The Safety and Tritium Applied Research (STAR) Facility, a US DOE National User Facility at the Idaho National Engineering and Environmental Laboratory (INEEL), comprises capabilities and infrastructure to support both tritium and non-tritium research activities important to the development of safe and environmentally friendly fusion energy. Research thrusts include (1) interactions of tritium and deuterium with plasma-facing-component (PFC) materials, (2) fusion safety issues [PFC material chemical reactivity and dust/debris generation, activation product mobilization, tritium behavior in fusion systems], and (3) molten salts and fusion liquids for tritium breeder and coolant applications. This paper updates the status of STAR and the capabilities for ongoing research activities, with an emphasis on the development, testing and integration of the infrastructure to support tritium research activities. Key elements of this infrastructure include a tritium storage and assay system, a tritium cleanup system to process glovebox and experiment tritiated effluent gases, and facility tritium monitoring systems.

  11. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    9 Total Lighting Shipments (Millions) and ENERGY STAR Market Share 1998 221.5 1% - N/A 1999 213.2 1% 1,328 0% 2000 210.8 2% 1,026 1% 2001 196.7 2% 1,088 5% 2002 220.5 1% 1,076 4% 2003 225.0 3% 1,161 5% 2004 237.8 2% 1,389 6% 2005 247.4 3% 1,343 7% 2006 248.6 4% 1,302 11% 2007 217.9 6% 1,518 21% 2008 194.6 10% 1,230 22% 2009 174.7 6% 1,681 15% 2010 182.4 15% 1,658 20% Note(s): Source(s): Medium Screw- Light Fixtures Base Lamps N/A = Not Applicable. ENERGY STAR specification did not exist. LBNL,

  12. Collision--induced absorption in dense atmospheres of cool stars

    SciTech Connect (OSTI)

    Borysow, Aleksandra; Joergensen, Uffe Graae

    1999-04-01

    In the atmosphere of the Sun the major interaction between the matter and the radiation is through light absorption by ions (predominantly the negative ion of hydrogen atoms), neutral atoms and a small amount of polar molecules. The majority of stars in the universe are, however, cooler and denser than our Sun, and for a large fraction of these, the above absorption processes are very weak. Here, collision-induced absorption (CIA) becomes the dominant opacity source. The radiation is absorbed during very short mutual passages ('collisions') of two non-polar molecules (and/or atoms), while their electric charge distributions are temporarily distorted which gives rise to a transient dipole moment. We present here a review of the present-day knowledge about the impact of collision-induced absorption processes on the structure and the spectrum of such stars.

  13. Massive Stars in Colliding Wind Systems: the GLAST Perspective

    SciTech Connect (OSTI)

    Reimer, Anita; Reimer, Olaf; /Stanford U., HEPL /KIPAC, Menlo Park

    2011-11-29

    Colliding winds of massive stars in binary systems are considered as candidate sites of high-energy non-thermal photon emission. They are already among the suggested counterparts for a few individual unidentified EGRET sources, but may constitute a detectable source population for the GLAST observatory. The present work investigates such population study of massive colliding wind systems at high-energy gamma-rays. Based on the recent detailed model (Reimer et al. 2006) for non-thermal photon production in prime candidate systems, we unveil the expected characteristics of this source class in the observables accessible at LAT energies. Combining the broadband emission model with the presently cataloged distribution of such systems and their individual parameters allows us to conclude on the expected maximum number of LAT-detections among massive stars in colliding wind binary systems.

  14. LIMB-DARKENED RADIATION-DRIVEN WINDS FROM MASSIVE STARS

    SciTech Connect (OSTI)

    Cure, M.; Cidale, L.

    2012-10-01

    We calculated the influence of the limb-darkened finite-disk correction factor in the theory of radiation-driven winds from massive stars. We solved the one-dimensional m-CAK hydrodynamical equation of rotating radiation-driven winds for all three known solutions, i.e., fast, {Omega}-slow, and {delta}-slow. We found that for the fast solution, the mass-loss rate is increased by a factor of {approx}10%, while the terminal velocity is reduced about 10%, when compared with the solution using a finite-disk correction factor from a uniformly bright star. For the other two slow solutions, the changes are almost negligible. Although we found that the limb darkening has no effects on the wind-momentum-luminosity relationship, it would affect the calculation of synthetic line profiles and the derivation of accurate wind parameters.

  15. ENHANCED ACCRETION RATES OF STARS ON SUPERMASSIVE BLACK HOLES BY STAR-DISK INTERACTIONS IN GALACTIC NUCLEI

    SciTech Connect (OSTI)

    Just, Andreas; Yurin, Denis; Makukov, Maxim; Berczik, Peter; Omarov, Chingis; Spurzem, Rainer; Vilkoviskij, Emmanuil Y.

    2012-10-10

    We investigate the dynamical interaction of a central star cluster surrounding a supermassive black hole (SMBH) and a central accretion disk (AD). The dissipative force acting on stars in the disk leads to an enhanced mass flow toward the SMBH and to an asymmetry in the phase space distribution due to the rotating AD. The AD is considered as a stationary Keplerian rotating disk, which is vertically extended in order to employ a fully self-consistent treatment of stellar dynamics including the dissipative force originating from star-gas ram pressure effects. The stellar system is treated with a direct high-accuracy N-body integration code. A star-by-star representation, desirable in N-body simulations, cannot be extended to real particle numbers yet. Hence, we carefully discuss the scaling behavior of our model with regard to particle number and tidal accretion radius. The main idea is to find a family of models for which the ratio of two-body relaxation time and dissipation time (for kinetic energy of stellar orbits) is constant, which then allows us to extrapolate our results to real parameters of galactic nuclei. Our model is derived from basic physical principles and as such it provides insight into the role of physical processes in galactic nuclei, but it should be regarded as a first step toward more realistic and more comprehensive simulations. Nevertheless, the following conclusions appear to be robust: the star accretion rate onto the AD and subsequently onto the SMBH is enhanced by a significant factor compared to purely stellar dynamical systems neglecting the disk. This process leads to enhanced fueling of central disks in active galactic nuclei (AGNs) and to an enhanced rate of tidal stellar disruptions. Such disruptions may produce electromagnetic counterparts in the form of observable X-ray flares. Our models improve predictions for their rates in quiescent galactic nuclei. We do not yet model direct stellar collisions in the gravitational potential

  16. Single-flavor CSL phase in compact stars

    SciTech Connect (OSTI)

    Blaschke, David; Sandin, Fredrik; Klaehn, Thomas; Berdermann, Jens

    2008-08-29

    We suggest a scenario where the three light quark flavors are sequentially deconfined under increasing pressure in cold asymmetric nuclear matter as, e.g., in neutron stars. The basis for our analysis is a chiral quark matter model of Nambu-Jona-Lasinio (NJL) type with diquark pairing in the spin-1 single flavor (CSL), spin-0 two flavor (2SC) and three flavor (CFL) channels. We find that nucleon dissociation sets in at about the saturation density, n{sub 0}, when the down-quark Fermi sea is populated (d-quark dripline) due to the flavor asymmetry induced by {beta}-equilibrium and charge neutrality. At about 3n{sub 0} u-quarks appear and a two-flavor color superconducting (2SC) phase is formed. The s-quark Fermi sea is populated only at still higher baryon density, when the quark chemical potential is of the order of the dynamically generated strange quark mass. We construct two different hybrid equations of state (EoS) using the Dirac-Brueckner Hartree-Fock (DBHF) approach and the EoS by Shen et al. in the nuclear matter sector. The corresponding hybrid star sequences have maximum masses of, respectively, 2.1 and 2.0 M{sub {center_dot}}. Two- and three-flavor quark-matter phases exist only in gravitationally unstable hybrid star solutions in the DBHF case, while the Shen-based EoS produce stable configurations with a 2SC phase component in the core of massive stars. Nucleon dissociation due to d-quark drip at the crust-core boundary fulfills basic criteria for a deep crustal heating process which is required to explain superbusts as well as cooling of X-ray transients.

  17. WIPP contractor receives VPP Legacy of Stars Award 2013

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

    Management and Operating Contractor Recognized for Continuous Safety Performance CARLSBAD, N.M., September 20, 2013 - The U.S. Department of Energy (DOE) recognized Nuclear Waste Partnership LLC (NWP), the Waste Isolation Pilot Plant (WIPP) management and operating (M&O) contractor, with the Voluntary Protection Program (VPP) Legacy of Stars Award in latter August 2013. "Safety is central to everything we do, and achieving this elite designation validates our work and the safety-focused

  18. Home Performance with ENERGY STAR Webinar (text version) | Department of

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

    Energy Webinar (text version) Home Performance with ENERGY STAR Webinar (text version) This Better Buildings webinar took place on August 5, 2010. Webinar transcript (150.29 KB) More Documents & Publications May 21, 2011 - Getting Useful Real Time Feedback About Your Program Webinar (text version) February 13, 2013 Webinar: Preliminary Process and Market Evaluation - Better Buildings Neighborhood Program Webcast April 27, 2011 - How to Work with the Media Webinar (text version)

  19. DYNAMO ACTION AND MAGNETIC CYCLES IN F-TYPE STARS

    SciTech Connect (OSTI)

    Augustson, Kyle C.; Toomre, Juri; Brun, Allan Sacha

    2013-11-10

    Magnetic activity and differential rotation are commonly observed features on main-sequence F-type stars. We seek to make contact with such observations and to provide a self-consistent picture of how differential rotation and magnetic fields arise in the interiors of these stars. The three-dimensional magnetohydrodynamic anelastic spherical harmonic code is employed to simulate global-scale convection and dynamo processes in a 1.2 M{sub ☉} F-type star at two rotation rates. The simulations are carried out in spherical shells that encompass most of the convection zone and a portion of the stably stratified radiative zone below it, allowing us to explore the effects a stable zone has upon the morphology of the global-scale magnetic fields. We find that dynamo action with a high degree of time variation occurs in the star rotating more rapidly at 20 Ω{sub ☉}, with the polarity of the mean field reversing on a timescale of about 1600 days. Between reversals, the magnetic energy rises and falls with a fairly regular period, with three magnetic energy cycles required to complete a reversal. The magnetic energy cycles and polarity reversals arise due to a linking of the polar-slip instability in the stable region and dynamo action present in the convection zone. For the more slowly rotating case (10 Ω{sub ☉}), persistent wreaths of magnetism are established and maintained by dynamo action. Compared to their hydrodynamic progenitors, the dynamo states here involve a marked reduction in the exhibited latitudinal differential rotation, which also vary during the course of a cycle.

  20. Determinants of Household Use of Selected Energy Star Appliances - Energy

    Gasoline and Diesel Fuel Update (EIA)

    Information Administration Determinants of Household Use of Selected Energy Star Appliances Release date: May 25, 2016 Introduction According to the 2009 Residential Energy Consumption Survey (RECS), household appliances1accounted for 35% of U.S. household energy consumption, up from 24% in 1993. Thus, improvements in the energy performance of residential appliances as well as increases in the use of more efficient appliances can be effective in reducing household energy consumption and

  1. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    5 Specification Dates for ENERGY STAR-Labeled Consumer Electronics and Office Equipment Labeled (Covered) Product Dates of updated specification Computers 1992 1995, 1999, 2000, 2007, 2009 Displays 1992 1995, 1998, 1999, 2005, 2006, 2009 Printers (1) 1993 1995, 2000, 2001, 2007, 2009 Fax Machines (1) 1995 1995, 2000, 2001, 2007, 2009 Copiers (1) 1995 1997, 1999, 2007, 2009 Scanners (1) 1997 2007, 2009 Multi-Function Devices (1) 1997 1999, 2007, 2009 Televisions 1998 2002, 2004, 2005, 2008, 2010,

  2. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    6 Specification Dates for ENERGY STAR-Labeled HVAC and Residential Appliances Heating and Cooling Equipment Dates of updated specification Central AC 1995 2002, 2006, 2009 Air-Source Heat Pumps 1995 2002, 2006, 2009 Oil Furnaces 1995 2006, 2008, 2012, 2013 Gas Furnaces 1995 2006, 2008, 2012, 2013 Programable Thermostats - Gas Boilers 1996 2002 Oil Boilers 1996 2002 Gas-Fired Heat Pumps - Geothermal Heat Pumps 2001 2009, 2011, 2012 Ventilating Fans 2001 2003, 2009, 2012 Ceiling Fans 2001 2003,

  3. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    7 Specification Dates for ENERGY STAR-Labeled Commercial and Miscellaneous Products Commercial Products Dates of updated specification Commercial Refrigerators and Freezers 2001 2009/2010 Hot Food Holding Cabinets 2003 2011 Commercial Steam Cookers 2003 - Commercial Fryers 2003 2011 Cold Beverage Vending Machines 2004 2006, 2007 Solid State Lighting 2008 2009 Commercial Dishwashers 2007 - Commercial Icemakers 2008 - Commercial Griddles 2009 2011 Commercial Ovens 2009 - Enterprise Servers 2009 -

  4. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    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

  5. DeepStar evaluation of subsea trees and manifold concepts

    SciTech Connect (OSTI)

    Kirkland, K.G.; Richardson, E.M.; Hey, C.

    1996-12-31

    This paper reviews the results of a study performed for the DeepStar Project, CTR A802-2, Concept Study and Investigation of Key Areas of Interest for Subsea Systems in Deepwater. The report documents the results of a study of subsea manifold systems as applied to the deepwater Gulf of Mexico. Of particular interest is the development of a range of system level philosophies based on recent and ongoing experience from the operators and vendors.

  6. Idaho National Engineering and Environmental Laboratory Awarded VPP Gold Star

    Broader source: Energy.gov [DOE]

    Our journey to safety excellence began some six (6) years ago. The task seemed ominous with 6000 plus employees ranging from administrative assistants and craftsman to research scientists and engineers. Another challenge was the geographic dispersion of work areas being as much as 50 miles apart. A core group of employees caught the vision and knew that it could be done, and it is that perseverance that has lead the INEEL to the DOE-VPP Gold Star.

  7. UPPER BOUND ON THE FIRST STAR FORMATION HISTORY

    SciTech Connect (OSTI)

    Inoue, Yoshiyuki; Madejski, Grzegorz M.; Tanaka, Yasuyuki T.; Domnguez, Alberto

    2014-02-01

    Our understanding of the nature of the extragalactic background light (EBL) has improved with the recent development of gamma-ray observation techniques. An open subject in the context of the EBL is the reionization epoch, which is an important probe of the formation history of first stars, the so-called Population III (Pop III) stars. Although the mechanisms for the formation of PopIII stars are rather well understood on theoretical grounds, their formation history is still veiled in mystery because of their faintness. To shed light on this matter, we study jointly the gamma-ray opacity of distant objects and the reionization constraints from studies of intergalactic gas. By combining these studies, we obtain a sensitive upper bound on the PopIII star formation rate density of ?-dot {sub ?}(z)<0.01[(1+z)/(1+7.0)]{sup 3.4}(f{sub esc}/0.2){sup ?1}(C/3.0)M{sub ?}yr{sup ?1}Mpc{sup ?3} at z ? 7, where f {sub esc} and C are the escape fraction of ionizing photons from galaxies and the clumping factor of the intergalactic hydrogen gas. This limit is a ?10times tighter constraint compared with previous studies that take into account gamma-ray opacity constraints only. Even if we do not include the current gamma-ray constraints, the results do not change. This is because the detected gamma-ray sources are still at z ? 4.35 where the reionization has already finished.

  8. CANDIDATE PLANETS IN THE HABITABLE ZONES OF KEPLER STARS

    SciTech Connect (OSTI)

    Gaidos, Eric

    2013-06-20

    A key goal of the Kepler mission is the discovery of Earth-size transiting planets in ''habitable zones'' where stellar irradiance maintains a temperate climate on an Earth-like planet. Robust estimates of planet radius and irradiance require accurate stellar parameters, but most Kepler systems are faint, making spectroscopy difficult and prioritization of targets desirable. The parameters of 2035 host stars were estimated by Bayesian analysis and the probabilities p{sub HZ} that 2738 candidate or confirmed planets orbit in the habitable zone were calculated. Dartmouth Stellar Evolution Program models were compared to photometry from the Kepler Input Catalog, priors for stellar mass, age, metallicity and distance, and planet transit duration. The analysis yielded probability density functions for calculating confidence intervals of planet radius and stellar irradiance, as well as p{sub HZ}. Sixty-two planets have p{sub HZ} > 0.5 and a most probable stellar irradiance within habitable zone limits. Fourteen of these have radii less than twice the Earth; the objects most resembling Earth in terms of radius and irradiance are KOIs 2626.01 and 3010.01, which orbit late K/M-type dwarf stars. The fraction of Kepler dwarf stars with Earth-size planets in the habitable zone ({eta}{sub Circled-Plus }) is 0.46, with a 95% confidence interval of 0.31-0.64. Parallaxes from the Gaia mission will reduce uncertainties by more than a factor of five and permit definitive assignments of transiting planets to the habitable zones of Kepler stars.

  9. On the capture of dark matter by neutron stars

    SciTech Connect (OSTI)

    Güver, Tolga; Erkoca, Arif Emre; Sarcevic, Ina; Reno, Mary Hall E-mail: aeerkoca@gmail.com E-mail: ina@physics.arizona.edu

    2014-05-01

    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 section with the nucleons as well as dark matter self-interaction cross section, based on the observation of old neutron stars. We show that for a dark matter density of 10{sup 3} GeV/cm{sup 3}and dark matter mass m{sub χ} ∼< 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{sub χ} ∼ 10 GeV when the dark matter interaction cross section with the nucleons ranges from σ{sub χn} ∼ 10{sup −52} cm{sup 2} to σ{sub χn} ∼ 10{sup −57} cm{sup 2}, the dark matter self-interaction cross section limit is σ{sub χχ} ∼< 10{sup −33} cm{sup 2}, which is about ten orders of magnitude stronger than the Bullet Cluster limit.

  10. THE ROLE OF THE MAGNETOROTATIONAL INSTABILITY IN MASSIVE STARS

    SciTech Connect (OSTI)

    Wheeler, J. Craig; Kagan, Daniel; Chatzopoulos, Emmanouil

    2015-01-20

    The magnetorotational instability (MRI) is key to physics in accretion disks and is widely considered to play some role in massive star core collapse. Models of rotating massive stars naturally develop very strong shear at composition boundaries, a necessary condition for MRI instability, and the MRI is subject to triply diffusive destabilizing effects in radiative regions. We have used the MESA stellar evolution code to compute magnetic effects due to the Spruit-Tayler (ST) mechanism and the MRI, separately and together, in a sample of massive star models. We find that the MRI can be active in the later stages of massive star evolution, leading to mixing effects that are not captured in models that neglect the MRI. The MRI and related magnetorotational effects can move models of given zero-age main sequence mass across ''boundaries'' from degenerate CO cores to degenerate O/Ne/Mg cores and from degenerate O/Ne/Mg cores to iron cores, thus affecting the final evolution and the physics of core collapse. The MRI acting alone can slow the rotation of the inner core in general agreement with the observed ''initial'' rotation rates of pulsars. The MRI analysis suggests that localized fields ?10{sup 12} G may exist at the boundary of the iron core. With both the ST and MRI mechanisms active in the 20 M {sub ?} model, we find that the helium shell mixes entirely out into the envelope. Enhanced mixing could yield a population of yellow or even blue supergiant supernova progenitors that would not be standard SN IIP.

  11. The mass-radius relationship of massive compact stars

    SciTech Connect (OSTI)

    Chowdhury, Partha Roy

    2015-02-24

    The properties of pure hadronic and hybrid compact stars are reviewed using nuclear equation of state (EoS) for β-equilibrated neutron star (NS) matter obtained using a density-dependent M3Y (DDM3Y) effective nucleon-nucleon interaction. Depending on the model, the energy density of quark matter can be lower than that of this nuclear EoS at higher densities, implying the possibility of transition to quark matter inside the core and the transition density depends on the particular quark matter model used. The recent observations of the binary millisecond pulsar J1614–2230 by P.B. Demorest et al. [1] and PSR J0348+0432 by J. Antoniadis et al. [2] suggest that the masses lie within 1.97 ± 0.04 M{sub ⊙} and 2.01 ± 0.04 M{sub ⊙}, respectively, where M{sub ⊙} is the solar mass. In conformity with recent observations, a pure nucleonic EoS determines that the maximum mass of NS rotating with frequency ν∼ 667 Hz below r-mode instability is ∼ 1.95 M{sub ⊙} with radius ∼ 10 km. Compact stars with quark cores rotating with same frequency have the maximum mass of ∼ 1.72 M{sub ⊙} turns out to be lower than the observed masses.

  12. THE NEARBY, YOUNG, ISOLATED, DUSTY STAR HD 166191

    SciTech Connect (OSTI)

    Schneider, Adam; Song, Inseok; Hufford, Tara; Melis, Carl; Zuckerman, B.; Bessell, Mike; Hinkley, Sasha E-mail: song@physast.uga.edu E-mail: cmelis@ucsd.edu E-mail: bessell@mso.anu.edu.au

    2013-11-01

    We report an in-depth study of the F8-type star HD 166191, identified in an ongoing survey for stars exhibiting infrared emission above their expected photospheres in the Wide-field Infrared Survey Explorer all-sky catalog. The fractional IR luminosity measured from 3.5 to 70 μm is exceptionally high (L{sub IR}/L{sub bol} ∼ 10%). Near-diffraction-limited imaging observations with the T-ReCS Si filter set on the Gemini South telescope and adaptive optics imaging with the NIRC2 Lp filter on the Keck II telescope confirmed that the excess emission coincides with the star. Si-band images show a strong solid-state emission feature at ∼10 μm. Theoretical evolutionary isochrones and optical spectroscopic observations indicate a stellar age in the range 10-100 Myr. The large dust mass seen in HD 166191's terrestrial planet zone is indicative of a recent collision between planetary embryos or massive ongoing collisional grinding associated with planet building.

  13. The swift UVOT stars survey. I. Methods and test clusters

    SciTech Connect (OSTI)

    Siegel, Michael H.; Porterfield, Blair L.; Linevsky, Jacquelyn S.; Bond, Howard E.; Hoversten, Erik A.; Berrier, Joshua L.; Gronwall, Caryl A.; Holland, Stephen T.; Breeveld, Alice A.; Brown, Peter J. E-mail: blp14@psu.edu E-mail: caryl@astro.psu.edu E-mail: aab@mssl.ucl.ac.uk

    2014-12-01

    We describe the motivations and background of a large survey of nearby stellar populations using the Ultraviolet Optical Telescope (UVOT) on board the Swift Gamma-Ray Burst Mission. UVOT, with its wide field, near-UV sensitivity, and 2.″3 spatial resolution, is uniquely suited to studying nearby stellar populations and providing insight into the near-UV properties of hot stars and the contribution of those stars to the integrated light of more distant stellar populations. We review the state of UV stellar photometry, outline the survey, and address problems specific to wide- and crowded-field UVOT photometry. We present color–magnitude diagrams of the nearby open clusters M67, NGC 188, and NGC 2539, and the globular cluster M79. We demonstrate that UVOT can easily discern the young- and intermediate-age main sequences, blue stragglers, and hot white dwarfs, producing results consistent with previous studies. We also find that it characterizes the blue horizontal branch of M79 and easily identifies a known post-asymptotic giant branch star.

  14. Calendar Year 2007 Program Benefits for ENERGY STAR Labeled Products

    SciTech Connect (OSTI)

    Sanchez, Marla Christine; Homan, Gregory; Brown, Richard

    2008-10-31

    ENERGY STAR is a voluntary energy efficiency-labeling program operated jointly by the United States Department of Energy and the United States Environmental Protection Agency (US EPA). Since the program inception in 1992, ENERGY STAR has become a leading international brand for energy efficient products. ENERGY STAR's central role in the development of regional, national, and international energy programs necessitates an open process whereby its program achievements to date as well as projected future savings are shared with committed stakeholders. Through 2007, the program saved 7.1 Quads of primary energy and avoided 128 MtC equivalent. The forecast shows that the program is expected to save 21.2 Quads of primary energy and avoid 375 MtC equivalent over the period 2008-2015. The sensitivity analysis bounds the best estimate of carbon avoided between 84 MtC and 172 MtC (1993 to 2007) and between 243 MtC and 519 MtC (2008 to 2015).

  15. Star formation bimodality in early-type galaxies

    SciTech Connect (OSTI)

    Amblard, A.; Riguccini, L.; Temi, P.; Im, S.; Fanelli, M.; Serra, P.

    2014-03-10

    We compute the properties of a sample of 221 local, early-type galaxies with a spectral energy distribution (SED) modeling software, CIGALEMC. Concentrating on the star-forming (SF) activity and dust contents, we derive parameters such as the specific star formation rate (sSFR), the dust luminosity, dust mass, and temperature. In our sample, 52% is composed of elliptical (E) galaxies and 48% of lenticular (S0) galaxies. We find a larger proportion of S0 galaxies among galaxies with a large sSFR and large specific dust emission. The stronger activity of S0 galaxies is confirmed by larger dust masses. We investigate the relative proportion of active galactic nuclei (AGNs) and SF galaxies in our sample using spectroscopic Sloan Digital Sky Survey data and near-infrared selection techniques, and find a larger proportion of AGN-dominated galaxies in the S0 sample than the E one. This could corroborate a scenario where blue galaxies evolve into red ellipticals by passing through an S0 AGN active period while quenching its star formation. Finally, we find a good agreement comparing our estimates with color indicators.

  16. Signatures of a companion star in type Ia supernovae

    SciTech Connect (OSTI)

    Maeda, Keiichi; Kutsuna, Masamichi; Shigeyama, Toshikazu

    2014-10-10

    Although type Ia supernovae (SNe Ia) have been used as precise cosmological distance indicators, their progenitor systems remain unresolved. One of the key questions is whether there is a nondegenerate companion star at the time of a thermonuclear explosion of a white dwarf. In this paper, we investigate whether an interaction between the SN ejecta and the companion star may result in observable footprints around the maximum brightness and thereafter, by performing multidimensional radiation transfer simulations based on hydrodynamic simulations of the interaction. We find that such systems result in variations in various observational characteristics due to different viewing directions, and the predicted behaviors (redder and fainter for the companion direction) are the opposite of what were suggested by the previous study. The variations are generally modest and within observed scatters. However, the model predicts trends between some observables different from those observationally derived, so a large sample of SNe Ia with small calibration errors may be used to constrain the existence of such a companion star. The variations in different colors in optical band passes can be mimicked by external extinctions, so such an effect could be a source of scatter in the peak luminosity and derived distance. After the peak, hydrogen-rich materials expelled from the companion will manifest themselves in hydrogen lines, but Hα is extremely difficult to identify. Alternatively, we find that P{sub β} in postmaximum near-infrared spectra can potentially provide a powerful diagnostic.

  17. STAR CLUSTER DISRUPTION IN THE STARBURST GALAXY MESSIER 82

    SciTech Connect (OSTI)

    Li, Shuo; Li, Chengyuan; De Grijs, Richard; Anders, Peter

    2015-01-01

    Using high-resolution, multiple-passband Hubble Space Telescope images spanning the entire optical/near-infrared wavelength range, we obtained a statistically complete U-band-selected sample of 846 extended star clusters across the disk of the nearby starburst galaxy M82. Based on a careful analysis of the clusters' spectral energy distributions, we determined their galaxy-wide age and mass distributions. The M82 clusters exhibit three clear peaks in their age distribution, thus defining relatively young, log (t yr{sup 1}) ? 7.5, intermediate-age, log (t yr{sup 1}) in [7.5, 8.5], and old samples, log (t yr{sup 1}) ? 8.5. Comparison of the completeness-corrected mass distributions offers a firm handle on the galaxy's star cluster disruption history. The most massive star clusters in the young and old samples are (almost) all concentrated in the most densely populated central region, while the intermediate-age sample's most massive clusters are more spatially dispersed, which may reflect the distribution of the highest-density gas throughout the galaxy's evolutionary history, combined with the solid-body nature of the galaxy's central region.

  18. THE STRUCTURAL EVOLUTION OF FORMING AND EARLY STAGE STAR CLUSTERS

    SciTech Connect (OSTI)

    Jaehnig, Karl O.; Da Rio, Nicola; Tan, Jonathan C. E-mail: ndario@ufl.edu

    2015-01-10

    We study the degree of angular substructure in the stellar position distribution of young members of Galactic star-forming regions, looking for correlations with distance from cluster center, surface number density of stars, and local dynamical age. To this end we adopt the catalog of members in 18 young (?1-3Myr) clusters from the Massive Young Star-Forming Complex Study in Infrared and X-ray Survey and the statistical analysis of the angular dispersion parameter, ?{sub ADP,} {sub N}. We find statistically significant correlation between ?{sub ADP,} {sub N} and physical projected distance from the center of the clusters, with the centers appearing smoother than the outskirts, consistent with more rapid dynamical processing on local dynamical, free-fall or orbital timescales. Similarly, smoother distributions are seen in regions of higher surface density, or older dynamical ages. These results indicate that dynamical processing that erases substructure is already well-advanced in young, sometimes still-forming, clusters. Such observations of the dissipation of substructure have the potential to constrain theoretical models of the dynamical evolution of young and forming clusters.

  19. HERSCHEL AND SPITZER OBSERVATIONS OF SLOWLY ROTATING, NEARBY ISOLATED NEUTRON STARS

    SciTech Connect (OSTI)

    Posselt, B.; Pavlov, G. G.; Popov, S.; Wachter, S.

    2014-11-01

    Supernova fallback disks around neutron stars have been suspected to influence the evolution of the diverse neutron star populations. Slowly rotating neutron stars are the most promising places to find such disks. Searching for the cold and warm debris of old fallback disks, we carried out Herschel PACS (70 μm, 160 mu m) and Spitzer IRAC (3.6 μm, 4.5 μm) observations of eight slowly rotating (P ≈ 3-11 s) nearby (<1 kpc) isolated neutron stars. Herschel detected 160 μm emission (>5σ) at locations consistent with the positions of the neutron stars RX J0806.4-4123 and RX J2143.0+0654. No other significant infrared emission was detected from the eight neutron stars. We estimate probabilities of 63%, 33%, and 3% that, respectively, none, one, or both Herschel PACS 160 μm detections are unrelated excess sources due to background source confusion or an interstellar cirrus. If the 160 μm emission is indeed related to cold (10-22 K) dust around the neutron stars, this dust is absorbing and re-emitting ∼10% to ∼20% of the neutron stars' X-rays. Such high efficiencies would be at least three orders of magnitude larger than the efficiencies of debris disks around nondegenerate stars. While thin dusty disks around the neutron stars can be excluded as counterparts of the 160 μm emission, dusty asteroid belts constitute a viable option.

  20. Detection of stars within ?0.8 in of Kepler objects of interest

    SciTech Connect (OSTI)

    Kolbl, Rea; Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew W.

    2015-01-01

    We present an algorithm to search for the faint spectrum of a second star mixed with the spectrum of a brighter star in high resolution spectra. We model optical stellar spectra as the sum of two input spectra drawn from a vast library of stars throughout the H-R diagram. From typical spectra having a resolution of R = 60,000, we are able to detect companions as faint as 1% relative to the primary star in approximately the V and R bandpasses of photometry. We are also able to find evidence for triple and quadruple systems, given that any additional companions are sufficiently bright. The precise threshold percentage depends on the signal-to-noise of the spectrum and the properties of the two stars. For cases of non-detection, we place a limit on the brightness of any potential companions. This algorithm is useful for detecting faint orbiting companions and background stars that are angularly close to a foreground target star. The size of the entrance slit to the spectrometer, 0.87 3 arcsec (typically), sets the angular domain within which the second star can be detected. We analyzed Keck-HIRES spectra of 1160 California Kepler Survey objects of interest (KOI) searching for the secondary spectra, with the two goals of alerting the community to two possible host stars of the transiting planet and to dilution of the light curve. We report 63 California KOI showing spectroscopic evidence of a secondary star.