National Library of Energy BETA

Sample records for difference star center

  1. 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 ...

  2. 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 ...

  3. 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 ...

  4. 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: ...

  5. 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: ...

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

    Office of Legacy Management (LM)

    0/06 Technical Report for S M Stoller Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F39137 Sampling Dates: 03/08/06 - 03/09/06 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast *

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

    Office of Legacy Management (LM)

    Quarterly Sampling, STAR Center, Largo, FL 7030-226 Accutest Job Number: F27229 Sampling Date: 10/07/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 *

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

    Office of Legacy Management (LM)

    2/04 Technical Report for S M Stoller Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F25409 Sampling Dates: 07/13/04 - 07/14/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast *

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

    Office of Legacy Management (LM)

    Quarterly Sampling, STAR Center, Largo, FL 110406202 Accutest Job Number: F33211 Sampling Dates: 07/13/05 - 07/14/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 *

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

    Office of Legacy Management (LM)

    6/04 Technical Report for S M Stoller Star Center-WWNA Monthly; Largo, FL 110406202 Accutest Job Number: F25242 Sampling Date: 07/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road *

  11. On the origin of the B-stars in the galactic center

    SciTech Connect (OSTI)

    Madigan, Ann-Marie; Pfuhl, Oliver; Gillessen, Stefan; Genzel, Reinhard; Levin, Yuri; Perets, Hagai B.

    2014-03-20

    We present a new directly observable statistic that uses sky position (x, y) and proper motion (v{sub x} , v{sub y} ) of stars near the massive black hole in the Galactic center to identify populations with high orbital eccentricities. It is most useful for stars with large orbital periods for which dynamical accelerations are difficult to determine. We apply this statistic to a data set of B-stars with a projected radii 0.''1 < p < 25'' (∼0.004-1 pc) from the massive black hole in the Galactic center. We compare the results with those from N-body simulations to distinguish between scenarios for their formation. We find that the scenarios favored by the data correlate strongly with particular K-magnitude intervals, corresponding to different zero-age, main-sequence (MS) masses and lifetimes. Stars with 14 ≲ m{sub K} ≲ 15 (15-20 M {sub ☉}, t {sub MS} = 8-13 Myr) match a disk formation origin well, whereas those with m{sub K} ≥ 15 (<15 M {sub ☉}, t {sub MS} > 13 Myr), if isotropically distributed, form a population that is more eccentric than thermal, which suggests a Hills binary-disruption origin.

  12. 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.

  13. Trigonometric parallaxes to star-forming regions within 4 kpc of the galactic center

    SciTech Connect (OSTI)

    Sanna, A.; Menten, K. M.; Zhang, B.; Sato, M.; Brunthaler, A.; Immer, K. [Max-Planck-Institut fr Radioastronomie, Auf dem Hgel 69, D-53121 Bonn (Germany); Reid, M. J.; Dame, T. M. [Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 (United States); Moscadelli, L., E-mail: asanna@mpifr-bonn.mpg.de [INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, I-50125 Firenze (Italy)

    2014-02-01

    We report four trigonometric parallaxes for high-mass star-forming regions within 4 kpc of the Galactic center. These measurements were made with the Very Long Baseline Array as part of the BeSSeL Survey. By associating these sources kinematically with large-scale features in CO and H I longitude-velocity diagrams, we begin to outline some major features of the inner Milky Way: the Connecting arm, the near and far 3 kpc arms, and the Norma arm. The Connecting arm in the first Galactic quadrant lies closer to the Galactic center than the far 3 kpc arm and is offset by the long-bar's major axis near its leading edge, supporting the presence of an inner Lindblad resonance. Assuming the 3 kpc arms are a continuous physical structure, the relative Galactocentric distance of its near and far sides suggests highly elliptical streamlines of gas around the bar(s) and a bar corotation radius, r {sub CR} ? 3.6 kpc. At a Galactic longitude near 10 and a heliocentric distance of about 5 kpc, the near 3 kpc arm and the Norma arm intersect on a face-on view of our Galaxy, while passing at different Galactic latitudes. We provide an accurate distance measurement to the W 31 star-forming complex of 4.95{sub ?0.43}{sup +0.51} kpc from the Sun, which associates it with a bright CO feature belonging to the near 3 kpc arm.

  14. Beam-based measurement of the center of the new STAR pipe

    SciTech Connect (OSTI)

    Robert-Demolaize, G.

    2014-02-25

    During the RHIC Shutdown preceding Run13 for polarized protons, various upgrades were brought to the STAR detector, one of which being the partial installation of the Forward GEM Tracker (FGT). This installation includes a new beam pipe at the center of the detector with an internal radius half the size of what the replaced pipe was, from 40 mm to 20 mm. The following reviews the results of a vertical aperture scans in the STAR interaction region performed at injection energy with both beams, and gives an estimate of the measured transverse offset of the new STAR pipe.

  15. Sinusoidal Siemens star spatial frequency response measurement errors due to misidentified target centers

    SciTech Connect (OSTI)

    Birch, Gabriel Carisle; Griffin, John Clark

    2015-07-23

    Numerous methods are available to measure the spatial frequency response (SFR) of an optical system. A recent change to the ISO 12233 photography resolution standard includes a sinusoidal Siemens star test target. We take the sinusoidal Siemens star proposed by the ISO 12233 standard, measure system SFR, and perform an analysis of errors induced by incorrectly identifying the center of a test target. We show a closed-form solution for the radial profile intensity measurement given an incorrectly determined center and describe how this error reduces the measured SFR of the system. As a result, using the closed-form solution, we propose a two-step process by which test target centers are corrected and the measured SFR is restored to the nominal, correctly centered values.

  16. Sinusoidal Siemens star spatial frequency response measurement errors due to misidentified target centers

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

    Birch, Gabriel Carisle; Griffin, John Clark

    2015-07-23

    Numerous methods are available to measure the spatial frequency response (SFR) of an optical system. A recent change to the ISO 12233 photography resolution standard includes a sinusoidal Siemens star test target. We take the sinusoidal Siemens star proposed by the ISO 12233 standard, measure system SFR, and perform an analysis of errors induced by incorrectly identifying the center of a test target. We show a closed-form solution for the radial profile intensity measurement given an incorrectly determined center and describe how this error reduces the measured SFR of the system. As a result, using the closed-form solution, we proposemore » a two-step process by which test target centers are corrected and the measured SFR is restored to the nominal, correctly centered values.« less

  17. 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

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

    SciTech Connect (OSTI)

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

    2008-06-30

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

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

    Office of Legacy Management (LM)

    Pinellas Environmental Restoration Project - Young- Rainey Star Center 110406202 Accutest Job Number: F33039 Sampling Date: 07/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road *

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

    Office of Legacy Management (LM)

    Sampling (Pinellas Co), STAR Center, Largo, FL 110406202 Accutest Job Number: F23259 Sampling Date: 04/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL

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

    Office of Legacy Management (LM)

    Young - Rainey Star Center 110406202 Accutest Job Number: F35489 Sampling Date: 10/05/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel:

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

    Office of Legacy Management (LM)

    Young - Rainey Star Center 110406202 Accutest Job Number: F30886 Sampling Date: 04/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel:

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

    Office of Legacy Management (LM)

    6/06 Technical Report for S M Stoller Pinellas Environmental Restoration Project - Young - Rainey Star Center 110406202 Accutest Job Number: F43553 Sampling Date: 09/07/06 Report to: U.S. Dept of Energy, Grand Jct Office 2597 B 3/4 Road Grand Juction, CO 81503 ATTN: Contracts Department, PO# 24231 x Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its

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

    Office of Legacy Management (LM)

    Pinellas Environmental Restoration Project - Young- Rainey Star Center 7030-226 Accutest Job Number: F29125 Sampling Date: 01/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite

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

    Office of Legacy Management (LM)

    STAR Center- 4.5 Acre Site, Largo, FL 7030-226/Monthly Accutest Job Number: F27168 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811

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

    Office of Legacy Management (LM)

    STAR Center- 4.5 Acre Site, Largo, FL 110406202 Accutest Job Number: F23552 Sampling Date: 04/20/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel:

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

    Office of Legacy Management (LM)

    STAR Center- 4.5 Acre Site, Largo, FL 110406202 Accutest Job Number: F25243 Sampling Date: 07/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel:

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

    Office of Legacy Management (LM)

    1/06 Technical Report for S M Stoller Star Center-B100 Monthly/Effluent; Largo, FL 7031-226 Accutest Job Number: F37650 Sampling Date: 01/05/06 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland

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

    Office of Legacy Management (LM)

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

  10. FROM BLUE STAR-FORMING TO RED PASSIVE: GALAXIES IN TRANSITION IN DIFFERENT ENVIRONMENTS

    SciTech Connect (OSTI)

    Vulcani, Benedetta; Poggianti, Bianca M.; Fasano, Giovanni; Moretti, Alessia; Fritz, Jacopo; Calvi, Rosa; Paccagnella, Angela

    2015-01-01

    Exploiting a mass-complete (M {sub *}>10{sup 10.25} M {sub ?}) sample at 0.03star-formation activity and/or morphology: green galaxies, red passive late types, and blue star-forming early types. Color fractions depend on mass and only for M {sub *}< 10{sup 10.7} M {sub ?} on environment. The incidence of red galaxies increases with increasing mass, and, for M {sub *}< 10{sup 10.7} M {sub ?}, decreases toward the group outskirts and in binary and single galaxies. The relative abundance of green and blue galaxies is independent of environment and increases monotonically with galaxy mass. We also inspect galaxy structural parameters, star-formation properties, histories, and ages and propose an evolutionary scenario for the different subpopulations. Color transformations are due to a reduction and suppression of the star-formation rate in both bulges and disks that does not noticeably affect galaxy structure. Morphological transitions are linked to an enhanced bulge-to-disk ratio that is due to the removal of the disk, not to an increase of the bulge. Our modeling suggests that green colors might be due to star-formation histories declining with long timescales, as an alternative scenario to the classical ''quenching'' processes. Our results suggest that galaxy transformations in star-formation activity and morphology depend neither on the environment nor on being a satellite or the most massive galaxy of a halo. The only environmental dependence we find is the higher fast quenching efficiency in groups giving origin to poststarburst signatures.

  11. THE FINAL FATE OF STARS THAT IGNITE NEON AND OXYGEN OFF-CENTER: ELECTRON CAPTURE OR IRON CORE-COLLAPSE SUPERNOVA?

    SciTech Connect (OSTI)

    Jones, Samuel; Hirschi, Raphael; Nomoto, Ken'ichi

    2014-12-20

    In the ONeMg cores of 8.8-9.5 M {sub ?}stars, neon and oxygen burning is ignited off-center. Whether or not the neon-oxygen flame propagates to the center is critical for determining whether these stars undergo Fe core collapse or electron-capture-induced ONeMg core collapse. We present more details of stars that ignite neon and oxygen burning off-center. The neon flame is established in a manner similar to the carbon flame of super-AGB stars, albeit with a narrower flame width. The criteria for establishing a flame can be met if the strict Schwarzschild criterion for convective instability is adopted. Mixing across the interface of the convective shell disrupts the conditions for the propagation of the burning front, and instead the shell burns as a series of inward-moving flashes. While this may not directly affect whether or not the burning will reach the center (as in super-AGB stars), the core is allowed to contract between each shell flash. Reduction of the electron fraction in the shell reduces the Chandrasekhar mass and the center reaches the threshold density for the URCA process to activate and steer the remaining evolution of the core. This highlights the importance of a more accurate treatment of mixing in the stellar interior for yet another important question in stellar astrophysicsdetermining the properties of stellar evolution and supernova progenitors at the boundary between electron capture supernova and iron core-collapse supernova.

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

    Broader source: Energy.gov [DOE]

    Since 2003, the Lewis and Clark Garden Club (LCGC) of St. Charles County, Missouri, has held their monthly meetings in the Weldon Spring Interpretive Center (WSIC). The LCGC has 22 active members...

  13. A dynamo model of magnetic activity in solar-like stars with different rotational velocities

    SciTech Connect (OSTI)

    Karak, Bidya Binay; Choudhuri, Arnab Rai; Kitchatinov, Leonid L.

    2014-08-10

    We attempt to provide a quantitative theoretical explanation for the observations that Ca II H/K emission and X-ray emission from solar-like stars increase with decreasing Rossby number (i.e., with faster rotation). Assuming that these emissions are caused by magnetic cycles similar to the sunspot cycle, we construct flux transport dynamo models of 1 M{sub ☉} stars rotating with different rotation periods. We first compute the differential rotation and the meridional circulation inside these stars from a mean-field hydrodynamics model. Then these are substituted in our dynamo code to produce periodic solutions. We find that the dimensionless amplitude f{sub m} of the toroidal flux through the star increases with decreasing rotation period. The observational data can be matched if we assume the emissions to go as the power 3-4 of f{sub m}. Assuming that the Babcock-Leighton mechanism saturates with increasing rotation, we can provide an explanation for the observed saturation of emission at low Rossby numbers. The main failure of our model is that it predicts an increase of the magnetic cycle period with increasing rotation rate, which is the opposite of what is found observationally. Much of our calculations are based on the assumption that the magnetic buoyancy makes the magnetic flux tubes rise radially from the bottom of the convection zone. Taking into account the fact that the Coriolis force diverts the magnetic flux tubes to rise parallel to the rotation axis in rapidly rotating stars, the results do not change qualitatively.

  14. INDEPENDENT TECHNICAL REVIEW OF THE BUILDING 100 PLUME, FORMER DOE PINELLAS SITE (YOUNG - RAINEY STAR CENTER), LARGO, FLORIDA

    SciTech Connect (OSTI)

    Eddy-Dilek, C.; Rossabi, J.; Amidon, M.; Riha, B.; Kaback, D.

    2010-07-30

    Contaminated groundwater associated with Building 100 at the Young-Rainey Science, Technology, and Research Center, formerly the DOE Pinellas plant, is the primary remedial challenge that remains to be addressed at the site. Currently, Building 100 is an active industrial facility that is now owned and operated by the Pinellas county government. Groundwater samples collected from monitoring wells recently installed near the southern boundary of the site suggest that contaminated groundwater has migrated off the plant site. In response to the challenges presented by the Building 100 plume, the Office of Legacy Management (LM) requested assistance from the DOE Office of Groundwater and Soil Remediation (EM-32) to provide a review team to make technical recommendations so that they can efficiently and effectively address characterization and remediation of the plume. The review team was unanimous in the conclusion that a dynamic strategy that combines a phased implementation of direct push samplers, sensors, and tools can be used to better delineate the extent of contamination, control plume migration, and rapidly remediate the contaminated groundwater at the site. The initial efforts of the team focused on reviewing the site history and data, organizing the information into a conceptual model, identifying appropriate technologies, and recommending an integrated strategy. The current groundwater data from the site indicate a two-lobed plume extending to the east and south. To the east vinyl chloride is the primary contaminant of concern, to the south, vinyl chloride and cis1, 2-DCE are the primary contaminants. The limited data that are available suggest that reductive dechlorination of the TCE is already occurring but is not sufficient to prevent offsite migration of low concentrations of TCE daughter products. The team recommends that DOE pursue a strategy that builds on the natural cleansing capacity of the subsurface with reductive methods including biostimulation

  15. 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

  16. The impact of galaxy geometry and mass evolution on the survival of star clusters

    SciTech Connect (OSTI)

    Madrid, Juan P.; Hurley, Jarrod R.; Martig, Marie

    2014-04-01

    Direct N-body simulations of globular clusters in a realistic Milky-Way-like potential are carried out using the code NBODY6 to determine the impact of the host galaxy disk mass and geometry on the survival of star clusters. A relation between disk mass and star-cluster dissolution timescale is derived. These N-body models show that doubling the mass of the disk from 5 10{sup 10} M {sub ?} to 10 10{sup 10} M {sub ?} halves the dissolution time of a satellite star cluster orbiting the host galaxy at 6 kpc from the galactic center. Different geometries in a disk of identical mass can determine either the survival or dissolution of a star cluster orbiting within the inner 6 kpc of the galactic center. Furthermore, disk geometry has measurable effects on the mass loss of star clusters up to 15 kpc from the galactic center. N-body simulations performed with a fine output time step show that at each disk crossing the outer layers of star clusters experiences an increase in velocity dispersion of ?5% of the average velocity dispersion in the outer section of star clusters. This leads to an enhancement of mass lossa clearly discernable effect of disk shocking. By running models with different inclinations, we determine that star clusters with an orbit that is perpendicular to the Galactic plane have larger mass loss rates than do clusters that evolve in the Galactic plane or in an inclined orbit.

  17. 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...

  18. 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...

  19. 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.

  20. Better Buildings Residential Program Solution Center Demonstration...

    Office of Environmental Management (EM)

    The Better Buildings Residential Program Solution Center is a robust online collection of ... Neighborhood Program partners, Home Performance with ENERGY STAR Sponsors, and others. ...

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

    SciTech Connect (OSTI)

    Jones, S.; Hirschi, R.; Nomoto, K.; Fischer, T.; Martinez-Pinedo, G.; Timmes, F. X.; Herwig, F.; Paxton, B.; Toki, H.; Suzuki, T.; Lam, Y. H.; Bertolli, M. G.

    2013-08-01

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

  2. 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.

  3. BUILDING LATE-TYPE SPIRAL GALAXIES BY IN-SITU AND EX-SITU STAR FORMATION

    SciTech Connect (OSTI)

    Pillepich, Annalisa; Madau, Piero; Mayer, Lucio

    2015-02-01

    We analyze the formation and evolution of the stellar components in ''Eris'', a 120pc resolution cosmological hydrodynamic simulation of a late-type spiral galaxy. The simulation includes the effects of a uniform UV background, a delayed-radiative-cooling scheme for supernova feedback, and a star formation recipe based on a high gas density threshold. It allows a detailed study of the relative contributions of ''in-situ'' (within the main host) and ''ex-situ'' (within satellite galaxies) star formation to each major Galactic component in a close Milky Way analog. We investigate these two star-formation channels as a function of galactocentric distance, along different lines of sight above and along the disk plane, and as a function of cosmic time. We find that: (1) approximately 70% of today's stars formed in-situ; (2) more than two thirds of the ex-situ stars formed within satellites after infall; (3) the majority of ex-situ stars are found today in the disk and in the bulge; (4) the stellar halo is dominated by ex-situ stars, whereas in-situ stars dominate the mass profile at distances ? 5 kpc from the center at high latitudes; and (5) approximately 25% of the inner, r ? 20 kpc, halo is composed of in-situ stars that have been displaced from their original birth sites during Eris' early assembly history.

  4. METHANOL MASER EMISSION FROM GALACTIC CENTER SOURCES WITH EXCESS 4.5 {mu}m EMISSION

    SciTech Connect (OSTI)

    Chambers, E. T.; Yusef-Zadeh, F.; Roberts, D. E-mail: zadeh@northwestern.edu

    2011-05-20

    We present a study of signatures of on-going star formation in a sample of protostellar objects with enhanced 4.5 {mu}m emission ('green' sources) near the Galactic center. To understand how star formation in the Galactic center region compares to that of the Galactic disk, we used the Expanded Very Large Array to observe radiatively excited Class II 6.7 GHz CH{sub 3}OH masers and collisionally excited Class I 44 GHz CH{sub 3}OH masers, both tracers of high-mass star formation, toward a sample of 34 Galactic center and foreground 'green' sources. We find that 33% {+-} 15% of Galactic center sources are coincident with 6.7 GHz masers, and that 44% {+-} 17% of foreground sources are coincident with 6.7 GHz masers. For 44 GHz masers, we find correlation rates of 27% {+-} 13% and 25% {+-} 13% for Galactic center green sources and foreground green sources, respectively. Based on these CH{sub 3}OH maser detection rates, as well as correlations of green sources with other tracers of star formation, such as 24 {mu}m emission and infrared dark clouds (IRDCs), we find no significant difference between the green sources in the Galactic center and those foreground to it. This suggests that once the star formation process has begun, the environmental differences between the Galactic center region and the Galactic disk have little effect on its observational signatures. We do find, however, some evidence that may support a recent episode of star formation in the Galactic center region.

  5. 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.

  6. 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.

  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 TIDAL DISRUPTION OF GIANT STARS AND THEIR CONTRIBUTION TO THE FLARING SUPERMASSIVE BLACK HOLE POPULATION

    SciTech Connect (OSTI)

    MacLeod, Morgan; Guillochon, James; Ramirez-Ruiz, Enrico E-mail: jfg@ucolick.org

    2012-10-01

    Sun-like stars are thought to be regularly disrupted by supermassive black holes (SMBHs) within galactic nuclei. Yet, as stars evolve off the main sequence their vulnerability to tidal disruption increases drastically as they develop a bifurcated structure consisting of a dense core and a tenuous envelope. Here we present the first hydrodynamic simulations of the tidal disruption of giant stars and show that the core has a substantial influence on the star's ability to survive the encounter. Stars with more massive cores retain large fractions of their envelope mass, even in deep encounters. Accretion flares resulting from the disruption of giant stars should last for tens to hundreds of years. Their characteristic signature in transient searches would not be the t {sup -5/3} decay typically associated with tidal disruption events, but a correlated rise over many orders of magnitude in brightness on timescales of months to years. We calculate the relative disruption rates of stars of varying evolutionary stages in typical galactic centers, then use our results to produce Monte Carlo realizations of the expected flaring event populations. We find that the demographics of tidal disruption flares are strongly dependent on both stellar and black hole mass, especially near the limiting SMBH mass scale of {approx}10{sup 8} M{sub Sun }. At this black hole mass, we predict a sharp transition in the SMBH flaring diet beyond which all observable disruptions arise from evolved stars, accompanied by a dramatic cutoff in the overall tidal disruption flaring rate. Black holes less massive than this limiting mass scale will show observable flares from both main-sequence and evolved stars, with giants contributing up to 10% of the event rate. The relative fractions of stars disrupted at different evolutionary states can constrain the properties and distributions of stars in galactic nuclei other than our own.

  9. 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.

  10. 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.

  11. The Worker Component At The World Trade Center Cleanup: Addressing Cultural And Language Differences In Emergency Operations

    SciTech Connect (OSTI)

    McCabe, B.; Carpenter, C.; Blair. D.

    2003-02-24

    On September 11, 2001, the terrorist attacks on the World Trade Center (WTC) caused astronomical loss of life and property. Systems in place to manage disaster response were strained to the limit because key first responders were among the casualties when the twin towers collapsed. In addition, the evolution of events required immediate response in a rapidly changing and extremely hazardous situation. Rescue, recovery, and clean up became an overpowering and sustained effort that would utilize the resources of federal, state and local governments and agencies. One issue during the response to the WTC disaster site that did not receive much attention was that of the limited and non-English speaking worker. The Operating Engineers National HAZMAT Program (OENHP), with its history of a Hispanic Outreach Program, was acutely aware of this issue with the Hispanic worker. The Hispanic population comprises approximately 27% of the population of New York City (1). The extremely unfortunate and tragic events of that day provided an opportunity to not only provide assistance for the Hispanic workers, but also to apply lessons learned and conduct studies on worker training with language barriers in a real life environment. However, due to the circumstances surrounding this tragedy, the study of these issues was conducted primarily by observation. Through partnerships with other organizations such as the Occupational Safety and Health Administration (OSHA), the New York Health Department, the New York Department of Design and Construction (DDC), the New York Committee for Occupational Safety and Health (NYCOSH), and private companies such as 3M and MSA, OENHP was able to provide translated information on hazards, protective measures, fit testing of respirators, and site specific safety and health training. The OENHP translated materials on hazards and how to protect workers into Spanish to assist in getting the information to the limited and non- English speaking workers.

  12. 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.

  13. 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.

  14. 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.

  15. 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...

  16. 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...

  17. 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.

  18. Center Organization | Center for Energy Efficient Materials

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

    Center Organization People People Scientific Advisory Board Center Organization

  19. Possible evidence for metal accretion onto the surfaces of metal-poor main-sequence stars

    SciTech Connect (OSTI)

    Hattori, Kohei; Yoshii, Yuzuru; Beers, Timothy C.; Carollo, Daniela; Lee, Young Sun

    2014-04-01

    The entire evolution of the Milky Way, including its mass-assembly and star-formation history, is imprinted onto the chemo-dynamical distribution function of its member stars, f(x, v, [X/H]), in the multi-dimensional phase space spanned by position, velocity, and elemental abundance ratios. In particular, the chemo-dynamical distribution functions for low-mass stars (e.g., G- or K-type dwarfs) are precious tracers of the earliest stages of the Milky Way's formation, since their main-sequence lifetimes approach or exceed the age of the universe. A basic tenet of essentially all previous analyses is that the stellar metallicity, usually parameterized as [Fe/H], is conserved over time for main-sequence stars (at least those that have not been polluted due to mass transfer from binary companions). If this holds true, any correlations between metallicity and kinematics for long-lived main-sequence stars of different masses, effective temperatures, or spectral types must strictly be the same, since they reflect the same mass-assembly and star-formation histories. By analyzing a sample of nearby metal-poor halo and thick-disk stars on the main sequence, taken from Data Release 8 of the Sloan Digital Sky Survey, we find that the median metallicity of G-type dwarfs is systematically higher (by about 0.2 dex) than that of K-type dwarfs having the same median rotational velocity about the Galactic center. If it can be confirmed, this finding may invalidate the long-accepted assumption that the atmospheric metallicities of long-lived stars are conserved over time.

  20. 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...

  1. Explosives Center

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

    Explosives Center Explosives Center at Los Alamos National Laboratory A world leader in energetic materials research, development and applications, the Explosives Center's unique capabilities enable a dynamic, flexible response to address multiple evolving mission needs. explosives experiment Comprehensive energetic materials development, characterization and testing are key strengths at Los Alamos National Laboratory. An experimental explosive is shown igniting during small-scale impact

  2. 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 ...

  3. 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...

  4. operations center

    National Nuclear Security Administration (NNSA)

    servers and other critical Operations Center equipment

  5. Independent air supply system filtered to protect against biological and radiological agents (99.7%).
  6. <...

  7. Help Center

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

    Los Alamos National Laboratory Advanced Simulation and Computing Menu Events Partnerships Help Center Events Partnerships Help Center Videos Advanced Simulation and Computing Program » Help Center Computing Help Center Help hotlines, hours of operation, training, technical assistance, general information Los Alamos National Laboratory Hours: Monday through Friday, 8:00 a.m. - noon, 1:00-5:00 p.m. Mountain time Telephone: (505) 665-4444 option 3 Fax: (505) 665-6333 E-mail: consult@lanl.gov 24

  8. The vast population of Wolf-Rayet and red supergiant stars in M101. I. Motivation and first results

    SciTech Connect (OSTI)

    Shara, Michael M.; Bibby, Joanne L.; Zurek, David; Crowther, Paul A.; Moffat, Anthony F. J.; Drissen, Laurent

    2013-12-01

    Assembling a catalog of at least 10,000 Wolf-Rayet (W-R) stars is an essential step in proving (or disproving) that these stars are the progenitors of Type Ib and Type Ic supernovae. To this end, we have used the Hubble Space Telescope (HST) to carry out a deep, He II optical narrowband imaging survey of the ScI spiral galaxy M101. Almost the entire galaxy was imaged with the unprecedented depth and resolution that only the HST affords. Differenced with archival broadband images, the narrowband images allow us to detect much of the W-R star population of M101. We describe the extent of the survey and our images, as well as our data reduction procedures. A detailed broadband-narrowband imaging study of a field east of the center of M101, containing the giant star-forming region NGC 5462, demonstrates our completeness limits, how we find W-R candidates, their properties and spatial distribution, and how we rule out most contaminants. We use the broadband images to locate luminous red supergiant (RSG) candidates. The spatial distributions of the W-R and RSG stars near NGC 5462 are strikingly different. W-R stars dominate the complex core, while RSGs dominate the complex halo. Future papers in this series will describe and catalog more than a thousand W-R and RSG candidates that are detectable in our images, as well as spectra of many of those candidates.

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

    Broader source: Energy.gov [DOE]

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

  10. Voluntary Protection Program Onsite Review, Transuranic Waste Processing Center- May 2009

    Broader source: Energy.gov [DOE]

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

  11. [?/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].

  12. 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.

  13. CenterPoint Energy Advanced Residential Lighting Program

    Office of Energy Efficiency and Renewable Energy (EERE)

    CenterPoint Energy’s Advanced Lighting program provides a point-of-sale discount on the purchase of selected Energy Star® rated LED products, such as screw-in LEDs and LED fixtures, which are...

  14. 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....

  15. 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...

  16. 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:...

  17. 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,

  18. Exploring atmospheres of hot mini-Neptune and extrasolar giant planets orbiting different stars with application to HD 97658b, WASP-12b, CoRoT-2b, XO-1b, and HD 189733b

    SciTech Connect (OSTI)

    Miguel, Y.; Kaltenegger, L.

    2014-01-10

    We calculated an atmospheric grid for hot mini-Neptune and giant exoplanets that links astrophysical observable parametersorbital distance and stellar typewith the chemical atmospheric species expected. The grid can be applied to current and future observations to characterize exoplanet atmospheres and serves as a reference to interpret atmospheric retrieval analysis results. To build the grid, we developed a one-dimensional code for calculating the atmospheric thermal structure and linked it to a photochemical model that includes disequilibrium chemistry (molecular diffusion, vertical mixing, and photochemistry). We compare the thermal profiles and atmospheric composition of planets at different semimajor axes (0.01 AU ? a ? 0.1 AU) orbiting F, G, K, and M stars. Temperature and UV flux affect chemical species in the atmosphere. We explore which effects are due to temperature and which are due to stellar characteristics, showing the species most affected in each case. CH{sub 4} and H{sub 2}O are the most sensitive to UV flux, H displaces H{sub 2} as the most abundant gas in the upper atmosphere for planets receiving a high UV flux. CH{sub 4} is more abundant for cooler planets. We explore vertical mixing, to inform degeneracies on our models and in the resulting spectral observables. For lower pressures, observable species like H{sub 2}O or CO{sub 2} can indicate the efficiency of vertical mixing, with larger mixing ratios for a stronger mixing. By establishing the grid, testing the sensitivity of the results, and comparing our model to published results, our paper provides a tool to estimate what observations could yield. We apply our model to WASP-12b, CoRoT-2b, XO-1b, HD189733b, and HD97658b.

  19. THE PUZZLE OF TWO DIFFERENT SUB-MICROMETER TUNGSTEN-RICH DEPOSITS IN BULK YBCO: ONE ACTS AS PINNING CENTERS AND THE OTHER DOES NOT

    SciTech Connect (OSTI)

    Sawh, Ravi-Persad; Weinstein, Roy; Parks, Drew; Gandini, Alberto [Beam Particle Dynamics Laboratory, Department of Physics, and Texas Center for Superconductivity, University of Houston, Houston, Texas, 77204 (United States)

    2010-04-08

    Two types of large grain YBCO samples doped with tungsten oxide, one with platinum and the other without, were produced using a slow cooling process. Observations of the trapped magnetic flux density showed that the flux density of the W-doped, Pt-free samples did not change with W doping levels of up to 2.1 mol%. In contrast, the (W+Pt)-doped samples resulted in a monotonic improvement in trapped magnetic flux density as a function of W doping. Microstructure studies indicate that both types of samples contain profuse sub-micrometer deposits of a W-rich compound. The Pt-free samples contain (W{sub 0.4}Y{sub 0.6})BaO{sub 3} deposits while the (W+Pt)-doped samples contain deposits of a (W{sub 0.5}Pt{sub 0.5})YBa{sub 2}O{sub 6} compound. Both types of deposits are of essentially the same size and have comparable number density. The results are strikingly similar to an earlier experiment in which uranium doped, Pt-free, large grain YBCO also did not show any improvement in trapped magnetic flux density. The U-doped, Pt-free samples contain profuse sub-micrometer deposits of a (U{sub 0.4}Y{sub 0.6})BaO{sub 3} compound, which have been shown to be ferromagnetic. The inability of both the (W{sub 0.4}Y{sub 0.6})BaO{sub 3} and (U{sub 0.4}Y{sub 0.6})BaO{sub 3} sub-micrometer deposits to act as pinning centers in self-field, suggest that this behavior is systematic.

  20. 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.

  21. 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

  22. Covered Product Category: Uninterruptible Power Supplies (for Data Center,

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

    Computer, and Telecommunication Applications) | Department of Energy Categories » Covered Product Category: Uninterruptible Power Supplies (for Data Center, Computer, and Telecommunication Applications) Covered Product Category: Uninterruptible Power Supplies (for Data Center, Computer, and Telecommunication Applications) The Federal Energy Management Program (FEMP) provides acquisition guidance for uninterruptible power supplies (UPS), a product category covered by the ENERGY STAR program.

  1. Covered Product Category: Uninterruptible Power Supplies (for Data Center,

    Office of Environmental Management (EM)

    Computer, and Telecommunication Applications) | Department of Energy Categories » Covered Product Category: Uninterruptible Power Supplies (for Data Center, Computer, and Telecommunication Applications) Covered Product Category: Uninterruptible Power Supplies (for Data Center, Computer, and Telecommunication Applications) The Federal Energy Management Program (FEMP) provides acquisition guidance for uninterruptible power supplies (UPS), a product category covered by the ENERGY STAR program.

  2. 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.

  3. 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.

  4. 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.

  5. 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)

  6. 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)

    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...

  7. 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:...

  8. 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...

  9. 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...

  10. 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...

  11. Danforth Center Tour | Photosynthetic Antenna Research Center

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

    Danforth Center Tour Danforth Center Tour As part of our Events & Topics in Bioenergy and the Environment series, we hosted a tour to the Donald Danforth Plant Science Center to...

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

    Office of Legacy Management (LM)

    531 Sampling Date: 04/16/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test results

  13. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    B100 7030-226/Monthly Accutest Job Number: F27169 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax:

  14. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    B100 Monthly Sampling, 110406202 Accutest Job Number: F25245 Sampling Date: 07/06/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 *

  15. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    B100 110406202 Accutest Job Number: F33040 Sampling Date: 07/06/05 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707

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

    Office of Legacy Management (LM)

    7170 Sampling Date: 10/05/04 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC (573), NJ (FL002), MA (FL946), IA (366), LA (03051), KS (E-10327), SC, AK This report shall not be reproduced, except in its entirety, without the written approval of Accutest Laboratories. Southeast * 4405 Vineland Road * Suite C-15 * Orlando, FL 32811 * tel: 407-425-6700 * fax: 407-425-0707 * http://www.accutest.com Test

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

    Office of Legacy Management (LM)

    ... anr Chromium 10 .4 anr Cobalt 50 .5 anr Copper 25 .44 anr Iron 300 7.1 anr Lead 5.0 1.2 ... anr Calcium anr Chromium anr Cobalt anr Copper anr Iron anr Lead anr Magnesium anr ...

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

    Office of Legacy Management (LM)

    ... 1000 3.8 Chromium 10 .4 Cobalt 50 .5 Copper 25 .4 Iron 300 7.1 anr Lead 5.0 1.2 anr ... Beryllium Cadmium Calcium Chromium Cobalt Copper Iron anr Lead anr Magnesium Manganese ...

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

    Office of Legacy Management (LM)

    ... 1000 3.8 Chromium 10 .4 Cobalt 50 .5 Copper 25 .44 anr Iron 300 7.1 anr Lead 5.0 1.2 ... Beryllium Cadmium Calcium Chromium Cobalt Copper anr Iron anr Lead anr Magnesium anr ...

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

    Office of Legacy Management (LM)

    ... anr Chromium 10 .5 anr Cobalt 50 .5 anr Copper 25 .4 anr Iron 300 16 anr Lead 5.0 1.2 ... anr Calcium anr Chromium anr Cobalt anr Copper anr Iron anr Lead anr Magnesium anr ...

  1. Quarterly Progress Report for the Young-Rainey STAR Center's...

    Office of Legacy Management (LM)

    ... changes during biosparge operations; * Determining biodegradation rates and oxygen consumption rates utilizing microcosm experiments with site soils and ground water; * Performing ...

  2. Quarterly Progress Report for the Young-Rainey STAR Center's...

    Office of Legacy Management (LM)

    ... Progress Report January 2003 Page 3 * Determining biodegradation rates and oxygen consumption rates utilizing microcosm experiments with site soils and ground water; * Performing ...

  3. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    Sampling Date: 060206 Report to: US Dept of Energy, Grand Jct Office 2597 B34 Road Grand Junction, CO 81503 ATTN: Contracts Department, PO 24231 x Total number of pages in ...

  4. 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...

  5. 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...

  6. Energy Frontier Research Center

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

    Energy Frontier Research Centers: Solid-State Lighting Science Center for Frontiers of ... Energy Frontier Research Center HomeEnergy ResearchEFRCsSolid-State Lighting Science ...

  7. ARM - External Data Center

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

    govExternal Data Center External Data Center Order Data Description of External Data Streams Data Viewers and Plots (selected data sets) XDC Documentation External Data Center The ...

  8. 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.

  9. 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.

  10. 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.

  11. 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.

  12. 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.

  13. 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.

  14. 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,...

  15. 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.

  16. 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.

  17. A SURVEY OF STELLAR FAMILIES: MULTIPLICITY OF SOLAR-TYPE STARS

    SciTech Connect (OSTI)

    Raghavan, Deepak; McAlister, Harold A.; Henry, Todd J.; Gies, Douglas R.; White, Russel J.; Latham, David W.; Marcy, Geoffrey W.; Mason, Brian D.; Ten Brummelaar, Theo A.

    2010-09-15

    We present the results of a comprehensive assessment of companions to solar-type stars. A sample of 454 stars, including the Sun, was selected from the Hipparcos catalog with {pi}>40 mas, {sigma}{sub {pi}/{pi}} < 0.05, 0.5 {<=} B - V {<=} 1.0 ({approx}F6-K3), and constrained by absolute magnitude and color to exclude evolved stars. These criteria are equivalent to selecting all dwarf and subdwarf stars within 25 pc with V-band flux between 0.1 and 10 times that of the Sun, giving us a physical basis for the term 'solar-type'. New observational aspects of this work include surveys for (1) very close companions with long-baseline interferometry at the Center for High Angular Resolution Astronomy Array, (2) close companions with speckle interferometry, and (3) wide proper-motion companions identified by blinking multi-epoch archival images. In addition, we include the results from extensive radial-velocity monitoring programs and evaluate companion information from various catalogs covering many different techniques. The results presented here include four new common proper-motion companions discovered by blinking archival images. Additionally, the spectroscopic data searched reveal five new stellar companions. Our synthesis of results from many methods and sources results in a thorough evaluation of stellar and brown dwarf companions to nearby Sun-like stars. The overall observed fractions of single, double, triple, and higher-order systems are 56% {+-} 2%, 33% {+-} 2%, 8% {+-} 1%, and 3% {+-} 1%, respectively, counting all confirmed stellar and brown dwarf companions. If all candidate, i.e., unconfirmed, companions identified are found to be real, the percentages would change to 54% {+-} 2%, 34% {+-} 2%, 9% {+-} 2%, and 3% {+-} 1%, respectively. Our completeness analysis indicates that only a few undiscovered companions remain in this well-studied sample, implying that the majority (54% {+-} 2%) of solar-type stars are single, in contrast to the results of prior

  18. Bisfuel links - Research centers

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

    Research centers http://bioenergy.asu.edu/" target="_blank">Center for Bioenergy and Photosynthesis

  19. 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.

  20. 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...

  1. Alternative Fuels Data Center

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

    Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples Summary Tables Key Federal Legislation The information below includes a brief chronology and

  2. Alternative Fuels Data Center

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

    Local Examples Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  3. Alternative Fuels Data Center

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

    Search Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples Summary

  4. Alternative Fuels Data Center

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

    Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Fuel Properties Search Fuel Properties Comparison Create a custom chart

  5. Alternative Fuels Data Center

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

    About the Data Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  6. Alternative Fuels Data Center

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

    State Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples Summary

  7. Alternative Fuels Data Center

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

    Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  8. Alternative Fuels Data Center

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

    Summary Tables Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  9. Alternative Fuels Data Center

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

    Federal Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples Summary

  10. Alternative Fuels Data Center

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

    State Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples Summary

  11. Alternative Fuels Data Center

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

    Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Truckstop Electrification Truck Stop Electrification Locator Locate

  12. Alternative Fuels Data Center

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

    AFDC Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... Vehicle and Infrastructure Cash-Flow Evaluation Model VICE 2.0: Vehicle

  13. Alternative Fuels Data Center

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

    Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  14. Alternative Fuels Data Center

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

    Incentives » Federal Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local

  15. Alternative Fuels Data Center

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

    Incentives Printable Version Share this resource Send a link to Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center on Delicious Rank Alternative Fuels Data Center on Digg Find More places to share Alternative Fuels Data Center on AddThis.com... More in this section... Search Federal State Local Examples

  16. 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.

  17. 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.

  18. 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

  19. 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.

  20. 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 ...

  1. 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

  2. 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.

  3. Center for Nonlinear Studies

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

    Applied Geophysical Experiences Materials Design Calendar NSEC Center for Nonlinear Studies Center for Nonlinear Studies Serving as an interface between mission...

  4. NREL: Education Center - Programs

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

    Education Center Printable Version Programs NREL's Education Center in Golden, Colorado, offers a variety of program topics and experiences for students and adult groups addressing...

  5. NREL: Education Center - Events

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

    Education Center Printable Version Events Unless otherwise notified, events listed here will be held at the NREL Education Center, 15013 Denver West Parkway, Golden, CO. The...

  6. Biofuels Information Center

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

    Biofuels Information Center BETO 2015 Peer Review Kristi Moriarty March 24, 2015 2 Goal Statement * The purpose of the Biofuels Information Center (BIC) task is to increase ...

  7. First National Technology Center

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

    First National Technology First National Technology Center Center Electronic Equipment - manufactured to withstand 8 milliseconds of voltage disruption CBEMA Curve - Chips ...

  8. Electron Microscopy Center

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

    Electron Microscopy Center Argonne Home > EMC > EMC Home Electron Microscopy Center Web Site has moved This page has moved to http:www.anl.govcnmgroupelectron-microscopy-cente...

  9. 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.

  10. 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...

  11. 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.

  12. 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.

  13. 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

  14. 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...

  15. RSF Data Center Tour

    SciTech Connect (OSTI)

    Powers, Chuck

    2011-01-01

    The Data Center in the Research Support Facility on the campus of the U.S. Department of Energy's National Renewable Energy Laboratory (NREL) marks a significant accomplishment in its ultra-efficiency. Data centers by nature are very energy intensive. The RSF Data Center was designed to use 80% less energy than NREL's old data center, which had been in use for the last 30 years. This tour takes you through the data center highlighting its energy saving techniques.

  16. Theory Center | Jefferson Lab

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

    Theory Center The Center for Theoretical and Computational Physics pursues a broad program of research in support of the physics being studied at Jefferson Lab and related facilities around the world. The Theory Center provides opportunities for interested scientists and students to visit the lab and work closely with theoretical and experimental colleagues.The center also advises the lab on the scientific merit of its program and its plans for future development. The center provides scientific

  17. tracc-comuting-center-html

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

    Transportation Research and Analysis Computing Center

  18. 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

  19. 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...

  20. 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,...

  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. 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...

  3. 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...

  4. 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.

  5. 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.

  6. 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.

  7. 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.

  8. Neutron stars' X-ray superbursts mystify, inspire Los Alamos scientists

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

    Neutron stars' X-ray superbursts mystify, inspire Neutron stars' X-ray superbursts mystify, inspire Los Alamos scientists Massive X-ray superbursts near the surface of neutron stars are providing a unique window into the operation of fundamental forces of nature under extreme conditions. December 6, 2013 A small, dense object only 12 miles in diameter is responsible for this beautiful X-ray nebula that spans 150 light years. At the center of this image made by NASA's Chandra X-ray Observatory is

  9. Star formation histories across the interacting galaxy NGC 6872, the largest-known spiral

    SciTech Connect (OSTI)

    Eufrasio, Rafael T.; De Mello, Duilia F.; Dwek, Eli; Arendt, Richard G.; Benford, Dominic J.; Gadotti, Dimitri A.; Urrutia-Viscarra, Fernanda; De Oliveira, Claudia Mendes

    2014-11-01

    NGC 6872, hereafter the Condor, is a large spiral galaxy that is interacting with its closest companion, the S0 galaxy IC 4970. The extent of the Condor provides an opportunity for detailed investigation of the impact of the interaction on the current star formation rate and its history across the galaxy, on the age and spatial distribution of its stellar population, and on the mechanism that drives the star formation activity. To address these issues we analyzed the far-ultraviolet (FUV) to near-infrared (near-IR) spectral energy distribution of seventeen 10 kpc diameter regions across the galaxy, and derived their star formation history, current star formation rate, and stellar population and mass. We find that most of the star formation takes place in the extended arms, with very little star formation in the central 5 kpc of the galaxy, in contrast to what was predicted from previous numerical simulations. There is a trend of increasing star formation activity with distance from the nucleus of the galaxy, and no evidence for a recent increase in the current star formation rate due to the interaction. The nucleus itself shows no significant current star formation activity. The extent of the Condor also provides an opportunity to test the applicability of a single standard prescription for conversion of the FUV + IR (22 ?m) intensities to a star formation rate for all regions. We find that the conversion factor differs from region to region, arising from regional differences in the stellar populations.

  10. CONSTRAINING TIDAL DISSIPATION IN STARS FROM THE DESTRUCTION RATES OF EXOPLANETS

    SciTech Connect (OSTI)

    Penev, Kaloyan; Jackson, Brian; Spada, Federico; Thom, Nicole

    2012-06-01

    We use the distribution of extrasolar planets in circular orbits around stars with surface convective zones detected by ground-based transit searches to constrain how efficiently tides raised by the planet are dissipated on the parent star. We parameterize this efficiency as a tidal quality factor (Q{sub *}). We conclude that the population of currently known planets is inconsistent with Q{sub *} < 10{sup 7} at the 99% level. Previous studies show that values of Q{sub *} between 10{sup 5} and 10{sup 7} are required in order to explain the orbital circularization of main-sequence low-mass binary stars in clusters, suggesting that different dissipation mechanisms might be acting in the two cases, most likely due to the very different tidal forcing frequencies relative to the stellar rotation frequency occurring for star-star versus planet-star systems.

  11. 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...

  12. 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...

  13. UAIEE and Industrial Assessment Centers

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

    55-62011| Industrial Assessment Centers * Started in 1976 * Currently 26 Centers across the US * Almost...

  14. Service Center Evaluation Guide

    Office of Energy Efficiency and Renewable Energy (EERE)

    To be assured of a quality product, customers of motor repair service centers need to be knowledgeable about the service they're purchasing. This guide provides information to assist in evaluating motor repair service centers.

  15. ASU EFRC - Center researchers

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

    Center researchers Chad Simmons Academic Professional Gerdenis Kodis Research Assistant Professor Raimund Fromme Faculty Research Associate Yuichi Terazono Faculty Research...

  16. Applied Research Center

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

    ARC Privacy and Security Notice Skip over navigation Search the JLab Site Applied Research Center Please upgrade your browser. This site's design is only visible in a graphical browser that supports web standards, but its content is accessible to any browser. Concerns? Applied Research Center ARC Home Consortium News EH&S Reports print version ARC Resources Commercial Tenants ARC Brochure Library Conference Room Applied Research Center Applied Research Center front view Applied Research

  17. Green Jobs Training Center

    Broader source: Energy.gov [DOE]

    Provides an overview of the training available through the Green Jobs Training Center including certification courses and the apprenticeship program.

  18. Center for Nanoscale Materials

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

    Laboratory is a U.S. Department of Energy laboratory managed by UChicago Argonne, LLC. www.anl.gov CENTER FOR NANOSCALE MATERIALS A premier user facility providing expertise, instruments, and infrastructure for interdisciplinary nanoscience and nanotechnology research. The Center for Nanoscale Materials (CNM) is a premier user facility operating as one of the five centers built across the nation as part of the U.S. Department of Energy's (DOE's) Nanoscale Science Research Center program under

  19. Center for Advanced Photophysics | About The Center

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

    Victor Klimov - Center for Advanced Solar Photophysics Message from Center Director The solution to the global energy challenge requires revolutionary breakthroughs in areas such as the conversion of solar energy into electrical power or chemical fuels. The principles for capturing solar light and converting it into electrical charges have not changed for more than four decades. Previous advances in this area have mostly relied on iterative improvements in material quality and/or device

  20. 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.

  1. Data center cooling method

    DOE Patents [OSTI]

    Chainer, Timothy J.; Dang, Hien P.; Parida, Pritish R.; Schultz, Mark D.; Sharma, Arun

    2015-08-11

    A method aspect for removing heat from a data center may use liquid coolant cooled without vapor compression refrigeration on a liquid cooled information technology equipment rack. The method may also include regulating liquid coolant flow to the data center through a range of liquid coolant flow values with a controller-apparatus based upon information technology equipment temperature threshold of the data center.

  2. 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;...

  3. 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...

  4. 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.

  5. THE DETAILED CHEMICAL PROPERTIES OF M31 STAR CLUSTERS. I. Fe, ALPHA AND LIGHT ELEMENTS

    SciTech Connect (OSTI)

    Colucci, Janet E.; Bernstein, Rebecca A.; Cohen, Judith G.

    2014-12-20

    We present ages, [Fe/H] and abundances of the α elements Ca I, Si I, Ti I, Ti II, and light elements Mg I, Na I, and Al I for 31 globular clusters (GCs) in M31, which were obtained from high-resolution, high signal-to-noise ratio >60 echelle spectra of their integrated light (IL). All abundances and ages are obtained using our original technique for high-resolution IL abundance analysis of GCs. This sample provides a never before seen picture of the chemical history of M31. The GCs are dispersed throughout the inner and outer halo, from 2.5 kpc < R {sub M31} < 117 kpc. We find a range of [Fe/H] within 20 kpc of the center of M31, and a constant [Fe/H] ∼ – 1.6 for the outer halo clusters. We find evidence for at least one massive GC in M31 with an age between 1 and 5 Gyr. The α-element ratios are generally similar to the Milky Way GC and field star ratios. We also find chemical evidence for a late-time accretion origin for at least one cluster, which has a different abundance pattern than other clusters at similar metallicity. We find evidence for star-to-star abundance variations in Mg, Na, and Al in the GCs in our sample, and find correlations of Ca, Mg, Na, and possibly Al abundance ratios with cluster luminosity and velocity dispersion, which can potentially be used to constrain GC self-enrichment scenarios. Data presented here were obtained with the HIRES echelle spectrograph on the Keck I telescope.

  6. Alternative Fuels Data Center: About the Alternative Fuels Data Center

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

    About Printable Version Share this resource Send a link to Alternative Fuels Data Center: About the Alternative Fuels Data Center to someone by E-mail Share Alternative Fuels Data Center: About the Alternative Fuels Data Center on Facebook Tweet about Alternative Fuels Data Center: About the Alternative Fuels Data Center on Twitter Bookmark Alternative Fuels Data Center: About the Alternative Fuels Data Center on Google Bookmark Alternative Fuels Data Center: About the Alternative Fuels Data

  7. Center for Inverse Design: Organization of the Center for Inverse...

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

    Organization of the Center for Inverse Design This page shows the organizational management structure of the Center for Inverse Design, an Energy Frontier Research Center. It also ...

  8. 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.

  9. Abramovo Counterterrorism Training Center

    SciTech Connect (OSTI)

    Hayes, Christopher M; Ross, Larry; Lingenfelter, Forrest E; Sokolnikov, Pavel I; Kaldenbach, Karen Yvonne; Estigneev, Yuri; Murievav, Andrey

    2011-01-01

    The U.S. government has been assisting the Russian Federation (RF) Ministry of Defense (MOD) for many years with nuclear weapons transportation security (NWTS) through the provision of specialized guard escort railcars and cargo railcars with integrated physical security and communication systems, armored transport vehicles, and armored escort vehicles. As a natural continuation of the NWTS program, a partnership has been formed to construct a training center that will provide counterterrorism training to personnel in all branches of the RF MOD. The Abramovo Counterterrorism Training Center (ACTC) is a multinational, multiagency project with funding from Canada, RF and the U.S. Departments of Defense and Energy. ACTC will be a facility where MOD personnel can conduct basic through advanced training in various security measures to protect Category IA material against the threat of terrorist attack. The training will enhance defense-in-depth principles by integrating MOD guard force personnel into the overall physical protection systems and improving their overall response time and neutralization capabilities. The ACTC project includes infrastructure improvements, renovation of existing buildings, construction of new buildings, construction of new training facilities, and provision of training and other equipment. Classroom training will be conducted in a renovated training building. Basic and intermediate training will be conducted on three different security training areas where various obstacles and static training devices will be constructed. The central element of ACTC, where advanced training will be held, is the 'autodrome,' a 3 km road along which various terrorist events can be staged to challenge MOD personnel in realistic and dynamic nuclear weapons transportation scenarios. This paper will address the ACTC project elements and the vision for training development and integrating this training into actual nuclear weapons transportation operations.

  10. Protoneutron star evolution and the neutrino-driven wind in general relativistic neutrino radiation hydrodynamics simulations

    SciTech Connect (OSTI)

    Fischer, T.; Mezzacappa, Anthony; Thielemann, F.-K.; Liebendoerfer, M.; Whitehouse, S.

    2010-01-01

    Massive stars end their lives in explosions with kinetic energies on the order of 10{sup 51} erg. Immediately after the explosion has been launched, a region of low density and high entropy forms behind the ejecta, which is continuously subject to neutrino heating. The neutrinos emitted from the remnant at the center, the protoneutron star (PNS), heat the material above the PNS surface. This heat is partly converted into kinetic energy, and the material accelerates to an outflow that is known as the neutrino-driven wind. For the first time we simulate the collapse, bounce, explosion, and the neutrino-driven wind phases consistently over more than 20 s. Our numerical model is based on spherically symmetric general relativistic radiation hydrodynamics using spectral three-flavor Boltzmann neutrino transport. In simulations where no explosions are obtained naturally, we model neutrino-driven explosions for low- and intermediate-mass Fe-core progenitor stars by enhancing the charged current reaction rates. In the case of a special progenitor star, the 8.8 M{circle_dot} O-Ne-Mg-core, the explosion in spherical symmetry was obtained without enhanced opacities. The post-explosion evolution is in qualitative agreement with static steady-state and parametrized dynamic models of the neutrino-driven wind. On the other hand, we generally find lower neutrino luminosities and mean neutrino energies, as well as a different evolutionary behavior of the neutrino luminosities and mean neutrino energies. The neutrino-driven wind is proton-rich for more than 10 s and the contraction of the PNS differs from the assumptions made for the conditions at the inner boundary in previous neutrino-driven wind studies. Despite the moderately high entropies of about 100 k{sub B}/baryon and the fast expansion timescales, the conditions found in our models are unlikely to favor r-process nucleosynthesis. The simulations are carried out until the neutrino-driven wind settles down to a quasi

  11. 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...

  12. Polymer Engineering Center

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

    Polymer Engineering Center University of Wisconsin-Madison Experimental and Numerical Studies of the Temperature Field in Selective Laser Sintering to Improve Shrinkage and Warpage Prediction Prof. Dr.-Ing. Natalie Rudolph Polymer Engineering Center Department of Mechanical Engineering University of Wisconsin-Madison 1513 University Ave Madison, WI 53706 Advanced Qualification of Additive Manufacturing Materials Workshop, July 20-21, 2015 in Santa Fe, NM Polymer Engineering Center University of

  13. Relativistic Guiding Center Equations

    SciTech Connect (OSTI)

    White, R. B.; Gobbin, M.

    2014-10-01

    In toroidal fusion devices it is relatively easy that electrons achieve relativistic velocities, so to simulate runaway electrons and other high energy phenomena a nonrelativistic guiding center formalism is not sufficient. Relativistic guiding center equations including flute mode time dependent field perturbations are derived. The same variables as used in a previous nonrelativistic guiding center code are adopted, so that a straightforward modifications of those equations can produce a relativistic version.

  14. LANSCE | Lujan Center | Publications

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

    Department of Energy, National Nuclear Security Administration nnsa.energy.gov Publications 2009 Publications Please use the following acknowledgement when publishing results based on data measured at the Lujan Center: "This work has benefited from the use of [add here name of specific Lujan instruments] at the Lujan Center at Los Alamos Neutron Science Center, funded by DOE Office of Basic Energy Sciences. Los Alamos National Laboratory is operated by Los Alamos National Security LLC

  15. Lujan Neutron Scattering Center

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

    responds to radiological incident August 27, 2012 The Laboratory is investigating the inadvertent spread of Technetium 99 by employees and contractors at the Lujan Neutron Scattering Center August 27, 2012-The Laboratory is investigating the inadvertent spread of Technetium 99 by employees and contractors at the Lujan Neutron Scattering Center at the Los Alamos Neutron Science Center (LANSCE), a multidisciplinary accelerator facility used for both civilian and national security research. The

  16. Center for Nonlinear Studies

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

    Center for Nonlinear Studies Center for Nonlinear Studies We conduct and support basic scientific research in nonlinear and complex systems phenomena and promote their use in applied research programs. Contact CNLS Office (505) 667-1444 Email Leader Robert Ecke (505) 667-6733 Email Conducting and supporting basic scientific research in nonlinear and complex systems phenomena The Center for Nonlinear Studies (CNLS) at Los Alamos chooses a small number (two to three) focus topics periodically and

  17. WIPP - Joint Information Center

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

    The Joint Information Center is located at 4021 National Parks Highway in Carlsbad, N.M. Joint Information Center In the unlikely event of an emergency, the WIPP Joint Information Center (JIC) serves as a central control point to coordinate multi-agency efforts to issue timely and accurate information to the public, news media and project employees. Emergency contact information: The public If the JIC is activated, members of the general public, including family members, may call (575) 234-7380

  18. Small cell foams containing a modified dense star polymer or dendrimer as a nucleating agent

    DOE Patents [OSTI]

    Hedstrand, D.M.; Tomalia, D.A.

    1995-02-28

    A small cell foam having a modified dense star polymer or dendrimer is described. This modified dense star polymer or dendrimer has a highly branched interior of one monomeric composition and an exterior structure of a different monomeric composition capable of providing a hydrophobic outer shell and a particle diameter of from about 5 to about 1,000 nm with a matrix polymer.

  19. Small cell foams containing a modified dense star polymer or dendrimer as a nucleating agent

    DOE Patents [OSTI]

    Hedstrand, David M.; Tomalia, Donald A.

    1995-01-01

    A small cell foam having a modified dense star polymer or dendrimer is described. This modified dense star polymer or dendrimer has a highly branched interior of one monomeric composition and an exterior structure of a different monomeric composition capable of providing a hydrophobic outer shell and a particle diameter of from about 5 to about 1,000 nm with a matrix polymer.

  20. Energy Frontier Research Centers

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

    This list is frequently updated and will provide users with the latest information on Center publications. http:science.energy.govbesefrcpublications View all News Items

  1. National Security Education Center

    SciTech Connect (OSTI)

    Hurd, Alan J.

    2015-04-22

    Information about the National Security Education Center is given. Information about the Center’s history and current practices, including its facilities and its practicality are outlined.

  2. NREL: Education Center - Webmaster

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

    to reply. Your name: Your email address: Your message: Send Message Printable Version Education Center Home Hours, Directions & Contact Information Group Programs A Model of...

  3. Data Center Energy Efficiency

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

    Center Energy Efficiency In 2014, data centers in the U.S. con- sumed an estimated 70 billion kWh, 1.8% of total U.S. electricity consump- tion. 1 Thus, it is no surprise that both private and public sector efforts are underway to reduce energy use in data centers. Executive Order (E.O.) 13693 "Planning for Federal Sustain- ability in the Next Decade" outlines the energy efficiency requirements and strategies for federal data centers. The Federal Energy Management Program (FEMP)

  4. Data Center Cooling

    SciTech Connect (OSTI)

    Rutberg, Michael; Cooperman, Alissa; Bouza, Antonio

    2013-10-31

    The article discusses available technologies for reducing energy use for cooling data center facilities. This article addresses the energy savings and market potential of these strategies as well.

  5. Alternative Fuels Data Center

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

    research of national importance at research centers and through the National Biodiesel Board. For more information, see the STRDD Program website. The program is not...

  6. ARM - News Center Archive

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

    CenterNews Center Archive Media Contact Hanna Goss hanna-dot-goss-at-pnnl-dot-gov @armnewsteam Field Notes Blog Topics Field Notes117 AGU 3 AMIE 10 ARM Aerial Facility 2 ARM Mobile Facility 1 7 ARM Mobile Facility 2 47 ARM Mobile Facility 3 1 BAECC 1 BBOP 4 CARES 1 Data Quality Office 2 ENA 2 GOAMAZON 7 HI-SCALE 4 LASIC 3 MAGIC 15 MC3E 17 PECAN 3 SGP 8 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center All Categories Features and

  7. APS Conference Center

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

    combines intellectual stimulation with natural beauty. The Conference Center is within walking distance of the Argonne Guest House, a full-service, professionally-managed hotel and...

  8. Alternative Fuels Data Center

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

    New propane commercial mowers are eligible for 15% of the cost of the equipment. Dedicated propane mower conversions are eligible for 750. New center articulated or oscillating ...

  9. Center of Innovation- Energy

    Broader source: Energy.gov [DOE]

    Jill Stuckey, Director, Center fof Innovation - Energy, presents on Georgia's workforce development opportunities for the Biomass/Clean Cities States Webinar.

  10. BINARIES MIGRATING IN A GASEOUS DISK: WHERE ARE THE GALACTIC CENTER BINARIES?

    SciTech Connect (OSTI)

    Baruteau, C.; Lin, D. N. C.; Cuadra, J. E-mail: lin@ucolick.org

    2011-01-01

    The massive stars in the Galactic center inner arcsecond share analogous properties with the so-called Hot Jupiters. Most of these young stars have highly eccentric orbits and were probably not formed in situ. It has been proposed that these stars acquired their current orbits from the tidal disruption of compact massive binaries scattered toward the proximity of the central supermassive black hole. Assuming a binary star formed in a thin gaseous disk beyond 0.1 pc from the central object, we investigate the relevance of disk-satellite interactions to harden the binding energy of the binary, and to drive its inward migration. A massive, equal-mass binary star is found to become more tightly wound as it migrates inward toward the central black hole. The migration timescale is very similar to that of a single-star satellite of the same mass. The binary's hardening is caused by the formation of spiral tails lagging the stars inside the binary's Hill radius. We show that the hardening timescale is mostly determined by the mass of gas inside the binary's Hill radius and that it is much shorter than the migration timescale. We discuss some implications of the binary's hardening process. When the more massive (primary) components of close binaries eject most their mass through supernova explosion, their secondary stars may attain a range of eccentricities and inclinations. Such processes may provide an alternative unified scenario for the origin of the kinematic properties of the central cluster and S-stars in the Galactic center as well as the high-velocity stars in the Galactic halo.

  11. 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.

  12. 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

  13. 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.

  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. 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...

  20. 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...

  1. 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...

  2. 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.

  3. Energy efficient data centers

    SciTech Connect (OSTI)

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

    2004-03-30

    Data Center facilities, prevalent in many industries and institutions are essential to California's economy. Energy intensive data centers are crucial to California's industries, and many other institutions (such as universities) in the state, and they play an important role in the constantly evolving communications industry. To better understand the impact of the energy requirements and energy efficiency improvement potential in these facilities, the California Energy Commission's PIER Industrial Program initiated this project with two primary focus areas: First, to characterize current data center electricity use; and secondly, to develop a research ''roadmap'' defining and prioritizing possible future public interest research and deployment efforts that would improve energy efficiency. Although there are many opinions concerning the energy intensity of data centers and the aggregate effect on California's electrical power systems, there is very little publicly available information. Through this project, actual energy consumption at its end use was measured in a number of data centers. This benchmark data was documented in case study reports, along with site-specific energy efficiency recommendations. Additionally, other data center energy benchmarks were obtained through synergistic projects, prior PG&E studies, and industry contacts. In total, energy benchmarks for sixteen data centers were obtained. For this project, a broad definition of ''data center'' was adopted which included internet hosting, corporate, institutional, governmental, educational and other miscellaneous data centers. Typically these facilities require specialized infrastructure to provide high quality power and cooling for IT equipment. All of these data center types were considered in the development of an estimate of the total power consumption in California. Finally, a research ''roadmap'' was developed through extensive participation with data center professionals, examination of case

  4. LoanSTAR Revolving Loan Program

    Broader source: Energy.gov [DOE]

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

  5. 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.

  6. 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.

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. ARM - News Center

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

    Center Media Contact Hanna Goss hanna-dot-goss-at-pnnl-dot-gov @armnewsteam Field Notes Blog Topics Field Notes117 AGU 3 AMIE 10 ARM Aerial Facility 2 ARM Mobile Facility 1 7 ARM Mobile Facility 2 47 ARM Mobile Facility 3 1 BAECC 1 BBOP 4 CARES 1 Data Quality Office 2 ENA 2 GOAMAZON 7 HI-SCALE 4 LASIC 3 MAGIC 15 MC3E 17 PECAN 3 SGP 8 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center All Categories Features and Releases Facility

  12. LANSCE | Lujan Center | Publications

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

    0 Publications Please use the following acknowledgement when publishing results based on data measured at the Lujan Center: "This work has benefited from the use of [add here name of specific Lujan instruments] at the Lujan Center at Los Alamos Neutron Science Center, funded by DOE Office of Basic Energy Sciences. Los Alamos National Laboratory is operated by Los Alamos National Security LLC under DOE Contract DE-AC52-06NA25396." Year Citation citation # (as of 06/2013) Instrument 115

  13. LANSCE | Lujan Center | Publications

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

    1 Publications Please use the following acknowledgement when publishing results based on data measured at the Lujan Center: "This work has benefited from the use of [add here name of specific Lujan instruments] at the Lujan Center at Los Alamos Neutron Science Center, funded by DOE Office of Basic Energy Sciences. Los Alamos National Laboratory is operated by Los Alamos National Security LLC under DOE Contract DE-AC52-06NA25396." Year Citation citation # (as of 06/2013) Instrument 244

  14. Star formation trends in the unrelaxed, post-merger cluster A2255

    SciTech Connect (OSTI)

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

    2014-10-10

    The effects of dense environments on normal field galaxies are still up for debate despite much study since Abell published his catalog of nearby clusters in 1958. There are changes in color, morphology, and star formation properties when galaxies fall into groups and clusters, but the specifics of how and where these modifications occur are not fully understood. To look for answers, we focused on star-forming galaxies in A2255, an unrelaxed cluster thought to have recently experienced a merger with another cluster or large group. We used H?, MIPS 24 ?m, and WISE 22 ?m to estimate total star formation rates (SFRs) and Sloan Digital Sky Survey photometry to find stellar masses (M {sub *}) for galaxies out to ?5 r {sub 200}. We compared the star-forming cluster galaxies with the field SFR-mass distribution and found no enhancement or suppression of star formation in currently star-forming galaxies of high mass (log (M {sub *}/M {sub ?}) ? 10). This conclusion holds out to very large distances from the cluster center. However, the core (r {sub proj} < 3 Mpc) has a much lower fraction of star-forming galaxies than anywhere else in the cluster. These results indicate that for the mass range studied here, the majority of the star formation suppression occurs in the core on relatively short timescales, without any enhancement prior to entering the central region. If any significant enhancement or quenching of star formation occurs, it will be in galaxies of lower mass (log (M {sub *}/M {sub ?}) < 10).

  15. Buildings Energy Data Book: 9.1 ENERGY STAR

    Buildings Energy Data Book [EERE]

    2 Home Performance with ENERGY STAR, Completed Jobs Rank Program Sponsor State 1 NY State Energy R&D Authority NY 2 National Grid MA 3 Austin Energy TX 4 Wisconsin Energy Conservation Corp. WI 5 New Jersey Board of Public Utilities NJ 6 Energy Trust of Oregon OR 7 Sacramento Municipal Utility District (1) CA 8 Long Island Power Authority NY 9 Metropolitan Energy Center MO 10 Efficiency Vermont VT Total Note(s): Source(s): Personal communication, Chandler Von Schrader, U.S. EPA, February 10,

  16. Prospects for measuring neutron-star masses and radii with X-ray pulse profile modeling

    SciTech Connect (OSTI)

    Psaltis, Dimitrios; Özel, Feryal; Chakrabarty, Deepto E-mail: fozel@email.arizona.edu

    2014-06-01

    Modeling the amplitudes and shapes of the X-ray pulsations observed from hot, rotating neutron stars provides a direct method for measuring neutron-star properties. This technique constitutes an important part of the science case for the forthcoming NICER and proposed LOFT X-ray missions. In this paper, we determine the number of distinct observables that can be derived from pulse profile modeling and show that using only bolometric pulse profiles is insufficient for breaking the degeneracy between inferred neutron-star radius and mass. However, we also show that for moderately spinning (300-800 Hz) neutron stars, analysis of pulse profiles in two different energy bands provides additional constraints that allow a unique determination of the neutron-star properties. Using the fractional amplitudes of the fundamental and the second harmonic of the pulse profile in addition to the amplitude and phase difference of the spectral color oscillations, we quantify the signal-to-noise ratio necessary to achieve a specified measurement precision for neutron star radius. We find that accumulating 10{sup 6} counts in a pulse profile is sufficient to achieve a ≲ 5% uncertainty in the neutron star radius, which is the level of accuracy required to determine the equation of state of neutron-star matter. Finally, we formally derive the background limits that can be tolerated in the measurements of the various pulsation amplitudes as a function of the system parameters.

  17. 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.

  18. Alternative Fuels Data Center: Biodiesel

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

    Biodiesel Printable Version Share this resource Send a link to Alternative Fuels Data Center: Biodiesel to someone by E-mail Share Alternative Fuels Data Center: Biodiesel on Facebook Tweet about Alternative Fuels Data Center: Biodiesel on Twitter Bookmark Alternative Fuels Data Center: Biodiesel on Google Bookmark Alternative Fuels Data Center: Biodiesel on Delicious Rank Alternative Fuels Data Center: Biodiesel on Digg Find More places to share Alternative Fuels Data Center: Biodiesel on

  19. Alternative Fuels Data Center: Contacts

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

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

  20. Alternative Fuels Data Center: Electricity

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

    Electricity Printable Version Share this resource Send a link to Alternative Fuels Data Center: Electricity to someone by E-mail Share Alternative Fuels Data Center: Electricity on Facebook Tweet about Alternative Fuels Data Center: Electricity on Twitter Bookmark Alternative Fuels Data Center: Electricity on Google Bookmark Alternative Fuels Data Center: Electricity on Delicious Rank Alternative Fuels Data Center: Electricity on Digg Find More places to share Alternative Fuels Data Center:

  1. Alternative Fuels Data Center: Ethanol

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

    Ethanol Printable Version Share this resource Send a link to Alternative Fuels Data Center: Ethanol to someone by E-mail Share Alternative Fuels Data Center: Ethanol on Facebook Tweet about Alternative Fuels Data Center: Ethanol on Twitter Bookmark Alternative Fuels Data Center: Ethanol on Google Bookmark Alternative Fuels Data Center: Ethanol on Delicious Rank Alternative Fuels Data Center: Ethanol on Digg Find More places to share Alternative Fuels Data Center: Ethanol on AddThis.com... More

  2. Alternative Fuels Data Center: Hydrogen

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

    Hydrogen Printable Version Share this resource Send a link to Alternative Fuels Data Center: Hydrogen to someone by E-mail Share Alternative Fuels Data Center: Hydrogen on Facebook Tweet about Alternative Fuels Data Center: Hydrogen on Twitter Bookmark Alternative Fuels Data Center: Hydrogen on Google Bookmark Alternative Fuels Data Center: Hydrogen on Delicious Rank Alternative Fuels Data Center: Hydrogen on Digg Find More places to share Alternative Fuels Data Center: Hydrogen on

  3. Alternative Fuels Data Center: Propane

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

    Vehicles » Propane Printable Version Share this resource Send a link to Alternative Fuels Data Center: Propane to someone by E-mail Share Alternative Fuels Data Center: Propane on Facebook Tweet about Alternative Fuels Data Center: Propane on Twitter Bookmark Alternative Fuels Data Center: Propane on Google Bookmark Alternative Fuels Data Center: Propane on Delicious Rank Alternative Fuels Data Center: Propane on Digg Find More places to share Alternative Fuels Data Center: Propane on

  4. Alternative Fuels Data Center: Tools

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

    Tools to someone by E-mail Share Alternative Fuels Data Center: Tools on Facebook Tweet about Alternative Fuels Data Center: Tools on Twitter Bookmark Alternative Fuels Data Center: Tools on Google Bookmark Alternative Fuels Data Center: Tools on Delicious Rank Alternative Fuels Data Center: Tools on Digg Find More places to share Alternative Fuels Data Center: Tools on AddThis.com... Tools The Alternative Fuels Data Center offers a large collection of helpful tools. These calculators,

  5. Alternative Fuels Data Center: Widgets

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

    Tools Printable Version Share this resource Send a link to Alternative Fuels Data Center: Widgets to someone by E-mail Share Alternative Fuels Data Center: Widgets on Facebook Tweet about Alternative Fuels Data Center: Widgets on Twitter Bookmark Alternative Fuels Data Center: Widgets on Google Bookmark Alternative Fuels Data Center: Widgets on Delicious Rank Alternative Fuels Data Center: Widgets on Digg Find More places to share Alternative Fuels Data Center: Widgets on AddThis.com... Widgets

  6. Alternative Fuels Data Center: Glossary

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

    AFDC Printable Version Share this resource Send a link to Alternative Fuels Data Center: Glossary to someone by E-mail Share Alternative Fuels Data Center: Glossary on Facebook Tweet about Alternative Fuels Data Center: Glossary on Twitter Bookmark Alternative Fuels Data Center: Glossary on Google Bookmark Alternative Fuels Data Center: Glossary on Delicious Rank Alternative Fuels Data Center: Glossary on Digg Find More places to share Alternative Fuels Data Center: Glossary on AddThis.com...

  7. Alternative Fuels Data Center: Webmaster

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

    About Printable Version Share this resource Send a link to Alternative Fuels Data Center: Webmaster to someone by E-mail Share Alternative Fuels Data Center: Webmaster on Facebook Tweet about Alternative Fuels Data Center: Webmaster on Twitter Bookmark Alternative Fuels Data Center: Webmaster on Google Bookmark Alternative Fuels Data Center: Webmaster on Delicious Rank Alternative Fuels Data Center: Webmaster on Digg Find More places to share Alternative Fuels Data Center: Webmaster on

  8. Energy Technology Engineering Center

    Office of Energy Efficiency and Renewable Energy (EERE)

    The Energy Technology Engineering Center (ETEC) is located within Area IV of the Santa Susana Field Laboratory. The ETEC occupies 90-acres within the 290 acre site. The Santa Susana Field...

  9. BPA Visitor Center

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

    and is located at BPA headquarters in Portland, Oregon at 905 NE 11th Ave. (Public Transit @ the Lloyd Center MAX Station). Many of the publications available in the Visitor...

  10. Data center cooling system

    SciTech Connect (OSTI)

    Chainer, Timothy J; Dang, Hien P; Parida, Pritish R; Schultz, Mark D; Sharma, Arun

    2015-03-17

    A data center cooling system may include heat transfer equipment to cool a liquid coolant without vapor compression refrigeration, and the liquid coolant is used on a liquid cooled information technology equipment rack housed in the data center. The system may also include a controller-apparatus to regulate the liquid coolant flow to the liquid cooled information technology equipment rack through a range of liquid coolant flow values based upon information technology equipment temperature thresholds.