National Library of Energy BETA

Sample records for difference star center

  1. 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: F39137 Sampling Dates: 030806 - 030906 Report to: S M Stoller ...

  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: F25409 Sampling Dates: 071304 - 071404 Report to: S M Stoller ...

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

    Office of Legacy Management (LM)

    11 Section 5: Metals Analysis - QC Data Summaries ......Sample Summary S M Stoller Job No: F36361 Star Center-WWNA Monthly; Largo, FL Project No: ...

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

    Office of Legacy Management (LM)

    11 Section 5: Metals Analysis - QC Data Summaries ......Sample Summary S M Stoller Job No: F33038 Star Center-WWNA Monthly; Largo, FL Project No: ...

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

    Office of Legacy Management (LM)

    11 Section 5: Metals Analysis - QC Data Summaries ......Sample Summary S M Stoller Job No: F29623 Star Center-WWNA Monthly; Largo, FL Project No: ...

  6. 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 ...

  7. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    1906 Technical Report for S M Stoller Star Center-B100 110406202 7031-877 Accutest Job Number: F41217 Sampling Date: 060206 Report to: US Dept of Energy, Grand Jct Office 2597 ...

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

    Office of Legacy Management (LM)

    604 Technical Report for S M Stoller Star Center-WWNA Monthly; Largo, FL 110406202 Accutest Job Number: F25242 Sampling Date: 070604 Report to: S M Stoller Cathy.Kelleher@gjo.doe.go...

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

    Office of Legacy Management (LM)

    Test results contained within this data package meet the requirements of the National ... Sample Summary S M Stoller Job No: F30885 Star Center-WWNA Monthly; Largo, FL Project No: ...

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

    Office of Legacy Management (LM)

    Test results contained within this data package meet the requirements of the National ... Sample Summary S M Stoller Job No: F25982 Star Center-WWNA Monthly; Largo, FL Project No: ...

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

    Office of Legacy Management (LM)

    Test results contained within this data package meet the requirements of the National ... Sample Summary S M Stoller Job No: F28014 Star Center-WWNA Monthly; Largo, FL Project No: ...

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

    Office of Legacy Management (LM)

    7 Section 5: GCMS Volatiles - QC Data Summaries ......Sample Summary S M Stoller Job No: F35493 Star Center-B100 MonthlyEffluent; Largo, FL ...

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

    Office of Legacy Management (LM)

    7 Section 5: GCMS Volatiles - QC Data Summaries ......Sample Summary S M Stoller Job No: F29123 Star Center-B100 MonthlyEffluent; Largo, FL ...

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

    Office of Legacy Management (LM)

    Technical Report for S M Stoller Star Center-B100 MonthlyEffluent; Largo, FL 7031-226 Accutest Job Number: F37650 Sampling Date: 010506 Report to: S M Stoller ...

  15. 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: ... Test results contained within this data package meet the requirements of the National ...

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

    Office of Legacy Management (LM)

    STAR Center- 4.5 Acre Site, Largo, FL 7030-226Monthly Accutest Job Number: F27168 ... Test results contained within this data package meet the requirements of the National ...

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

    Office of Legacy Management (LM)

    Test results contained within this data package meet the requirements of the National ... Sample Summary S M Stoller Job No: F30882 Star Center-B100 MonthlyEffluent; Largo, FL ...

  18. 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.

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

    Office of Legacy Management (LM)

    ... a summary of the IRA treatment system performance, and a ... a slight ground water low in the center of the site ... turbidity, and temperature recorded at the time ...

  20. 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.

  1. 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.

  2. 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

  3. 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 » Running on Carver STAR software has been copied from the usual

  4. How ORISE is Making a Difference: Virtual Community Reception Center

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

    Virtual Community Reception Center 3-D virtual training equips health departments for mass casualty radiation emergencies Virtual Community Reception Center The Virtual Community Reception Center. Click Image to launch video. Following a mass casualty radiation emergency, public health professionals will play a crucial role in assessing radiation exposures, screening for radioactive contamination, and prioritizing people for further care. This process-population monitoring-will be conducted in

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

    Office of Legacy Management (LM)

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

  6. 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.

  7. 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.

  8. 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.

  9. CENTER

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

    Science and people highlights from the Lujan Neutron Scattering Center at LANSCE CENTER SCIENCE & PEOPLE the Lujan April 2014 LA-UR-14-22812 I N S I D E 2 Seeking design rules for efficient lighting sources 3 Rate-dependent deformation mechanisms in beryllium 4 Improved understanding of a semiconductor used in infrared detectors 6 Mike Fitzsimmons elected NNSA Fellow 7 Pressure tuning: a new approach for making zero thermal expansion materials 8 Neutron scattering enables structural

  10. 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 and/or bioaugmentation to provide a sustainable remediation system within the flow path of the plume. Additional data will be required to implement this approach and will include: (1) Better delineation of the nature and extent of contamination; (2) Demonstration the plume is currently stable or shrinking; and (3) Demonstration the full reductive dechlorination is occurring. The technical team recommends that DOE use a phased approach to identify residual contamination and to provide rapid installation of remedies. Matrices of characterization and remediation sensors, technologies, and tools were developed by the team in order to match the specific conditions and requirements of the site. The team provides a specific example of remedy that includes the incorporation of a dynamic characterization strategy moving from minimally invasive to more aggressive field techniques, the consideration of multiple complementary remediation approaches based on a spatiotemporally phased approach keyed to the different demands of different parts of the plume, and the integration and sequencing of the characterization and remediation activities.

  11. 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

  12. 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.

  13. 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...

  14. Covered Product Category: Data Center Storage

    Broader source: Energy.gov [DOE]

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

  15. 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...

  16. 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.

  17. 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.

  18. 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.

  19. 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.

  20. 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.

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

    Office of Scientific and Technical Information (OSTI)

    Ames Research Center, we successfully integrated the Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research (4STAR-Air) instrument for flight operation aboard ...

  2. Neutron Star Science with the NuSTAR

    SciTech Connect (OSTI)

    Vogel, J. K.

    2015-10-16

    The Nuclear Spectroscopic Telescope Array (NuSTAR, Figure 1), 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.

  3. 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.

  4. 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.

  5. 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.

  6. Explosives Center

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

    ... Facility Proton Radiography Facility Lujan Neutron Scattering Center Center for Integrated Nanotechnologies Materials Science Laboratory National High Magnetic Field Laboratory ...

  7. 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.

  8. 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.

  9. 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.

  10. 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.

  11. 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.

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

    Office of Scientific and Technical Information (OSTI)

    EXTENDED SCHMIDT LAW: ROLE OF EXISTING STARS IN CURRENT STAR FORMATION Citation Details In-Document Search Title: EXTENDED SCHMIDT LAW: ROLE OF EXISTING STARS IN CURRENT STAR ...

  13. 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

  14. 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...

  15. 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...

  16. 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.

  17. 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

  18. 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.

  19. 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

  20. operations center

    National Nuclear Security Administration (NNSA)

    servers and other critical Operations Center equipment

  21. Independent air supply system filtered to protect against biological and radiological agents (99.7%).
  22. <...

  1. 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...

  2. 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.

  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. 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.

  5. [?/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].

  6. CenterPoint Energy Advanced Residential Lighting Program

    Broader source: Energy.gov [DOE]

    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...

  7. 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.

  8. 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....

  9. Aircraft Integration and Flight Testing of 4STAR (Technical Report) |

    Office of Scientific and Technical Information (OSTI)

    SciTech Connect Technical Report: Aircraft Integration and Flight Testing of 4STAR Citation Details In-Document Search Title: Aircraft Integration and Flight Testing of 4STAR Under funding from the U.S. Dept. of Energy, in conjunction with a funded NASA 2008 ROSES proposal, with internal support from Battelle Pacific Northwest Division (PNWD), and in collaboration with NASA Ames Research Center, we successfully integrated the Spectrometer for Sky-Scanning, Sun-Tracking Atmospheric Research

  10. 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.

  11. 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,

  12. 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...

  13. 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:...

  14. 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.

  15. 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...

  16. 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.

  17. 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 ...

  18. 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.

  19. 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.

  20. 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.

  1. 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)

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

    Office of Legacy Management (LM)

    407-425-0707 * http:www.accutest.com Test results contained within this data package ... 407-425-0707 * http:www.accutest.com Test results contained within this data package ...

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

    Office of Legacy Management (LM)

    407-425-0707 * http:www.accutest.com Test results contained within this data package ... 407-425-0707 * http:www.accutest.com Test results contained within this data package ...

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

    Office of Legacy Management (LM)

    531 Sampling Date: 041604 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 ...

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

    Office of Legacy Management (LM)

    Accutest Job Number: F27229 Sampling Date: 100704 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH ...

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

    Office of Legacy Management (LM)

    227 Sampling Dates: 033104 - 040104 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH E83510), NC ...

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

    Office of Legacy Management (LM)

    Accutest Job Number: F33211 Sampling Dates: 071305 - 071405 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: ...

  8. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    Accutest Job Number: F27169 Sampling Date: 100504 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH ...

  9. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    Accutest Job Number: F33040 Sampling Date: 070605 Report to: S M Stoller Cathy.Kelleher@gjo.doe.gov ATTN: Cathy Kelleher Total number of pages in report: Certifications: FL (DOH ...

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

    Office of Legacy Management (LM)

    124 Sampling Date: 010605 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 ...

  11. S M Stoller Star Center-B100

    Office of Legacy Management (LM)

    ... ALSE is not responsible for any assumptions of data quality if partial data packages are ... with a force of 110mph winds. As a result power was lost at Accutest Labs SE as well as at ...

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

    Office of Legacy Management (LM)

    ... was replaced with an in-situ biosparge treatment system. ... of iron oxidation (3) Low dissolved oxygen and ... turbidity, and temperature recorded at the time ...

  13. 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

  14. 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...

  15. 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:...

  16. 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...

  17. 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...

  18. 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...

  19. 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...

  20. 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...

  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)]

    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

  4. 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

  5. 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

  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)]

    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

  8. 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

  9. 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

  10. 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

  11. 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.

  12. Synthetic guide star generation

    DOE Patents [OSTI]

    Payne, Stephen A. [Castro Valley, CA; Page, Ralph H. [Castro Valley, CA; Ebbers, Christopher A. [Livermore, CA; Beach, Raymond J. [Livermore, CA

    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.

  13. 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.

  14. 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.

  15. 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.

  16. 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,...

  17. 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.

  18. 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.

  19. 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.

  20. 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 multiplicity studies. Our sample is large enough to enable a check of the multiplicity dependence on various physical parameters by analyzing appropriate subsamples. Bluer, more massive stars are seen as more likely to have companions than redder, less massive ones, consistent with the trend seen over the entire spectral range. Systems with larger interaction cross sections, i.e., those with more than two components or long orbital periods, are preferentially younger, suggesting that companions may be stripped over time by dynamical interactions. We confirm the planet-metallicity correlation (i.e., higher metallicity stars are more likely to host planets), but are unable to check it for brown dwarfs due to the paucity of such companions, implying that the brown dwarf desert extends over all separation regimes. We find no correlation between stellar companions and metallicity for B - V < 0.625, but among the redder subset, metal-poor stars ([Fe/H] <-0.3) are more likely to have companions with a 2.4{sigma} significance. The orbital-period distribution of companions is unimodal and roughly log normal with a peak and median of about 300 years. The period-eccentricity relation shows the expected circularization for periods below 12 days, caused by tidal forces over the age of the Galaxy, followed by a roughly flat distribution. The mass-ratio distribution shows a preference for like-mass pairs, which occur more frequently in relatively close pairs. The fraction of planet hosts among single, binary, and multiple systems are statistically indistinguishable, suggesting that planets are as likely to form around single stars as they are around components of binary or multiple systems with sufficiently wide separations. This, along with the preference of long orbital periods among stellar systems, increases the space around stars conducive for planet formation, and perhaps life.

  1. First National Technology Center

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

    ... BYPASS 19 First National Technology First National Technology Center Center System Performance Specifications Fault Clearing Without Grid: 10-15 X Rated Current Overload: 150% ...

  2. 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...

  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. 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...

  5. NJ Clean Energy- ENERGY STAR Appliance Rebate program

    Broader source: Energy.gov [DOE]

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

  6. Extreme neutron stars from Extended Theories of Gravity

    SciTech Connect (OSTI)

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

    2015-01-01

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

  7. A NEAR-INFRARED SURVEY OF THE INNER GALACTIC PLANE FOR WOLF-RAYET STARS. II. GOING FAINTER: 71 MORE NEW W-R STARS

    SciTech Connect (OSTI)

    Shara, Michael M.; Faherty, Jacqueline K.; Zurek, David; Moffat, Anthony F. J.; Doyon, Rene; Gerke, Jill; Artigau, Etienne; Drissen, Laurent E-mail: jfaherty@amnh.org E-mail: moffat@astro.umontreal.ca E-mail: gerke@astronomy.ohio-state.edu E-mail: ldrissen@phy.ulaval.ca

    2012-06-15

    We are continuing a J, K and narrowband imaging survey of 300 deg{sup 2} of the plane of the Galaxy, searching for new Wolf-Rayet (W-R) stars. Our survey spans 150 Degree-Sign in Galactic longitude and reaches 1 Degree-Sign above and below the Galactic plane. The survey has a useful limiting magnitude of K = 15 over most of the observed Galactic plane, and K = 14 (due to severe crowding) within a few degrees of the Galactic center. Thousands of emission-line candidates have been detected. In spectrographic follow-ups of 146 relatively bright W-R star candidates, we have re-examined 11 previously known WC and WN stars and discovered 71 new W-R stars, 17 of type WN and 54 of type WC. Our latest image analysis pipeline now picks out W-R stars with a 57% success rate. Star subtype assignments have been confirmed with the K-band spectra and distances approximated using the method of spectroscopic parallax. Some of the new W-R stars are among the most distant known in our Galaxy. The distribution of these new W-R stars is beginning to trace the locations of massive stars along the distant spiral arms of the Milky Way.

  8. Energy Frontier Research Center Center for Materials Science...

    Office of Scientific and Technical Information (OSTI)

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

  9. 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

  10. tracc-comuting-center-html

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

    Transportation Research and Analysis Computing Center

  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.

  12. 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

  13. 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.

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

    SciTech Connect (OSTI)

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

    2014-03-16

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

  15. 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...

  16. 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.

  17. 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.

  18. ARM - News Center

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

    SGP 6 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center All Categories Features and Releases Facility News Field...

  19. ARM - News Center Archive

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

    SGP 6 STORMVEX 29 TCAP 3 Search News Search Blog News Center All Categories What's this? Social Media Guidance News Center All Categories Features and Releases Facility News Field...

  20. 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...

  1. Energy Frontier Research Centers

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

    Fuels (Technical Report) | SciTech Connect Technical Report: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Citation Details In-Document Search Title: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Scientific Successes * The first phonon density of states (PDOS) measurements for UO2 to include anharmonicity were obtained using time-of-flight inelastic neutron scattering at the Spallation Neutron Source (SNS), and an innovative,

  2. 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 Education Center phone number is 303-384-6565. June 2016 Sustainable NREL Walking Campus Tour June 17, 2016, 9:30 - 11:15 am Golden, CO Contact: NREL Education Center 303-384-6565 NREL exemplifies environmental sustainability throughout its operations. Visitors learn about renewable energy and energy efficiency research as

  3. 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...

  4. Center for Nanoscale Materials

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

    National 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

  5. 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

  6. 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.

  7. 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

  8. 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.

  9. 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...

  10. 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

  11. 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.

  12. 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...

  13. 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...

  14. 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...

  15. 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...

  16. 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,...

  17. 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.

  18. 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

  19. 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.

  20. 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

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

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

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

  2. 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.

  3. LANSCE | Lujan Center | Data Management

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

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

  4. 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.

  5. 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

  6. 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.

  7. 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

  8. 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

  9. 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...

  10. 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...

  11. 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...

  12. 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

  13. 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.

  14. LANSCE | Lujan Center | Highlights

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

    * Julian Chen, new Protein Crystallography Station lead scientist, carving out elite niche: neutron studies of membrane proteins The Lujan Center Science & People October...

  15. 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...

  16. Extreme Environments (EFree) Center

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

    Extreme Environments (EFree ) Center LLNL Co-PI: Jonathon Crowhurst e-mail bio Novel materials for energy applications Ultrafast reflectivity measurements under high pressure...

  17. 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.

  18. Center for Nonlinear Studies

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

    Center for Nonlinear Studies We conduct and support basic scientific research in nonlinear and ... into consideration both the Lab's needs for basic science relevant to ...

  19. Polymer Engineering Center

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

    ... * DEA is suitable for online- measurements of phase transitions in composite manufacturing Conclusions Summary Polymer Engineering Center University of Wisconsin-Madison Prof. ...

  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. 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...

  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. 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 ? 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 2.5kpc< R {sub M31}< 117kpc. We find a range of [Fe/H] within 20kpc 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 5Gyr. The ?-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.

  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. 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 study findings, and participation in data center industry meetings and workshops. Industry partners enthusiastically provided valuable insight into current practice, and helped to identify areas where additional public interest research could lead to significant efficiency improvement. This helped to define and prioritize the research agenda. The interaction involved industry representatives with expertise in all aspects of data center facilities, including specialized facility infrastructure systems and computing equipment. In addition to the input obtained through industry workshops, LBNL's participation in a three-day, comprehensive design ''charrette'' hosted by the Rocky Mountain Institute (RMI) yielded a number of innovative ideas for future research.

  6. 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.

  7. 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

  8. 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

  9. LANSCE | Lujan Center | Publications

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

    2 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 373

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

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

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

  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. 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

  13. 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...

  14. 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:

  15. 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

  16. 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

  17. 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

  18. 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,

  19. 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

  20. 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...

  1. 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

  2. Alternative Fuels Data Center: Disclaimer

    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: Disclaimer to someone by E-mail Share Alternative Fuels Data Center: Disclaimer on Facebook Tweet about Alternative Fuels Data Center: Disclaimer on Twitter Bookmark Alternative Fuels Data Center: Disclaimer on Google Bookmark Alternative Fuels Data Center: Disclaimer on Delicious Rank Alternative Fuels Data Center: Disclaimer on Digg Find More places to share Alternative Fuels Data Center: Disclaimer on

  3. 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.

  4. 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.

  5. 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...

  6. 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...

  7. WIPP Information Center

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

    the Skeen-Whitlock Building in Carlsbad. The WIPP Experience Exhibit at 4021 National Parks Highway in Carlsbad, N.M. WIPP Information Center Address: 4021 National Parks Highway...

  8. Energy Security Center

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

    Energy Security Center Energy Security Center Developing new ideas for reliable, secure, and sustainable carbon neutral energy solutions for the nation-the portal to LANL's diverse energy security research enterprise. Contact Leader Steven Buelow (505) 663 5629 Email Program Administrator Jutta Kayser (505) 663-5649 Email Research focus areas Materials and concepts for clean energy Science for renewable energy sources Superconducting cables Energy storage Fuel cells Mitigating impacts of global

  9. Center for Nonlinear Studies

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

    NSEC » Center for Nonlinear Studies Center for Nonlinear Studies Serving as an interface between mission critical research at LANL and the outside research community. Contact Director Robert Ecke (505) 667-6733 Email Deputy Director Aric Hagberg (505) 665-4958 Email Executive Administrator Elissa (Ellie) Vigil (505) 667-2818 Email Identify and study complex nonlinear phenomena using a diverse set of research approaches and methodologies, particularly those of statistical physics, nonlinear

  10. Data center cooling system

    DOE Patents [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.

  11. LANSCE | Lujan Center | Publications

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

    Publications Lujan Publications: 2009 - 2012 2012 | 2011 | 2010 | 2009 Publication acknowledgement Lujan Center monitors the number of papers published as a result of the use of our facilities. The Lujan Center's sponsoring agencies requires users to publish results from their non proprietary research. Authorship of publications based on research from user facilities should reflect the normal considerations of recognizing collaborations. Proprietary users are not required to publish. Users are

  12. 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.

  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 Frontier Research Center Center for Materials Science...

    Office of Scientific and Technical Information (OSTI)

    Technical Report: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Citation ... dispersion, and, further, that advanced lattice dynamics simulations ...

  16. 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.

  17. 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...

  18. 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.

  19. 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.

  20. NorthStar Medical Technologies LLC

    National Nuclear Security Administration (NNSA)

    ... of a linear accelerator (linac) and chemical processing facility (the NorthStar ... Using the funding provided by NNSA, NorthStar proposes to construct a linac and chemical ...

  1. 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.

  2. 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...

  3. 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...

  4. 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...

  5. Alternative Fuels Data Center: Publications

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

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

  6. Alternative Fuels Data Center: Biobutanol

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

    Biobutanol to someone by E-mail Share Alternative Fuels Data Center: Biobutanol on Facebook Tweet about Alternative Fuels Data Center: Biobutanol on Twitter Bookmark Alternative Fuels Data Center: Biobutanol on Google Bookmark Alternative Fuels Data Center: Biobutanol on Delicious Rank Alternative Fuels Data Center: Biobutanol on Digg Find More places to share Alternative Fuels Data Center: Biobutanol on AddThis.com... More in this section... Biobutanol Dimethyl Ether Methanol Renewable

  7. Alternative Fuels Data Center: Methanol

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

    Methanol to someone by E-mail Share Alternative Fuels Data Center: Methanol on Facebook Tweet about Alternative Fuels Data Center: Methanol on Twitter Bookmark Alternative Fuels Data Center: Methanol on Google Bookmark Alternative Fuels Data Center: Methanol on Delicious Rank Alternative Fuels Data Center: Methanol on Digg Find More places to share Alternative Fuels Data Center: Methanol on AddThis.com... More in this section... Biobutanol Dimethyl Ether Methanol Renewable Hydrocarbon Biofuels

  8. Alternative Fuels Data Center: Newsletters

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

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

  9. Alternative Fuels Data Center: Ridesharing

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

    Ridesharing to someone by E-mail Share Alternative Fuels Data Center: Ridesharing on Facebook Tweet about Alternative Fuels Data Center: Ridesharing on Twitter Bookmark Alternative Fuels Data Center: Ridesharing on Google Bookmark Alternative Fuels Data Center: Ridesharing on Delicious Rank Alternative Fuels Data Center: Ridesharing on Digg Find More places to share Alternative Fuels Data Center: Ridesharing on AddThis.com... More in this section... Idle Reduction Parts & Equipment

  10. Alternative Fuels Data Center: Publications

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

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

  11. 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.

  12. 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.

  13. 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.

  14. 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.

  15. LoanSTAR Revolving Loan Program

    Broader source: Energy.gov [DOE]

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

  16. 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.

  17. Neutron Science Center

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

    Public to have rare opportunity to tour Neutron Science Center May 10, 2011 LANL Rosenfest will celebrate life of LANSCE founder Louis Rosen and offer tour LOS ALAMOS, New Mexico, May 10, 2011-Members of the public will have an unusual opportunity to tour the Los Alamos Neutron Science Center from 1 to 5 p.m. on Friday, May 20, 2011, as part of Rosenfest, a celebration of LANSCE founder Louis - 2 - Rosen and the remarkable facility he conceived. In addition, Rosenfest organizers are offering a

  18. DOE New Research Center

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

    is Part of New Research Center to do Energy Research at LSU The Department of Energy has awarded LSU a $12.5 million grant to set up an Energy Frontier Research Center (EFRC) to find greener and better sources of energy as efficient substitutes for fossil fuel. The EFRC will be headed by Jerry Spivey, McLaurin Shivers Professor of Chemical Engineering at LSU. His team will consist of 21 researchers from across nine institutions. The multi-disciplinary research project will utilize, among other

  19. Center for Advanced Photophysics | Science

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

    Los Alamos National Laboratory National Renewable Energy Laboratory U.S. Department of Energy Home About The Center Science Members Publications News & Press Releases Center...

  20. Learning Center | Argonne National Laboratory

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

    Argonne Learning Center The Argonne Learning Center contains four student research laboratories, three learning classrooms and a historic 1960's control room facility where...

  1. Data Center Economizer Contamination and Humidity Study

    SciTech Connect (OSTI)

    Shehabi, Arman; Tschudi, William; Gadgil, Ashok

    2007-03-06

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

  2. 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,

  3. 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.

  4. 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).

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

    SciTech Connect (OSTI)

    Psaltis, Dimitrios; zel, 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.

  6. Alternative Fuels Data Center

    SciTech Connect (OSTI)

    2013-06-01

    Fact sheet describes the Alternative Fuels Data Center, which provides information, data, and tools to help fleets and other transportation decision makers find ways to reduce petroleum consumption through the use of alternative and renewable fuels, advanced vehicles, and other fuel-saving measures.

  7. Carolinas Energy Career Center

    SciTech Connect (OSTI)

    Classens, Anver; Hooper, Dick; Johnson, Bruce

    2013-03-31

    Central Piedmont Community College (CPCC), located in Charlotte, North Carolina, established the Carolinas Energy Career Center (Center) - a comprehensive training entity to meet the dynamic needs of the Charlotte region's energy workforce. The Center provides training for high-demand careers in both conventional energy (fossil) and renewable energy (nuclear and solar technologies/energy efficiency). CPCC completed four tasks that will position the Center as a leading resource for energy career training in the Southeast: Development and Pilot of a New Advanced Welding Curriculum, Program Enhancement of Non-Destructive Examination (NDE) Technology, Student Support through implementation of a model targeted toward Energy and STEM Careers to support student learning, Project Management and Reporting. As a result of DOE funding support, CPCC achieved the following outcomes: Increased capacity to serve and train students in emerging energy industry careers; Developed new courses and curricula to support emerging energy industry careers; Established new training/laboratory resources; Generated a pool of highly qualified, technically skilled workers to support the growing energy industry sector.

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

    SciTech Connect (OSTI)

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

    2012-08-01

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

  9. THE ORIGIN OF HVS17, AN UNBOUND MAIN SEQUENCE B STAR AT 50 kpc

    SciTech Connect (OSTI)

    Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.; Cohen, Judith G. E-mail: mgeller@cfa.harvard.edu E-mail: jlc@astro.caltech.edu

    2013-09-20

    We analyze Keck Echellette Spectrograph and Imager spectroscopy of HVS17, a B-type star traveling with a Galactic rest frame radial velocity of +445 km s{sup 1} in the outer halo of the Milky Way. HVS17 has the projected rotation of a main sequence B star and is chemically peculiar, with solar iron abundance and sub-solar alpha abundance. Comparing measured T{sub eff} and log g with stellar evolution tracks implies that HVS17 is a 3.91 0.09 M{sub ?}, 153 9 Myr old star at a Galactocentric distance of r = 48.5 4.6 kpc. The time between its formation and ejection significantly exceeds 10 Myr and thus is difficult to reconcile with any Galactic disk runaway scenario involving massive stars. The observations are consistent, on the other hand, with a hypervelocity star ejection from the Galactic center. We show that Gaia proper motion measurements will easily discriminate between a disk and Galactic center origin, thus allowing us to use HVS17 as a test particle to probe the shape of the Milky Way's dark matter halo.

  10. Ultrafaint dwarfs—star formation and chemical evolution in the smallest galaxies

    SciTech Connect (OSTI)

    Webster, David; Bland-Hawthorn, Joss; Sutherland, Ralph

    2014-11-20

    In earlier work, we showed that a dark matter halo with a virial mass of 10{sup 7} M {sub ☉} can retain a major part of its baryons in the face of the pre-ionization phase and supernova (SN) explosion from a 25 M {sub ☉} star. Here, we expand on the results of that work, investigating the star formation and chemical evolution of the system beyond the first SN. In a galaxy with a mass M {sub vir} = 10{sup 7} M {sub ☉}, sufficient gas is retained by the potential for a second period of star formation to occur. The impact of a central explosion is found to be much stronger than that of an off-center explosion both in blowing out the gas and in enriching it, as in the off-center case most of the SN energy and metals escape into the intergalactic medium. We model the star formation and metallicity, given the assumption that stars form for 100, 200, 400, and 600 Myr, and discuss the results in the context of recent observations of very low-mass galaxies. We show that we can account for most features of the observed relationship between [α/Fe] and [Fe/H] in ultra-faint dwarf galaxies with the assumption that the systems formed at a low mass, rather than being remnants of much larger systems.

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

    Broader source: Energy.gov [DOE]

    Washington, DC - On January 25th, the General Counsel notified 25 manufacturers that the Department of Energy has withdrawn their right to use the Energy Star label on 34 different models of...

  12. PNNL Electricity Infrastructure Operations Center | Open Energy...

    Open Energy Info (EERE)

    Electricity Infrastructure Operations Center Jump to: navigation, search Logo: Electricity Infrastructure Operations Center Name Electricity Infrastructure Operations Center...

  13. YOUNG STARS IN AN OLD BULGE: A NATURAL OUTCOME OF INTERNAL EVOLUTION IN THE MILKY WAY

    SciTech Connect (OSTI)

    Ness, M.; Debattista, Victor P.; Cole, D. R.; Bensby, T.; Feltzing, S.; Roškar, R.; Johnson, J. A.; Freeman, K.

    2014-06-01

    The center of our disk galaxy, the Milky Way, is dominated by a boxy/peanut-shaped bulge. Numerous studies of the bulge based on stellar photometry have concluded that the bulge stars are exclusively old. The perceived lack of young stars in the bulge strongly constrains its likely formation scenarios, providing evidence that the bulge is a unique population that formed early and separately from the disk. However, recent studies of individual bulge stars using the microlensing technique have reported that they span a range of ages, emphasizing that the bulge may not be a monolithic structure. In this Letter we demonstrate that the presence of young stars that are located predominantly nearer to the plane is expected for a bulge that has formed from the disk via dynamical instabilities. Using an N-body+ smoothed particle hydrodynamics simulation of a disk galaxy forming out of gas cooling inside a dark matter halo and forming stars, we find a qualitative agreement between our model and the observations of younger metal-rich stars in the bulge. We are also able to partially resolve the apparent contradiction in the literature between results that argue for a purely old bulge population and those that show a population comprised of a range in ages; the key is where to look.

  14. Super massive black hole in galactic nuclei with tidal disruption of stars

    SciTech Connect (OSTI)

    Zhong, Shiyan; Berczik, Peter; Spurzem, Rainer

    2014-09-10

    Tidal disruption of stars by super massive central black holes from dense star clusters is modeled by high-accuracy direct N-body simulation. The time evolution of the stellar tidal disruption rate, the effect of tidal disruption on the stellar density profile, and, for the first time, the detailed origin of tidally disrupted stars are carefully examined and compared with classic papers in the field. Up to 128k particles are used in simulation to model the star cluster around a super massive black hole, and we use the particle number and the tidal radius of the black hole as free parameters for a scaling analysis. The transition from full to empty loss-cone is analyzed in our data, and the tidal disruption rate scales with the particle number, N, in the expected way for both cases. For the first time in numerical simulations (under certain conditions) we can support the concept of a critical radius of Frank and Rees, which claims that most stars are tidally accreted on highly eccentric orbits originating from regions far outside the tidal radius. Due to the consumption of stars moving on radial orbits, a velocity anisotropy is found inside the cluster. Finally we estimate the real galactic center based on our simulation results and the scaling analysis.

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

    SciTech Connect (OSTI)

    Harwit, Martin; Brisbin, Drew

    2015-02-20

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

  16. Thurston Energy Outreach Center

    SciTech Connect (OSTI)

    Pierce, P.; Young, M.

    1984-09-01

    In Olympia, the Washington Energy Extension Service program is provided by the Olympic Renewable Resources Association's Energy Outreach Center. The Center has provided Thurston County residents with consistent and reliable information on energy conservation and renewable resources since 1980. During those four years, a seasonal pattern of activities has developed which reflects strong shifts in class attendance and inquiries by EOC users over the course of the year. Classes include: design of superinsulated passive solar and earth sheltered homes; sunspace design, coldframe construction and tax credits for solar energy systems; caulking, weatherstripping, storm windows and chimney cleaning; and solar and wood hot water systems. All are scheduled according to dictates of seasonal needs and interests.

  17. National Training Center | Department of Energy

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

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

  18. Center for Functional Nanomaterials

    ScienceCinema (OSTI)

    BNL

    2009-09-01

    Staff from Brookhaven's new Center for Functional Nanomaterials (CFN) describe how this advanced facility will focus on the development and understanding of nanoscale materials. The CFN provides state-of-the-art capabilities for the fabrication and study of nanoscale materials, with an emphasis on atomic-level tailoring to achieve desired properties and functions. The overarching scientific theme of the CFN is the development and understanding of nanoscale materials that address the Nation's challenges in energy security.

  19. Center for Integrated Nanotechnologies

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

    ADEPS » MPA » MPA-CINT Center for Integrated Nanotechnologies Nanomaterials integration is one of many approaches we take in addressing a range of challenges, from human health to national defense. Contact Us CINT Co-Director Quanxi Jia Email Deputy Group Leader (acting) Alex Lacerda Email Group Office (505) 667-9243 First in-situ images of void collapse in explosives Los Alamos researchers and collaborators demonstrated a crucial diagnostic for studying how voids affect explosives under shock

  20. Doyle Conservation Center (DCC)

    High Performance Buildings Database

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

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

    SciTech Connect (OSTI)

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

    2005-06-01

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

  2. On the capture of dark matter by neutron stars

    SciTech Connect (OSTI)

    Gver, Tolga; Erkoca, Arif Emre; Sarcevic, Ina; Reno, Mary Hall E-mail: aeerkoca@gmail.com E-mail: ina@physics.arizona.edu

    2014-05-01

    We calculate the number of dark matter particles that a neutron star accumulates over its lifetime as it rotates around the center of a galaxy, when the dark matter particle is a self-interacting boson but does not self-annihilate. We take into account dark matter interactions with baryonic matter and the time evolution of the dark matter sphere as it collapses within the neutron star. We show that dark matter self-interactions play an important role in the rapid accumulation of dark matter in the core of the neutron star. We consider the possibility of determining an exclusion region of the parameter space for dark matter mass and dark matter interaction cross section with the nucleons as well as dark matter self-interaction cross section, based on the observation of old neutron stars. We show that for a dark matter density of 10{sup 3} GeV/cm{sup 3}and dark matter mass m{sub ?} ?< 10 GeV, there is a potential exclusion region for dark matter interactions with nucleons that is three orders of magnitude more stringent than without self-interactions. The potential exclusion region for dark matter self-interaction cross sections is many orders of magnitude stronger than the current Bullet Cluster limit. For example, for high dark matter density regions, we find that for m{sub ?} ? 10 GeV when the dark matter interaction cross section with the nucleons ranges from ?{sub ?n} ? 10{sup ?52} cm{sup 2} to ?{sub ?n} ? 10{sup ?57} cm{sup 2}, the dark matter self-interaction cross section limit is ?{sub ??} ?< 10{sup ?33} cm{sup 2}, which is about ten orders of magnitude stronger than the Bullet Cluster limit.

  3. Energy Frontier Research Center Center for Materials Science of Nuclear

    Office of Scientific and Technical Information (OSTI)

    Fuels (Technical Report) | SciTech Connect Frontier Research Center Center for Materials Science of Nuclear Fuels Citation Details In-Document Search Title: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Scientific Successes * The first phonon density of states (PDOS) measurements for UO2 to include anharmonicity were obtained using time-of-flight inelastic neutron scattering at the Spallation Neutron Source (SNS), and an innovative, experimental-based

  4. Energy Frontier Research Center Center for Materials Science of Nuclear

    Office of Scientific and Technical Information (OSTI)

    Fuels (Technical Report) | SciTech Connect Technical Report: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Citation Details In-Document Search Title: Energy Frontier Research Center Center for Materials Science of Nuclear Fuels Scientific Successes * The first phonon density of states (PDOS) measurements for UO2 to include anharmonicity were obtained using time-of-flight inelastic neutron scattering at the Spallation Neutron Source (SNS), and an innovative,

  5. Solar Technology Center

    SciTech Connect (OSTI)

    Boehm, Bob

    2011-04-27

    The Department of Energy, Golden Field Office, awarded a grant to the UNLV Research Foundation (UNLVRF) on August 1, 2005 to develop a solar and renewable energy information center. The Solar Technology Center (STC) is to be developed in two phases, with Phase I consisting of all activities necessary to determine feasibility of the project, including design and engineering, identification of land access issues and permitting necessary to determine project viability without permanently disturbing the project site, and completion of a National Environmental Policy Act (NEPA) Environmental Assessment. Phase II is the installation of infrastructure and related structures, which leads to commencement of operations of the STC. The STC is located in the Boulder City designated 3,000-acre Eldorado Valley Energy Zone, approximately 15 miles southwest of downtown Boulder City and fronting on Eldorado Valley Drive. The 33-acre vacant parcel has been leased to the Nevada Test Site Development Corporation (NTSDC) by Boulder City to accommodate a planned facility that will be synergistic with present and planned energy projects in the Zone. The parcel will be developed by the UNLVRF. The NTSDC is the economic development arm of the UNLVRF. UNLVRF will be the entity responsible for overseeing the lease and the development project to assure compliance with the lease stipulations established by Boulder City. The STC will be operated and maintained by University of Nevada, Las Vegas (UNLV) and its Center for Energy Research (UNLV-CER). Land parcels in the Eldorado Valley Energy Zone near the 33-acre lease are committed to the construction and operation of an electrical grid connected solar energy production facility. Other projects supporting renewable and solar technologies have been developed within the energy zone, with several more developments in the horizon.

  6. NREL: Education Center - Webmaster

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

    Webmaster To contact the Webmaster, please provide your name, e-mail address, and message below. When you are finished, click "Send Message." NOTE: If you enter your e-mail address incorrectly, we will be unable 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 Energy-Efficient Design Did you find what you needed? Yes 1 No 0 Thank you for your feedback. Would

  7. Valley Forge Corporate Center

    Energy Savers [EERE]

    55 Jefferson Ave. Valley Forge Corporate Center Norristown, PA 19403-2497 Pauline Foley Assistant General Counsel 610.666.8248 | Fax - 610.666.8211 foleyp@pjm.com October 30, 2013 Via Electronic Mail: juliea.smith@hq.doe.gov Christopher.lawrence@hq.doe.gov Julie A. Smith Office of Electricity Delivery and Energy Reliability Mail Code: OE-20 U.S. Department of Energy 1000 Independence Avenue, SW Washington, D.C. 20585 Re: Department of Energy - Improving Performance of Federal Permitting and

  8. COMPUTATIONAL SCIENCE CENTER

    SciTech Connect (OSTI)

    DAVENPORT, J.

    2005-11-01

    The Brookhaven Computational Science Center brings together researchers in biology, chemistry, physics, and medicine with applied mathematicians and computer scientists to exploit the remarkable opportunities for scientific discovery which have been enabled by modern computers. These opportunities are especially great in computational biology and nanoscience, but extend throughout science and technology and include, for example, nuclear and high energy physics, astrophysics, materials and chemical science, sustainable energy, environment, and homeland security. To achieve our goals we have established a close alliance with applied mathematicians and computer scientists at Stony Brook and Columbia Universities.

  9. Providence Newberg Medical Center

    High Performance Buildings Database

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

  10. Alternative Fuels Data Center

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

    Do alternative fuel vehicles (AFVs) improve air quality? How does the use of alternative fuels affect smog formation? You may find answers to these and other questions through the U.S. Department of Energy's (DOE) Alternative Fuels Data Center (AFDC)-the nation's most com- prehensive repository of perfor- mance data and general informa- tion on AFVs. To date, more than 600 vehi- cles-including light-duty cars, trucks, vans, transit buses, and heavy-duty trucks-have been tested on various

  11. Alternative Fuels Data Center

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

    Natural Gas Vehicle (NGV) and Fueling Infrastructure Rebates - Texas Gas Service The Texas Gas Service Conservation Program offers a rebate of up to $2,000 for the purchase of a qualified NGV or $3,000 for the conversion of a gasoline powered vehicle to operate on natural gas. The rebate is available for up to five vehicles per customer, and only centers certified by the Railroad Commission of Texas may perform conversions. A rebate of $1,000 is also available for the purchase of a natural gas

  12. Storage and Assay of Tritium in STAR

    SciTech Connect (OSTI)

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

    2005-07-15

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

  13. Carbon-enhanced metal-poor stars: CEMP-s and CEMP-no subclasses in the halo system of the Milky Way

    SciTech Connect (OSTI)

    Carollo, Daniela; Freeman, Ken; Beers, Timothy C.; Placco, Vinicius M.; Tumlinson, Jason; Martell, Sarah L. E-mail: kcf@mso.anu.edu.au E-mail: vplacco@gemini.edu E-mail: smartell@aao.gov.au

    2014-06-20

    We explore the kinematics and orbital properties of a sample of 323 very metal-poor stars in the halo system of the Milky Way, selected from the high-resolution spectroscopic follow-up studies of Aoki et al. and Yong et al. The combined sample contains a significant fraction of carbon-enhanced metal-poor (CEMP) stars (22% or 29%, depending on whether a strict or relaxed criterion is applied for this definition). Barium abundances (or upper limits) are available for the great majority of the CEMP stars, allowing for their separation into the CEMP-s and CEMP-no subclasses. A new method to assign membership to the inner- and outer-halo populations of the Milky Way is developed, making use of the integrals of motion, and applied to determine the relative fractions of CEMP stars in these two subclasses for each halo component. Although limited by small-number statistics, the data suggest that the inner halo of the Milky Way exhibits a somewhat higher relative number of CEMP-s stars than CEMP-no stars (57% versus 43%), while the outer halo possesses a clearly higher fraction of CEMP-no stars than CEMP-s stars (70% versus 30%). Although larger samples of CEMP stars with known Ba abundances are required, this result suggests that the dominant progenitors of CEMP stars in the two halo components were different; massive stars for the outer halo, and intermediate-mass stars in the case of the inner halo.

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

    Broader source: Energy.gov [DOE]

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

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

    Broader source: Energy.gov [DOE]

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

  16. Data center coolant switch

    SciTech Connect (OSTI)

    Iyengar, Madhusudan K.; Parida, Pritish R.; Schultz, Mark D.

    2015-10-06

    A data center cooling system is operated in a first mode; it has an indoor portion wherein heat is absorbed from components in the data center, and an outdoor heat exchanger portion wherein outside air is used to cool a first heat transfer fluid (e.g., water) present in at least the outdoor heat exchanger portion of the cooling system during the first mode. The first heat transfer fluid is a relatively high performance heat transfer fluid (as compared to the second fluid), and has a first heat transfer fluid freezing point. A determination is made that an appropriate time has been reached to switch from the first mode to a second mode. Based on this determination, the outdoor heat exchanger portion of the data cooling system is switched to a second heat transfer fluid, which is a relatively low performance heat transfer fluid, as compared to the first heat transfer fluid. It has a second heat transfer fluid freezing point lower than the first heat transfer fluid freezing point, and the second heat transfer fluid freezing point is sufficiently low to operate without freezing when the outdoor air temperature drops below a first predetermined relationship with the first heat transfer fluid freezing point.

  17. Information Center | Department of Energy

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

    Center Information Center The U.S. Department of Energy's (DOE) Office of Enterprise Assessments (EA) provides expert evaluations of management performance in safety, security and other areas by seasoned experts who are independent of line management. Information related to enforcement, safety, security, emergency management and cyber performance management is made available to the public in the EA Information Center. Enforcement Info Center The Department's Enforcement Office conducts

  18. Rapid cooling and structure of neutron stars

    SciTech Connect (OSTI)

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

    1992-07-01

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

  19. Rapid cooling and structure of neutron stars

    SciTech Connect (OSTI)

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

    1992-01-01

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

  20. William Fowler and Elements in the Stars

    Office of Scientific and Technical Information (OSTI)

    in physics for his research into the creation of chemical elements inside stars ... . ... reactions--how the nuclei of lighter chemical elements fuse to create the heavier ones ...

  1. Energy Star Rebate Finder | Open Energy Information

    Open Energy Info (EERE)

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

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

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

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

  3. Star Energy Systems | Open Energy Information

    Open Energy Info (EERE)

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

  4. Lone Star Transmission LLC | Open Energy Information

    Open Energy Info (EERE)

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

  5. Green Star Alternative Energy | Open Energy Information

    Open Energy Info (EERE)

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

  6. Blue Star Energy Services | Open Energy Information

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

  8. Green Star Energy LLC | Open Energy Information

    Open Energy Info (EERE)

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

  9. RegenaStar | Open Energy Information

    Open Energy Info (EERE)

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

  10. Data Center Airflow Management Retrofit

    Broader source: Energy.gov [DOE]

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

  11. COMPUTATIONAL SCIENCE CENTER

    SciTech Connect (OSTI)

    DAVENPORT, J.

    2006-11-01

    Computational Science is an integral component of Brookhaven's multi science mission, and is a reflection of the increased role of computation across all of science. Brookhaven currently has major efforts in data storage and analysis for the Relativistic Heavy Ion Collider (RHIC) and the ATLAS detector at CERN, and in quantum chromodynamics. The Laboratory is host for the QCDOC machines (quantum chromodynamics on a chip), 10 teraflop/s computers which boast 12,288 processors each. There are two here, one for the Riken/BNL Research Center and the other supported by DOE for the US Lattice Gauge Community and other scientific users. A 100 teraflop/s supercomputer will be installed at Brookhaven in the coming year, managed jointly by Brookhaven and Stony Brook, and funded by a grant from New York State. This machine will be used for computational science across Brookhaven's entire research program, and also by researchers at Stony Brook and across New York State. With Stony Brook, Brookhaven has formed the New York Center for Computational Science (NYCCS) as a focal point for interdisciplinary computational science, which is closely linked to Brookhaven's Computational Science Center (CSC). The CSC has established a strong program in computational science, with an emphasis on nanoscale electronic structure and molecular dynamics, accelerator design, computational fluid dynamics, medical imaging, parallel computing and numerical algorithms. We have been an active participant in DOES SciDAC program (Scientific Discovery through Advanced Computing). We are also planning a major expansion in computational biology in keeping with Laboratory initiatives. Additional laboratory initiatives with a dependence on a high level of computation include the development of hydrodynamics models for the interpretation of RHIC data, computational models for the atmospheric transport of aerosols, and models for combustion and for energy utilization. The CSC was formed to bring together researchers in these areas and to provide a focal point for the development of computational expertise at the Laboratory. These efforts will connect to and support the Department of Energy's long range plans to provide Leadership class computing to researchers throughout the Nation. Recruitment for six new positions at Stony Brook to strengthen its computational science programs is underway. We expect some of these to be held jointly with BNL.

  12. Atmospheric parameters and metallicities for 2191 stars in the globular cluster M4

    SciTech Connect (OSTI)

    Malavolta, Luca; Piotto, Giampaolo; Nascimbeni, Valerio; Sneden, Christopher; Milone, Antonino P.; Bedin, Luigi R. E-mail: giampaolo.piotto@unipd.it E-mail: luigi.bedin@oapd.inaf.it E-mail: milone@mso.anu.edu.au

    2014-02-01

    We report new metallicities for stars of Galactic globular cluster M4 using the largest number of stars ever observed at high spectral resolution in any cluster. We analyzed 7250 spectra for 2771 cluster stars gathered with the Very Large Telescope (VLT) FLAMES+GIRAFFE spectrograph at VLT. These medium-resolution spectra cover a small wavelength range, and often have very low signal-to-noise ratios. We approached this data set by reconsidering the whole method of abundance analysis of large stellar samples from beginning to end. We developed a new algorithm that automatically determines the atmospheric parameters of a star. Nearly all of the data preparation steps for spectroscopic analyses are processed on the syntheses, not the observed spectra. For 322 red giant branch (RGB) stars with V ≤ 14.7, we obtain a nearly constant metallicity, ([Fe/H]) = –1.07 (σ = 0.02). No difference in the metallicity at the level of 0.01 dex is observed between the two RGB sequences identified by Monelli et al. For 1869 subgiant and main-sequence stars with V > 14.7, we obtain ([Fe/H]) = –1.16 (σ = 0.09) after fixing the microturbulent velocity. These values are consistent with previous studies that have performed detailed analyses of brighter RGB stars at higher spectroscopic resolution and wavelength coverage. It is not clear if the small mean metallicity difference between brighter and fainter M4 members is real or is the result of the low signal-to-noise characteristics of the fainter stars. The strength of our approach is shown by recovering a metallicity close to a single value for more than 2000 stars, using a data set that is non-optimal for atmospheric analyses. This technique is particularly suitable for noisy data taken in difficult observing conditions.

  13. K{sub s} -BAND LUMINOSITY EVOLUTION OF THE ASYMPTOTIC GIANT BRANCH POPULATION BASED ON STAR CLUSTERS IN THE LARGE MAGELLANIC CLOUD

    SciTech Connect (OSTI)

    Ko, Youkyung; Lee, Myung Gyoon; Lim, Sungsoon E-mail: mglee@astro.snu.ac.kr

    2013-11-10

    We present a study of K{sub s} -band luminosity evolution of the asymptotic giant branch (AGB) population in simple stellar systems using star clusters in the Large Magellanic Cloud (LMC). We determine physical parameters of LMC star clusters including center coordinates, radii, and foreground reddenings. Ages of 83 star clusters are derived from isochrone fitting with the Padova models, and those of 19 star clusters are taken from the literature. The AGB stars in 102 star clusters with log(age) = 7.3-9.5 are selected using near-infrared color-magnitude diagrams based on Two Micron All Sky Survey photometry. Then we obtain the K{sub s} -band luminosity fraction of AGB stars in these star clusters as a function of ages. The K{sub s} -band luminosity fraction of AGB stars increases, on average, as age increases from log(age) ? 8.0, reaching a maximum at log(age) ? 8.5, and it decreases thereafter. There is a large scatter in the AGB luminosity fraction for given ages, which is mainly due to stochastic effects. We discuss this result in comparison with five simple stellar population models. The maximum K{sub s} -band AGB luminosity fraction for bright clusters is reproduced by the models that expect the value of 0.7-0.8 at log(age) = 8.5-8.7. We discuss the implication of our results with regard to the study of size and mass evolution of galaxies.

  14. THE GALEX NEARBY YOUNG-STAR SURVEY

    SciTech Connect (OSTI)

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

    2013-09-10

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

  15. PARALLAXES OF STAR-FORMING REGIONS IN THE OUTER SPIRAL ARM OF THE MILKY WAY

    SciTech Connect (OSTI)

    Hachisuka, K.; Choi, Y. K.; Reid, M. J.; Dame, T. M.; Brunthaler, A.; Menten, K. M.; Sanna, A.

    2015-02-10

    We report parallaxes and proper motions of three water maser sources in high-mass star-forming regions in the Outer Spiral Arm of the Milky Way. The observations were conducted with the Very Long Baseline Array as part of Bar and Spiral Structure Legacy Survey and double the number of such measurements in the literature. The Outer Arm has a pitch angle of 14.9 2.7 and a Galactocentric distance of 14.1 0.6 kpc toward the Galactic anticenter. The average motion of these sources toward the Galactic center is 10.7 2.1 km s{sup 1} and we see no sign of a significant fall in the rotation curve out to 15 kpc from the Galactic center. The three-dimensional locations of these star-forming regions are consistent with a Galactic warp of several hundred parsecs from the plane.

  16. MHK Technologies/WaveStar | Open Energy Information

    Open Energy Info (EERE)

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

  17. Winds of low-metallicity OB-type stars: HST-COS spectroscopy in IC 1613

    SciTech Connect (OSTI)

    Garcia, Miriam; Najarro, Francisco; Herrero, Artemio; Urbaneja, Miguel Alejandro

    2014-06-10

    We present the first quantitative ultraviolet spectroscopic analysis of resolved OB stars in IC 1613. Because of its alleged very low metallicity (?1/10 Z {sub ?}, from H II regions), studies in this Local Group dwarf galaxy could become a significant step forward from the Small Magellanic Cloud (SMC) toward the extremely metal-poor massive stars of the early universe. We present HST-COS data covering the ?1150-1800 wavelength range with resolution R ? 2500. We find that the targets do exhibit wind features, and these are similar in strength to SMC stars. Wind terminal velocities were derived from the observed P Cygni profiles with the Sobolev plus Exact Integration method. The v {sub ?}-Z relationship has been revisited. The terminal velocity of IC 1613 O stars is clearly lower than Milky Way counterparts, but there is no clear difference between IC 1613 and SMC or LMC analog stars. We find no clear segregation with host galaxy in the terminal velocities of B-supergiants, nor in the v {sub ?}/v {sub esc} ratio of the whole OB star sample in any of the studied galaxies. Finally, we present the first evidence that the Fe-abundance of IC 1613 OB stars is similar to the SMC, which is in agreement with previous results on red supergiants. With the confirmed ?1/10 solar oxygen abundances of B-supergiants, our results indicate that IC 1613's ?/Fe ratio is sub-solar.

  18. Signatures of a companion star in type Ia supernovae

    SciTech Connect (OSTI)

    Maeda, Keiichi; Kutsuna, Masamichi; Shigeyama, Toshikazu

    2014-10-10

    Although type Ia supernovae (SNe Ia) have been used as precise cosmological distance indicators, their progenitor systems remain unresolved. One of the key questions is whether there is a nondegenerate companion star at the time of a thermonuclear explosion of a white dwarf. In this paper, we investigate whether an interaction between the SN ejecta and the companion star may result in observable footprints around the maximum brightness and thereafter, by performing multidimensional radiation transfer simulations based on hydrodynamic simulations of the interaction. We find that such systems result in variations in various observational characteristics due to different viewing directions, and the predicted behaviors (redder and fainter for the companion direction) are the opposite of what were suggested by the previous study. The variations are generally modest and within observed scatters. However, the model predicts trends between some observables different from those observationally derived, so a large sample of SNe Ia with small calibration errors may be used to constrain the existence of such a companion star. The variations in different colors in optical band passes can be mimicked by external extinctions, so such an effect could be a source of scatter in the peak luminosity and derived distance. After the peak, hydrogen-rich materials expelled from the companion will manifest themselves in hydrogen lines, but Hα is extremely difficult to identify. Alternatively, we find that P{sub β} in postmaximum near-infrared spectra can potentially provide a powerful diagnostic.

  19. GRAVITATIONAL CONUNDRUM? DYNAMICAL MASS SEGREGATION VERSUS DISRUPTION OF BINARY STARS IN DENSE STELLAR SYSTEMS

    SciTech Connect (OSTI)

    De Grijs, Richard; Li, Chengyuan; Zheng, Yong; Kouwenhoven, M. B. N.; Deng, Licai; Hu, Yi; Wicker, James E.

    2013-03-01

    Upon their formation, dynamically cool (collapsing) star clusters will, within only a few million years, achieve stellar mass segregation for stars down to a few solar masses, simply because of gravitational two-body encounters. Since binary systems are, on average, more massive than single stars, one would expect them to also rapidly mass segregate dynamically. Contrary to these expectations and based on high-resolution Hubble Space Telescope observations, we show that the compact, 15-30 Myr old Large Magellanic Cloud cluster NGC 1818 exhibits tantalizing hints at the {approx}> 2{sigma} level of significance (>3{sigma} if we assume a power-law secondary-to-primary mass-ratio distribution) of an increasing fraction of F-star binary systems (with combined masses of 1.3-1.6 M {sub Sun }) with increasing distance from the cluster center, specifically between the inner 10''-20'' (approximately equivalent to the cluster's core and half-mass radii) and the outer 60''-80''. If confirmed, then this will offer support for the theoretically predicted but thus far unobserved dynamical disruption processes of the significant population of 'soft' binary systems-with relatively low binding energies compared to the kinetic energy of their stellar members-in star clusters, which we have access to here by virtue of the cluster's unique combination of youth and high stellar density.

  20. Hypervelocity star candidates in the SEGUE G and K dwarf sample

    SciTech Connect (OSTI)

    Palladino, Lauren E.; Holley-Bockelmann, Kelly; Schlesinger, Katharine J.; Allende Prieto, Carlos; Beers, Timothy C.; Lee, Young Sun; Schneider, Donald P. E-mail: k.holley@vanderbilt.edu

    2014-01-01

    We present 20 candidate hypervelocity stars from the Sloan Extension for Galactic Understanding and Exploration (SEGUE) G and K dwarf samples. Previous searches for hypervelocity stars have only focused on large radial velocities; in this study, we also use proper motions to select the candidates. We determine the hypervelocity likelihood of each candidate by means of Monte Carlo simulations, considering the significant errors often associated with high proper motion stars. We find that nearly half of the candidates exceed their escape velocities with at least 98% probability. Every candidate also has less than a 25% chance of being a high-velocity fluke within the SEGUE sample. Based on orbits calculated using the observed six-dimensional positions and velocities, few, if any, of these candidates originate from the Galactic center. If these candidates are truly hypervelocity stars, they were not ejected by interactions with the Milky Way's supermassive black hole. This calls for a more serious examination of alternative hypervelocity-star ejection scenarios.

  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 navigate the new Portfolio Manager, add a property and enter details about it, enter energy and water consumption data, and more.

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

    Broader source: Energy.gov [DOE]

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

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

    Energy Savers [EERE]

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

  4. Home Performance with ENERGY STAR -- Webinar Slides | Department of Energy

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

    STAR -- Webinar Slides Home Performance with ENERGY STAR -- Webinar Slides "Existing Homes Efficiency - If You Want BetterBuildings - Go with Home Performance with ENERGY STAR," webinar slides from the U.S. Department of Energy. PDF icon Webinar slides More Documents & Publications Home Performance with ENERGY STAR -- 10 Years of Continued Growth! Home Performance with ENERGY STAR - 2014 BTO Peer Review BetterBuildings: Home Performance with ENERGY STAR

  5. Implementing the Data Center Energy Productivity Metric in a High Performance Computing Data Center

    SciTech Connect (OSTI)

    Sego, Landon H.; Marquez, Andres; Rawson, Andrew; Cader, Tahir; Fox, Kevin M.; Gustafson, William I.; Mundy, Christopher J.

    2013-06-30

    As data centers proliferate in size and number, the improvement of their energy efficiency and productivity has become an economic and environmental imperative. Making these improvements requires metrics that are robust, interpretable, and practical. We discuss the properties of a number of the proposed metrics of energy efficiency and productivity. In particular, we focus on the Data Center Energy Productivity (DCeP) metric, which is the ratio of useful work produced by the data center to the energy consumed performing that work. We describe our approach for using DCeP as the principal outcome of a designed experiment using a highly instrumented, high-performance computing data center. We found that DCeP was successful in clearly distinguishing different operational states in the data center, thereby validating its utility as a metric for identifying configurations of hardware and software that would improve energy productivity. We also discuss some of the challenges and benefits associated with implementing the DCeP metric, and we examine the efficacy of the metric in making comparisons within a data center and between data centers.

  6. UNC Energy Frontier Research Center Center for Solar Fuels

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

    UNC Energy Frontier Research Center Center for Solar Fuels University of North Carolina at Chapel Hill (UNC-CH) VISION To provide the basic research to enable a revolution in the collection and conversion of sunlight into storable solar fuels. MISSION To conduct research on dye-sensitized photoelectrosynthesis cells (DSPECs) for water splitting and tandem cells for the reduction of carbon dioxide to carbon-based solar fuels. Center Director Thomas J. Meyer Arey Distinguished Professor of

  7. Ohio Advanced Energy Manufacturing Center

    SciTech Connect (OSTI)

    Kimberly Gibson; Mark Norfolk

    2012-07-30

    The program goal of the Ohio Advanced Energy Manufacturing Center (OAEMC) is to support advanced energy manufacturing and to create responsive manufacturing clusters that will support the production of advanced energy and energy-efficient products to help ensure the nation's energy and environmental security. This goal cuts across a number of existing industry segments critical to the nation's future. Many of the advanced energy businesses are starting to make the transition from technology development to commercial production. Historically, this transition from laboratory prototypes through initial production for early adopters to full production for mass markets has taken several years. Developing and implementing manufacturing technology to enable production at a price point the market will accept is a key step. Since these start-up operations are configured to advance the technology readiness of the core energy technology, they have neither the expertise nor the resources to address manufacturing readiness issues they encounter as the technology advances toward market entry. Given the economic realities of today's business environment, finding ways to accelerate this transition can make the difference between success and failure for a new product or business. The advanced energy industry touches a wide range of industry segments that are not accustomed to working together in complex supply chains to serve large markets such as automotive and construction. During its first three years, the Center has catalyzed the communication between companies and industry groups that serve the wide range of advanced energy markets. The Center has also found areas of common concern, and worked to help companies address these concerns on a segment or industry basis rather than having each company work to solve common problems individually. EWI worked with three industries through public-private partnerships to sew together disparate segments helping to promote overall industry health. To aid the overall advanced energy industry, EWI developed and launched an Ohio chapter of the non-profit Advanced Energy Economy. In this venture, Ohio joins with six other states including Colorado, Connecticut, Illinois, Maine, Massachusetts, New Hampshire, Rhode Island and Vermont to help promote technologies that deliver energy that is affordable, abundant and secure. In a more specific arena, EWI's advanced energy group collaborated with the EWI-run Nuclear Fabrication Consortium to promote the nuclear supply chain. Through this project EWI has helped bring the supply chain up to date for the upcoming period of construction, and assisted them in understanding the demands for the next generation of facilities now being designed. In a more targeted manner, EWI worked with 115 individual advanced energy companies that are attempting to bring new technology to market. First, these interactions helped EWI develop an awareness of issues common to companies in different advanced energy sectors. By identifying and addressing common issues, EWI helps companies bring technology to market sooner and at a lower cost. These visits also helped EWI develop a picture of industry capability. This helped EWI provide companies with contacts that can supply commercial solutions to their new product development challenges. By providing assistance in developing supply chain partnerships, EWI helped companies bring their technology to market faster and at a lower cost than they might have been able to do by themselves. Finally, at the most granular level EWI performed dedicated research and development on new manufacturing processes for advanced energy. During discussions with companies participating in advanced energy markets, several technology issues that cut across market segments were identified. To address some of these issues, three crosscutting technology development projects were initiated and completed with Center support. This included reversible welds for batteries and high temperature heat exchangers. It also included a novel advanced weld trainer that EWI has recently commercialized.

  8. | Center for Bio-Inspired Solar Fuel Production

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

    Center Video Library 31 Mar 2014 EFRC Creative Potential: Thinking Out of the Box Professor Petra Fromme is one of the Bisfuel Principal Investigators. "...Real advantage of the Center is that we have so many creative people working on different aspects of the process, on the hydrogen production catalysts, water splitting catalysts, on developing artificial antennas and reaction centers ... 17 Mar 2014 Rational Design of Artificial Metal-Based Enzymes Giovanna Ghirlanda is one of the EFRC

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

    Open Energy Info (EERE)

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

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

    Office of Scientific and Technical Information (OSTI)

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

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

    Office of Scientific and Technical Information (OSTI)

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

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

    Office of Scientific and Technical Information (OSTI)

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

  13. China National BlueStar Group Corporation | Open Energy Information

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

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

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

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

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

    Open Energy Info (EERE)

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

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

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

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

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

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

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

    Open Energy Info (EERE)

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

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

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

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

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

    Open Energy Info (EERE)

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

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

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

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

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

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

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

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

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

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

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

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

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

  9. National Carbon Capture Center Launches Post-Combustion Test Center |

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

    Department of Energy Carbon Capture Center Launches Post-Combustion Test Center National Carbon Capture Center Launches Post-Combustion Test Center June 6, 2011 - 2:32pm Addthis Jenny Hakun What does this mean for me? Commercial deployment of the processes tested here could cut carbon pollution. Innovation is important to finding ways to make energy cleaner. And testing the ideas and processes that researchers come up with is critical to moving ideas from the lab to the marketplace. That's

  10. Sandia Energy - Energy Frontier Research Center

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

    Energy Frontier Research Center Home Energy Research EFRCs Solid-State Lighting Science EFRC Energy Frontier Research Center Energy Frontier Research CenterTara...

  11. Potential for Data Center Efficiency Improvements | Department...

    Office of Environmental Management (EM)

    Data Center Efficiency Improvements Potential for Data Center Efficiency Improvements Document offers an overview of the Federal Energy Management Program's data center activities. ...

  12. Clean Energy Solutions Center | Open Energy Information

    Open Energy Info (EERE)

    Center Jump to: navigation, search Logo: Clean Energy Solutions Center Name Clean Energy Solutions Center AgencyCompany Organization Clean Energy Ministerial Sector Energy Focus...

  13. Facilities and Centers | Argonne National Laboratory

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

    Energy Storage Argonne Tandem Linac Accelerator System Argonne-Northwestern Solar Energy Research Center Center for Nanoscale Materials Facilities & Centers Argonne's...

  14. Industrial Assessment Centers (IACs) | Department of Energy

    Office of Environmental Management (EM)

    Technical Assistance Industrial Assessment Centers (IACs) Industrial Assessment Centers (IACs) Industrial Assessment Centers (IACs) Small- and medium-sized manufacturers may be...

  15. Online Learning Center | Department of Energy

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

    Online Learning Center Online Learning Center Online Learning Center Whether you're looking to discover new learning opportunities, better manage your career, request external ...

  16. BLM National Training Center | Open Energy Information

    Open Energy Info (EERE)

    National Training Center Jump to: navigation, search Logo: BLM National Training Center Name: BLM National Training Center Address: 9828 North 31st Avenue Place: Phoenix, AZ Zip:...

  17. Western Cooling Efficiency Center | Open Energy Information

    Open Energy Info (EERE)

    Cooling Efficiency Center Jump to: navigation, search Name: Western Cooling Efficiency Center Place: Davis, CA Website: http: References: Western Cooling Efficiency Center 1...

  18. Minco Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Wind Energy Center Jump to: navigation, search Name Minco Wind Energy Center Facility Minco Wind Energy Center Sector Wind energy Facility Type Commercial Scale Wind Facility...

  19. Weatherford Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Weatherford Wind Energy Center Jump to: navigation, search Name Weatherford Wind Energy Center Facility Weatherford Wind Energy Center Sector Wind energy Facility Type Commercial...

  20. Mountaineer Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Mountaineer Wind Energy Center Jump to: navigation, search Name Mountaineer Wind Energy Center Facility Mountaineer Wind Energy Center Sector Wind energy Facility Type Commercial...

  1. Wyoming Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Wind Energy Center Jump to: navigation, search Name Wyoming Wind Energy Center Facility Wyoming Wind Energy Center Sector Wind energy Facility Type Commercial Scale Wind Facility...

  2. Vantage Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Wind Energy Center Jump to: navigation, search Name Vantage Wind Energy Center Facility Vantage Wind Energy Center Sector Wind energy Facility Type Commercial Scale Wind Facility...

  3. Oliver Wind Energy Center | Open Energy Information

    Open Energy Info (EERE)

    Wind Energy Center Jump to: navigation, search Name Oliver Wind Energy Center Facility Oliver Wind Energy Center Sector Wind energy Facility Type Commercial Scale Wind Facility...

  4. Natural Gas Technologies Center | Open Energy Information

    Open Energy Info (EERE)

    Technologies Center Jump to: navigation, search Logo: Natural Gas Technologies Center Name: Natural Gas Technologies Center Address: 1350, Nobel, Boucherville, Quebec, Canada...

  5. Solar Energy Resource Center | Department of Energy

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

    Resource Center Solar Energy Resource Center The SunShot Initiative's Solar Energy Resource Center contains work developed by DOE, national laboratories and SunShot awardees. The ...

  6. Arizona Solar Center | Open Energy Information

    Open Energy Info (EERE)

    Center Jump to: navigation, search Logo: Arizona Solar Center Name: Arizona Solar Center Place: Mesa, Arizona Number of Employees: 1-10 Year Founded: 1999 Website:...

  7. Easton Pond Business Center | Open Energy Information

    Open Energy Info (EERE)

    Easton Pond Business Center Jump to: navigation, search Name Easton Pond Business Center Facility Easton Pond Business Center Sector Wind energy Facility Type Small Scale Wind...

  8. Hydrogen Engine Center HEC | Open Energy Information

    Open Energy Info (EERE)

    Engine Center HEC Jump to: navigation, search Name: Hydrogen Engine Center (HEC) Place: Algona, Iowa Zip: IA 50511 Sector: Hydro, Hydrogen Product: The Hydrogen Engine Center (HEC)...

  9. National Wind Technology Center | NREL

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

    Center The National Wind Technology Center (NWTC) is about 5 miles south of Boulder, Colorado. The cities of Louisville and Broomfield are nearby. The NWTC is approximately 37 miles northwest of Denver International Airport. Please note that the NWTC is not located at the main NREL facility in Golden, Colorado; it is approximately 25 miles north of Golden. View Larger Map National Wind Technology Center Site Entrance Building - Boulder 18200 Highway 128 Boulder, CO 80303 303-384-6900 GPS

  10. Poeh Cultural Center wins grant

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

    Poeh Cultural Center wins grant, educates public Community Connections: Your link to news and opportunities from Los Alamos National Laboratory Latest Issue:May 2016 all issues All Issues » submit Poeh Cultural Center wins grant Native American Venture Acceleration Fund money helps increase education and tourism. May 2, 2016 Poeh Cultural Center and Museum received a grant through the Native American Venture Acceleration Fund in January to develop training programs for artists and to increase

  11. WIPP Activates Emergency Operations Center

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

    August 5, 2015 WIPP Activates Emergency Operations Center At approximately 7:00 p.m. MDT on Tuesday, August 4, the Waste Isolation Pilot Plant (WIPP) activated the Emergency Operations Center (EOC) and the Joint Information Center (JIC) after a radiological control technician detected what was believed to be elevated radiological readings on a filter from an air particulate sampler located where air is exhausted from the WIPP underground. It was later determined that an error was made in the

  12. Precise rotation rates for five slowly rotating A stars

    SciTech Connect (OSTI)

    Gray, David F.

    2014-04-01

    Projected rotation rates of five early A-type slowly rotating stars are measured spectroscopically to a precision of 0.2 km s{sup 1}. A detailed Fourier analysis is done, as well as a comparison of profiles directly. Macroturbulence is needed in addition to rotation to reproduce the profile shapes. An upper limit of ?2 km s{sup 1} is placed on the microturbulence dispersion. Small unexplained differences between the models and the observations are seen in the sidelobe structure of the transforms. The v sin i results are: ? Dra, 26.2; ? Leo, 22.5; ? CMa A, 16.7; ? Gem A, 10.7; o Peg, 6.0 km s{sup 1}. These stars are suitable as standards for measuring rotation using less fundamental methods.

  13. Center for Energy Efficient Materials

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

    Program Overview The Center for Energy Efficient Materials (CEEM) is an Energy Frontier ... Innovative materials and novel devices for sustainable energy efficient applications are ...

  14. Solar Energy Research Center (SERC)

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

    Solar Energy Research Center (SERC) Community Berkeley Global Campus Environmental Documents Tours Community Programs Friends of Berkeley Lab Navigate Section Community ...

  15. ORISE: Center for Epidemiologic Research

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

    the Center for Epidemiologic Research (CER). CER has changed over time as worker health assessment needs have evolved. Since the early 1990s, CER researchers have concentrated on...

  16. Regency Centers | Open Energy Information

    Open Energy Info (EERE)

    with NREL Yes Partnership Type Test & Evaluation Partner Partnering Center within NREL Electricity Resources & Building Systems Integration Partnership Year 2009 Link to project...

  17. Massachusetts realizes wind center dream

    Broader source: Energy.gov [DOE]

    The new testing center will be able to test blades longer than 50 meters, which currently can only be done overseas.

  18. Center for Advanced Solar Photophysics

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

    Solution-processed solar cells The goal of this center ... to boost the efficiency of solar energy conversion through ... light-harvesting and high-efficiency coupling ...

  19. SUPERMASSIVE DARK STARS: DETECTABLE IN JWST

    SciTech Connect (OSTI)

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

    2010-06-20

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

  20. | ANSER Center | Argonne-Northwestern National Laboratory

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

    forms for more information. ANSER Center Travel Checklist ANSER Center Grant Acknowledgment ANSER Center Purchase Order Instructions ANSER Center Purchase Order Form Bid Documentation Form Sole Source Justification Form Project Cafe Security Express Form Instructions Project Cafe Security Express Form

  1. Clean Energy Application Center

    SciTech Connect (OSTI)

    Freihaut, Jim

    2013-09-30

    The Mid Atlantic Clean Energy Application Center (MACEAC), managed by The Penn State College of Engineering, serves the six states in the Mid-Atlantic region (Pennsylvania, New Jersey, Delaware, Maryland, Virginia and West Virginia) plus the District of Columbia. The goals of the Mid-Atlantic CEAC are to promote the adoption of Combined Heat and Power (CHP), Waste Heat Recovery (WHR) and District Energy Systems (DES) in the Mid Atlantic area through education and technical support to more than 1,200 regional industry and government representatives in the region. The successful promotion of these technologies by the MACEAC was accomplished through the following efforts; (1)The MACEAC developed a series of technology transfer networks with State energy and environmental offices, Association of Energy Engineers local chapters, local community development organizations, utilities and, Penn State Department of Architectural Engineering alumni and their firms to effectively educate local practitioners about the energy utilization, environmental and economic advantages of CHP, WHR and DES; (2) Completed assessments of the regional technical and market potential for CHP, WHR and DE technologies application in the context of state specific energy prices, state energy and efficiency portfolio development. The studies were completed for Pennsylvania, New Jersey and Maryland and included a set of incentive adoption probability models used as a to guide during implementation discussions with State energy policy makers; (3) Using the technical and market assessments and adoption incentive models, the Mid Atlantic CEAC developed regional strategic action plans for the promotion of CHP Application technology for Pennsylvania, New Jersey and Maryland; (4) The CHP market assessment and incentive adoption model information was discussed, on a continuing basis, with relevant state agencies, policy makers and Public Utility Commission organizations resulting in CHP favorable incentive programs in New Jersey, Pennsylvania, Maryland and Delaware; (5) Developed and maintained a MACEAC website to provide technical information and regional CHP, WHR and DE case studies and site profiles for use by interested stakeholders in information transfer and policy discussions; (6) Provided Technical Assistance through feasibility studies and on site evaluations. The MACEAC completed 28 technical evaluations and 9 Level 1 CHP analyses ; and (7) the MACEAC provided Technical Education to the region through a series of 29 workshops and webinars, 37 technical presentations, 14 seminars and participation in 13 CHP conferences.

  2. Simulations Reveal Unusual Death for Ancient Stars

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

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

  3. Saving Energy at Data Centers

    SciTech Connect (OSTI)

    2007-10-12

    Data centers provide mission-critical computing functions essential to the daily operation of top U.S. economic, scientific, and technological organizations. These data centers consume large amounts of energy to run and maintain their computer systems, servers, and associated high-performance components.

  4. PNNL Electricity Infrastructure Operations Center | Open Energy...

    Open Energy Info (EERE)

    PNNL Electricity Infrastructure Operations Center (Redirected from Electricity Infrastructure Operations Center) Jump to: navigation, search Logo: Electricity Infrastructure...

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

    SciTech Connect (OSTI)

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

    2012-04-20

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

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

    SciTech Connect (OSTI)

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

    2011-11-15

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

  7. Alternative Fuels Data Center

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

    Natural Gas Vehicle (NGV) Weight Exemption NGVs may exceed the federal maximum gross vehicle weight limit by an amount equal to the difference of the weight of the natural gas tank and fueling system and the weight of a comparable diesel tank and fueling system. The NGV must not exceed a maximum gross vehicle weight of 82,000 pounds. (Reference Public Law 114-94, 2015, and 23 U.S. Code 127(s)

  8. Geothermal Academy: Focus Center

    Broader source: Energy.gov [DOE]

    Project objective: to develop a sufficiently robust data collection and analysis framework to: Accommodate many different kinds of GHP systems and environments. Adequately capture economic; ecological; and socio-economic benefits of GHP systems in policy-levelŽ metrics according to a triple bottom lineŽ framework. Provide policymakers with greater understanding of GHPs; to spur pro-GHP policy development.

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

    Energy Savers [EERE]

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

  10. Home Performance with Energy Star | Department of Energy

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

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

  11. Better Buildings Residential Program Solution Center Demonstration |

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

    Department of Energy Residential Program Solution Center Demonstration Better Buildings Residential Program Solution Center Demonstration Better Buildings Residential Program Solution Center Demonstration from the U.S. Department of Energy. PDF icon Solution Center Demo More Documents & Publications Building Science Solutions … Faster and Better Presentation: Better Buildings Residential Program Solution Center Presentation: Better Buildings Residential Program Solution Center

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

    SciTech Connect (OSTI)

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

    2015-02-24

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

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

    Energy Savers [EERE]

    Bioenergy Upcoming Events Bioenergy Upcoming Events April 2016 < prev next > Sun Mon Tue Wed Thu Fri Sat 27 28 29 30 31 1 2 3 4 5 6 7 8 9 U.S. Regional Association of the International Association for Landscape Ecology Annual Meeting 9:00AM to 5:00PM EDT 10 11 12 13 14 15 16 Oak Ridge National Laboratory Southeast United States Bioenergy Study Tour 2:00PM to 12:00PM EDT International Biomass Conference and Expo 8:00AM to 4:00PM EDT Algal Flow-way Technologies Webinar 12:00PM to 1:30PM EDT

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

    Office of Legacy Management (LM)

    407-425-0707 * http:www.accutest.com Test results contained within this data package ... 407-425-0707 * http:www.accutest.com Test results contained within this data package ...

  15. Successful Field-Scale In Situ Thermal NAPL Remediation at the Young- Rainey STAR Center

    Broader source: Energy.gov [DOE]

    Proceedings of the Fourth International Conference on Remediation of Chlorinated and Recalcitrant Compounds.May 2004, Monterey, California.Randall Juhlin, Michael Butherus, Joseph Daniel, David S....

  16. FIRST Center Research Perspective_Mamontov_QENS

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

    gradual development of the separate localized relaxation in liquids on cooling down makes one- component QENS data fitting inadequate, as manifested by the difference plot (data minus fit) deviation from zero level. Measurements performed at the neutron backscattering spectrometer BASIS of the Spallation Neutron Source, ORNL, suggest that the extent of the separation between the main and secondary relaxations scales with temperature as (T b /T), where T b is boiling temperature. FIRST Center

  17. EPA ENERGY STAR Webcast- Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  18. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  19. EPA ENERGY STAR Webcast: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  20. ENERGY STAR Webinar: Portfolio Manager 301

    Broader source: Energy.gov [DOE]

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

  1. EPA ENERGY STAR Webcast- Portfolio Manager 201

    Broader source: Energy.gov [DOE]

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

  2. EPA ENERGY STAR Webcast: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

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

  3. ENERGY STAR Webinar: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

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

  4. Sue Tierney (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  5. Intirion: ENERGY STAR Referral (MFRA-4GF)

    Broader source: Energy.gov [DOE]

    DOE referred the matter of Intirion refrigerator model MFRA-4GF to the EPA for appropriate action after DOE testing showed that the model does not meet the ENERGY STAR specification.

  6. Michael Liebreich (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  7. Neutron stars in Einstein-aether theory

    SciTech Connect (OSTI)

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

    2007-08-15

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

  8. Haier: ENERGY STAR Referral (DE45EK)

    Broader source: Energy.gov [DOE]

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

  9. Mayor Antonio Villaraigosa (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  10. Edgestar: ENERGY STAR Referral (DEP400EW)

    Office of Energy Efficiency and Renewable Energy (EERE)

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

  11. Xcel Energy- Home Performance with ENERGY STAR

    Broader source: Energy.gov [DOE]

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

  12. Solar Star NAFB LLC | Open Energy Information

    Open Energy Info (EERE)

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

  13. ASKO: ENERGY STAR Referral (D5122XXLB)

    Broader source: Energy.gov [DOE]

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

  14. Whirlpool: ENERGY STAR Referral (ASD2524VE)

    Broader source: Energy.gov [DOE]

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

  15. Home Performance with ENERGY STAR Program

    Broader source: Energy.gov [DOE]

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

  16. Jennifer Granholm (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  17. EPA ENERGY STAR Webcast: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  18. Bill Nye (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

  19. EPA ENERGY STAR Webcast: Portfolio Manager 201

    Broader source: Energy.gov [DOE]

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

  20. Danby: ENERGY STAR Referral (DDR7009REE)

    Broader source: Energy.gov [DOE]

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

  1. Samsung: ENERGY STAR Referral (RF26VAB)

    Broader source: Energy.gov [DOE]

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

  2. Doyle Beneby (Energy All Stars Presentation)

    Broader source: Energy.gov [DOE]

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

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

    Broader source: Energy.gov [DOE]

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

  4. Emerson: ENERGY STAR Referral (CR289E)

    Broader source: Energy.gov [DOE]

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

  5. Danby: ENERGY STAR Referral (DUFM304WDB)

    Broader source: Energy.gov [DOE]

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

  6. Two ENERGY STAR Products Fail Testing

    Broader source: Energy.gov [DOE]

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

  7. Dayton: ENERGY STAR Referral (5NTX1)

    Broader source: Energy.gov [DOE]

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

  8. Danby: ENERGY STAR Referral (DAC10507EE)

    Broader source: Energy.gov [DOE]

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

  9. Magnetic Fields in Population III Star Formation

    SciTech Connect (OSTI)

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

    2012-02-22

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

  10. Astrophysics Simulations from the ASC/Alliances Center for Astrophysical Thermonuclear Flashes

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

    The "Flash Center" works to solve the long-standing problem of thermonuclear flashes on the surfaces of compact stars such as neutron stars and white dwarfs, and in the interior of white dwarfs (i.e., Type I supernovae). The physical conditions, and many of the physical phenomena, are similar to those confronted by the Department of Energy Stockpile Stewardship program. The (fully ionized) plasmas are at very high temperatures and densities; and the physical problems of nuclear ignition, deflagration or detonation, turbulent mixing, and interface dynamics for complex multicomponent fluids are common to the weapons program. Because virtually every aspect of this problem represents a computational Grand Challenge, large-scale numerical simulations are at the heart of its resolution (Taken from Executive Summary page). More than 35 simulations and computer animations developed through research at the "Flash Center" are available here. Each .avi or .mov file also references the related research paper or presentation and provides a link.

  11. ENERGY STAR Webinar: Portfolio Manager 101

    Broader source: Energy.gov [DOE]

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

  12. Christmas burst reveals neutron star collision

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

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

  13. STAR FORMATION IN TWO LUMINOUS SPIRAL GALAXIES

    SciTech Connect (OSTI)

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

    2013-10-01

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

  14. NorthStar Medical Technologies LLC

    National Nuclear Security Administration (NNSA)

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

  15. Modeling tracers of young stellar population age in star-forming galaxies

    SciTech Connect (OSTI)

    Levesque, Emily M.; Leitherer, Claus

    2013-12-20

    The young stellar population of a star-forming galaxy is the primary engine driving its radiative properties. As a result, the age of a galaxy's youngest generation of stars is critical for a detailed understanding of its star formation history, stellar content, and evolutionary state. Here we present predicted equivalent widths for the H?, H?, and Br? recombination lines as a function of stellar population age. The equivalent widths are produced by the latest generations of stellar evolutionary tracks and the Starburst99 stellar population synthesis code, and are the first to fully account for the combined effects of both nebular emission and continuum absorption produced by the synthetic stellar population. Our grid of model stellar populations spans six metallicities (0.001 < Z < 0.04), two treatments of star formation history (a 10{sup 6} M {sub ?} instantaneous burst and a continuous star formation rate of 1 M {sub ?} yr{sup 1}), and two different treatments of initial rotation rate (v {sub rot} = 0.0v {sub crit} and 0.4v {sub crit}). We also investigate the effects of varying the initial mass function. Given constraints on galaxy metallicity, our predicted equivalent widths can be applied to observations of star-forming galaxies to approximate the age of their young stellar populations.

  16. Universality of the acceleration due to gravity on the surface of a rapidly rotating neutron star

    SciTech Connect (OSTI)

    AlGendy, Mohammad; Morsink, Sharon M.

    2014-08-20

    On the surface of a rapidly rotating neutron star, the effective centrifugal force decreases the effective acceleration due to gravity (as measured in the rotating frame) at the equator while increasing the acceleration at the poles due to the centrifugal flattening of the star into an oblate spheroid. We compute the effective gravitational acceleration for relativistic rapidly rotating neutron stars and show that for a star with mass M, equatorial radius R{sub e} , and angular velocity ?, the deviations of the effective acceleration due to gravity from the nonrotating case take on a universal form that depends only on the compactness ratio M/R{sub e} , the dimensionless square of the angular velocity ?{sup 2}R{sub e}{sup 3}/GM, and the latitude on the star's surface. This dependence is universal, in that it has very little dependence on the neutron star's equation of state. The effective gravity is expanded in the slow-rotation limit to show the dependence on the effective centrifugal force, oblate shape of the star, and the quadrupole moment of the gravitational field. In addition, an empirical fit and simple formula for the effective gravity is found. We find that the increase in the acceleration due to gravity at the poles is of the same order of magnitude as the decrease in the effective acceleration due to gravity at the equator for all realistic value of mass, radius, and spin. For neutron stars that spin with frequencies near 600 Hz, the difference between the effective gravity at the poles and the equator is about 20%.

  17. Center for Inverse Design: Collaboration Tool for the Center...

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

    directly to the Center for Inverse Design SharePoint Collaboration Tool. If you have forgotten your password, contact the Webmaster. If you would like to request access to the...

  18. PROCEEDINGS OF RIKEN BNL RESEARCH CENTER WORKSHOP ENTITLED "ODDERON SEARCHES AT RHIC" (VOLUME 76)

    SciTech Connect (OSTI)

    ORGANIZERS: GURYN, W.; KOVCHEGOV, Y.; VOGELSANG, W.; TRUEMAN, L.

    2005-10-25

    The Odderon, a charge-conjugation-odd partner of the Pomeron, has been a puzzle ever since its introduction in 1973. The Pomeron describes a colorless exchange with vacuum quantum numbers in the t-channel of hadronic scattering at high energies. The concept was originally formulated for the non-perturbative regime of Quantum Chromodynamics (QCD). In perturbation theory, the simplest picture of the Poineron is that of a two-gluon exchange process, whereas an Odderon can be thought of as an exchange of three gluons. Both the Pomeron and the Odderon are expected in QCD. However, while there exists plenty of experimental data that could be successfully described by Pomeron exchanges (for example in electron-proton and hadron-hadron scattering at high energies), no experimental sign of the Odderon has been observed. One of the very few hints so far is the difference in the diffractive minima of elastic proton-proton and proton-antiproton scattering measured at the ISR. The Odderon has recently received renewed attention by QCD researchers, mainly for the following two reasons. First of all, RHIC has entered the scene, offering exciting unique new opportunities for Odderon searches. RHIC provides collisions of nuclei at center-of-mass energies far exceeding those at all previous experiments. RHIC also provides collisions of protons of the highest center-of-mass energy, and in the interval, which has not been explored previously in p {bar p} collisions. In addition, it also has the unique feature of polarization for the proton beams, promising to become a crucial tool in Odderon searches. Indeed, theorists have proposed possible signatures of the Odderon in some spin asymmetries measurable at RHIC. Qualitatively unique signals should be seen in these observables if the Odderon coupling is large. Secondly, the Odderon has recently been shown to naturally emerge from the Color Glass Condensate (CGC), a theory for the high-energy asymptotics of QCD. It has been argued that saturation/CGC effects tend to decrease the Odderon intercept, possibly providing an explanation for the lack of experimental evidence for the Odderon so far. This has added further motivation for pursuing searches for the Odderon. During the workshop the status of the Odderon in QCD and its phenomenology were reviewed. The participants also agreed on the most promising observables for the Odderon search at RHIC, which we list. The conclusion of the workshop is that the best available setup to address experimental questions related to the search for the Odderon at RHIC is the proposed combination of STAR experiment and Roman pots of pp2pp experiment, described in the proposal ''Physics with Tagged Forward Protons with the STAR detector at RHIC''.

  19. Pair instability supernovae of very massive population III stars (Journal

    Office of Scientific and Technical Information (OSTI)

    Article) | SciTech Connect Pair instability supernovae of very massive population III stars Citation Details In-Document Search Title: Pair instability supernovae of very massive population III stars Numerical studies of primordial star formation suggest that the first stars in the universe may have been very massive. Stellar models indicate that non-rotating Population III stars with initial masses of 140-260 M {sub ☉} die as highly energetic pair-instability supernovae. We present new

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

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

    Department of Energy Home Performance with ENERGY STAR -- 10 Years of Continued Growth! Home Performance with ENERGY STAR -- 10 Years of Continued Growth! Provides an overview of the HPwES program, HPwES successes, and information on how to become a HPwES sponsor. PDF icon Home Performance with ENERGY STAR Presentation More Documents & Publications Home Performance with Energy Star Home Performance with ENERGY STAR - 2014 BTO Peer Review Home Performance with ENERGY STAR®

  1. SUPERNOVA NEUTRINO LIGHT CURVES AND SPECTRA FOR VARIOUS PROGENITOR STARS:

    Office of Scientific and Technical Information (OSTI)

    FROM CORE COLLAPSE TO PROTO-NEUTRON STAR COOLING (Journal Article) | SciTech Connect SUPERNOVA NEUTRINO LIGHT CURVES AND SPECTRA FOR VARIOUS PROGENITOR STARS: FROM CORE COLLAPSE TO PROTO-NEUTRON STAR COOLING Citation Details In-Document Search Title: SUPERNOVA NEUTRINO LIGHT CURVES AND SPECTRA FOR VARIOUS PROGENITOR STARS: FROM CORE COLLAPSE TO PROTO-NEUTRON STAR COOLING We present a new series of supernova neutrino light curves and spectra calculated by numerical simulations for a variety

  2. Storage and Assay of Tritium in STAR

    SciTech Connect (OSTI)

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

    2004-09-01

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

  3. TIME-VARYING DYNAMICAL STAR FORMATION RATE

    SciTech Connect (OSTI)

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

    2015-02-10

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

  4. Star formation relations in nearby molecular clouds

    SciTech Connect (OSTI)

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

    2014-02-20

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

  5. Measurements of dielectron production in Au + Au collisions at sNN=200 GeV from the STAR experiment

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

    Adamczyk, L.; Adkins, J. K.; Agakishiev, G.; Aggarwal, M. M.; Ahammed, Z.; Alekseev, I.; Alford, J.; Aparin, A.; Arkhipkin, D.; Aschenauer, E. C.; et al

    2015-08-24

    We report on measurements of dielectron (e⁺e⁻) production in Au+Au collisions at a center-of-mass energy of 200 GeV per nucleon-nucleon pair using the STAR detector at RHIC. Systematic measurements of the dielectron yield as a function of transverse momentum (pT) and collision centrality show an enhancement compared to a cocktail simulation of hadronic sources in the low invariant-mass region (Mee < 1GeV/c2). This enhancement cannot be reproduced by the ρ-meson vacuum spectral function. In minimum-bias collisions, in the invariant-mass range of 0.30 – 0.76GeV/c², integrated over the full pT acceptance, the enhancement factor is 1.76±0.06(stat.)±0.26(sys.)±0.29(cocktail). The enhancement factor exhibits weakmore » centrality and pT dependence in STAR's accessible kinematic regions, while the excess yield in this invariant-mass region as a function of the number of participating nucleons follows a power-law shape with a power of 1.44±0.10. Models that assume an in-medium broadening of the ρ-meson spectral function consistently describe the observed excess in these measurements. In addition, we report on measurements of ω- and Φ-meson production through their e⁺e⁻ decay channel. These measurements show good agreement with Tsallis blast-wave model predictions, as well as, in the case of the Φ meson, results through its K⁺K⁻ decay channel. In the intermediate invariant-mass region (1.1 < Mee < 3GeV/c²), we investigate the spectral shapes from different collision centralities. Physics implications for possible in-medium modification of charmed hadron production and other physics sources are discussed.« less

  6. Alternative Fuels Data Center: Fuel Prices

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

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

  7. Influence of stellar multiplicity on planet formation. II. Planets are less common in multiple-star systems with separations smaller than 1500 AU

    SciTech Connect (OSTI)

    Wang, Ji; Fischer, Debra A.; Xie, Ji-Wei; Ciardi, David R.

    2014-08-20

    Almost half of the stellar systems in the solar neighborhood are made up of multiple stars. In multiple-star systems, planet formation is under the dynamical influence of stellar companions, and the planet occurrence rate is expected to be different from that of single stars. There have been numerous studies on the planet occurrence rate of single star systems. However, to fully understand planet formation, the planet occurrence rate in multiple-star systems needs to be addressed. In this work, we infer the planet occurrence rate in multiple-star systems by measuring the stellar multiplicity rate for planet host stars. For a subsample of 56 Kepler planet host stars, we use adaptive optics (AO) imaging and the radial velocity (RV) technique to search for stellar companions. The combination of these two techniques results in high search completeness for stellar companions. We detect 59 visual stellar companions to 25 planet host stars with AO data. Three stellar companions are within 2'' and 27 within 6''. We also detect two possible stellar companions (KOI 5 and KOI 69) showing long-term RV acceleration. After correcting for a bias against planet detection in multiple-star systems due to flux contamination, we find that planet formation is suppressed in multiple-star systems with separations smaller than 1500 AU. Specifically, we find that compared to single star systems, planets in multiple-star systems occur 4.5 3.2, 2.6 1.0, and 1.7 0.5 times less frequently when a stellar companion is present at a distance of 10, 100, and 1000 AU, respectively. This conclusion applies only to circumstellar planets; the planet occurrence rate for circumbinary planets requires further investigation.

  8. Center for Energy Efficient Design

    High Performance Buildings Database

    Rocky Mount, VA As the first Passivhaus public school in North America, the Center for Energy Efficient Design (CEED) in Rocky Mount, Virginia, is a national model for green school construction. An extension of The Leonard A.

  9. Energy Frontier Research Center News

    Office of Science (SC) Website

    a>, was supported in part by the Solid-State Solar Thermal Energy Conversion Center (S3TEC), an EFRC led by Gang Chen at MIT.

    ...

  10. USCA Convocation Center 375 Robert ...

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

    1, 2013 USCA Convocation Center 375 Robert M. Bell Parkway, Aiken, SC 29801 Cash Bar Reception 6:00-6:45 pm BanquetLecture 7:00 pm Tickets: 50 per person Must be...

  11. STAR FORMATION IN ULTRA-FAINT DWARFS: CONTINUOUS OR SINGLE-AGE BURSTS?

    SciTech Connect (OSTI)

    Webster, David; Bland-Hawthorn, Joss; Sutherland, Ralph

    2015-01-30

    We model the chemical evolution of six ultra-faint dwarfs (UFDs): Bootes I, Canes Venatici II, Coma Berenices, Hercules, Leo IV, and Ursa Major I based on their recently determined star formation histories. We show that two single-age bursts cannot explain the observed [α/Fe] versus [Fe/H] distribution in these galaxies and that some self-enrichment is required within the first burst. An alternative scenario is modeled, in which star formation is continuous except for short interruptions when one or more supernovae temporarily blow the dense gas out from the center of the system. This model allows for self-enrichment and can reproduce the chemical abundances of the UFDs in which the second burst is only a trace population. We conclude that the most likely star formation history is one or two extended periods of star formation, with the first burst lasting for at least 100 Myr. As found in earlier work, the observed properties of UFDs can be explained by formation at a low mass (M{sub vir}∼10{sup 7} M{sub ⊙}), rather than being stripped remnants of much larger systems.

  12. NREL: Education Center Home Page

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

    Photo of the NREL Education Center. Clean Energy Innovation Programs for Student and Community Groups NREL's Education Center offers a variety of program topics and experiences for student and adult groups addressing renewable energy and energy efficiency innovations and introducing the work of NREL to audiences. A launch-pad for energy innovations, NREL is home to world-renowned energy experts. NREL researches and develops technologies for powering our homes, buildings, and businesses, and

  13. Kirsch Center for Environmental Studies

    High Performance Buildings Database

    Cupertino, CA The Kirsch Center for Environmental Studies is a two story building completed in summer 2005. The center is the home of the Biological, Health and Environmental Sciences Division of the De Anza College. On the first floor there is a biodiversity lab, a biodiversity outdoor classroom, an energy exhibit hall, a small group learning space, a 90-seat lecture classroom and two 45-seat lecture classrooms.

  14. WINDExchange: About Regional Resource Centers

    Wind Powering America (EERE)

    Deployment Activities Printable Version Bookmark and Share Regional Resource Centers About Economic Development Siting About Regional Resource Centers Significant expansion of wind energy deployment will be required to achieve the President's goal of doubling renewable energy production in the United States by 2020. Wind energy currently provides more than 4% of the nation's electricity but has the potential to provide much more. Increasing the country's percentage from wind power will mean

  15. Information Center | Department of Energy

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

    Center Information Center EM Site Manager Reflects on Field Office's Formative Year, Looks to Future EM Site Manager Reflects on Field Office's Formative Year, Looks to Future EM Los Alamos Field Office Manager Douglas E. Hintze recently spoke with EM Update about the launch of EM's newest site office and its challenges and accomplishments. Read more Los Alamos Demolition Work Progresses Toward Goal of Completing Cleanup Los Alamos Demolition Work Progresses Toward Goal of Completing Cleanup

  16. Information Center | Department of Energy

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

    Center Information Center Congressional Testimony Testimony to Congress by various members of OE. Library Repository of reports and documents; fact sheets; presentations and other documentation from peer review events; and Federal Register notices. Educational Resources Educational material on the generation, transmission, and usage of electricity as well as how the electric grid works and how it needs to be modernized. Reporting Reporting to OE including Electric Disturbance Incidents and

  17. ORISE: Center for Epidemiologic Research

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

    Center for Epidemiologic Research The Oak Ridge Institute for Science and Education (ORISE) has been building its capability in epidemiology since 1978. Early ORISE studies of mortality among U.S. Department of Energy (DOE) nuclear workers led researchers to develop increasing expertise in epidemiologic research, occupational health studies and DOE worker populations. ORISE's researchers and skills coalesced into an operating unit that became the Center for Epidemiologic Research (CER). CER has

  18. LANSCE | Lujan Center | Ancillary Equipment

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

    Ancillary Equipment For general questions, please contact the Lujan Center Sample Environments responsible: Victor Fanelli | vfanelli@lanl.gov | 505.667.8755 Sample and Equipment Shipping Instructions For questions regarding shipping procedures, contact the Lujan Center Experiment Coordinator: TBA Low Temperature Equipment Specifications Flight Path/Instrument Compatibility Responsible Displex closed-cycle refrigerators Tmin= 4 K to 12 K Tmax= 300 K to 340 K 11 - Asterix 04 - HIPPO 03 - HIPD 10

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

    Broader source: Energy.gov [DOE]

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

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

    Broader source: Energy.gov [DOE]

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

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

    Broader source: Energy.gov [DOE]

    The U.S. Environmental Protection Agency (EPA) is hosting a webinar on how to apply for ENERGY STAR certification in Portfolio Manager. Understand the value of the ENERGY STAR certification, see the step-by-step process of applying, and gain tips to help your property get from application to award.

  2. A PARAMETRIC STUDY OF POSSIBLE SOLUTIONS TO THE HIGH-REDSHIFT OVERPRODUCTION OF STARS IN MODELED DWARF GALAXIES

    SciTech Connect (OSTI)

    White, Catherine E.; Somerville, Rachel S.; Ferguson, Henry C.

    2015-02-01

    Both numerical hydrodynamic and semi-analytic cosmological models of galaxy formation struggle to match observed star formation histories of galaxies in low-mass halos (M {sub H} ? 10{sup 11} M {sub ?}), predicting more star formation at high redshift and less star formation at low redshift than observed. The fundamental problem is that galaxies' gas accretion and star formation rates are too closely coupled in the models: the accretion rate largely drives the star formation rate. Observations point to gas accretion rates that outpace star formation at high redshift, resulting in a buildup of gas and a delay in star formation until lower redshifts. We present three empirical adjustments of standard recipes in a semi-analytic model motivated by three physical scenarios that could cause this decoupling: (1) the mass-loading factors of outflows driven by stellar feedback may have a steeper dependence on halo mass at earlier times, (2) the efficiency of star formation may be lower in low-mass halos at high redshift, and (3) gas may not be able to accrete efficiently onto the disk in low-mass halos at high redshift. These new recipes, once tuned, better reproduce the evolution of f {sub *}? M {sub *}/M {sub H} as a function of halo mass as derived from abundance matching over redshifts z = 0 to 3, though they have different effects on cold gas fractions, star formation rates, and metallicities. Changes to gas accretion and stellar-driven winds are promising, while direct modification of the star formation timescale requires drastic measures that are not physically well motivated.

  3. High-resolution H-band spectroscopy of Be stars with SDSS-III/apogee. I. New Be stars, line identifications, and line profiles

    SciTech Connect (OSTI)

    Chojnowski, S. Drew; Majewski, Steven R.; Hall, Matthew; Beaton, Rachael; Burton, Adam; Damke, Guillermo; Wilson, John; Whelan, David G.; Wisniewski, John P.; Shetrone, Matthew; Eikenberry, Steve; Hasselquist, Sten; Holtzman, Jon A.; Brewington, Howard; Brinkmann, J.; Mszros, Szabolcs; Nidever, David; Schneider, Donald P.; Zasowski, Gail; Bizyaev, Dmitry; and others

    2015-01-01

    The Apache Point Observatory Galactic Evolution Experiment (APOGEE) has amassed the largest ever collection of multi-epoch, high-resolution (R?22,500), H-band spectra for B-type emission line (Be) stars. These stars were targeted by APOGEE as telluric standard stars and subsequently identified via visual inspection as Be stars based on H i Brackett series emission or shell absorption in addition to otherwise smooth continua and occasionally non-hydrogen emission features. The 128/238 APOGEE Be stars for which emission had never previously been reported serve to increase the total number of known Be stars by ?6%. Because the H band is relatively unexplored compared to other wavelength regimes, we focus here on identification of the H-band lines and analysis of the emission peak velocity separations (?v{sub p}) and emission peak intensity ratios (V/R) of the usually double-peaked H i and non-hydrogen emission lines. H i Br11 emission is found to preferentially form in the circumstellar disks at an average distance of ?2.2 stellar radii. Increasing ?v{sub p} toward the weaker Br12Br20 lines suggests these lines are formed interior to Br11. By contrast, the observed IR Fe ii emission lines present evidence of having significantly larger formation radii; distinctive phase lags between IR Fe ii and H i Brackett emission lines further supports that these species arise from different radii in Be disks. Several emission lines have been identified for the first time including C i 16895, a prominent feature in the spectra for almost a fifth of the sample and, as inferred from relatively large ?v{sub p} compared to the Br11Br20, a tracer of the inner regions of Be disks. Emission lines at 15760 ? and 16781 ? remain unidentified, but usually appear along with and always have similar line profile morphology to Fe ii 16878. Unlike the typical metallic lines observed for Be stars in the optical, the H-band metallic lines, such as Fe ii 16878, never exhibit any evidence of shell absorption, even when the H i lines are clearly shell-dominated. The first known example of a quasi-triple-peaked Br11 line profile is reported for HD 253659, one of several stars exhibiting intra- and/or extra-species V/R and radial velocity variation within individual spectra. Br11 profiles are presented for all discussed stars, as are full APOGEE spectra for a portion of the sample.

  4. NNSA Service Center Chart | Department of Energy

    Energy Savers [EERE]

    NNSA Service Center Chart NNSA Service Center Chart Office of Chief Counsel at the NNSA Service Center in Albuquerque, NM PDF icon NNSA Service Center Chart More Documents & Publications Technical Qualification Program Accreditation Schedule 2011 Annual Planning Summary for NNSA Service Center (NNSASC) EIS-0466: Notice of Intent to Prepare an Environmental Impact Statement

  5. About the Center for Bio-Inspired Solar Fuel Production | Center...

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

    About the Center for Bio-Inspired Solar Fuel Production Center Objective The Science Center ... drawn from the fundamental concepts that underlie photosynthetic energy conversion. ...

  6. Effects of magnetic fields on lithium evolution in F and G stars

    SciTech Connect (OSTI)

    Li, T. D.; Bi, S. L.; Yang, W. M.; Liu, K.; Tian, Z. J.; Ge, Z. S., E-mail: litanda@mail.bnu.edu.cn, E-mail: bisl@bnu.edu.cn [Astronomy Department, Beijing Normal University, Beijing 100875 (China)

    2014-02-01

    To study the effects of magnetic fields on lithium depletion and to explain the characteristics of lithium evolution in F- and G-type stars in open clusters, we construct a stellar model that includes a Tayler-Spruit dynamo-type field. Through examining the features of extra-mixing caused by magnetic fields in stellar interiors and the relationship between lithium depletion and the input parameters (i.e., mass, metallicity, and the initial rotational condition), we find that the magnetic model produces extra-mixing processes different from other models. During pre-main sequence, the model exhibits very efficient extra-mixing, resulting in strong lithium depletion. As a star evolves, the efficiency of extra-mixing rapidly decreases and lithium depletion slows down at old ages. By setting up different initial rotating conditions, the model predicts dispersions of lithium abundance in both main sequence and pre-main sequence stages. The dispersion begins when a radiative core forms in the interior. The number sees a rapid growth afterward, reaching 0.1-0.5 dex at zero age main sequence in G and late-F stars. The increase of dispersion continues in the main sequence, which is slight in G and late-F stars while significant in mid-F stars. Finally, a comparison is carried out between the theoretical results and the observed data in four open clusters. Good agreements are obtained.

  7. Northeast Clean Energy Application Center

    SciTech Connect (OSTI)

    Bourgeois, Tom

    2013-09-30

    From October 1, 2009 through September 30, 2013 (“contract period”), the Northeast Clean Energy Application Center (“NE-CEAC”) worked in New York and New England (Connecticut, Rhode Island, Vermont, Massachusetts, New Hampshire, and Maine) to create a more robust market for the deployment of clean energy technologies (CETs) including combined heat and power (CHP), district energy systems (DES), and waste heat recovery (WHR) systems through the provision of technical assistance, education and outreach, and strategic market analysis and support for decision-makers. CHP, DES, and WHR can help reduce greenhouse gas emissions, reduce electrical and thermal energy costs, and provide more reliable energy for users throughout the United States. The NE-CEAC’s efforts in the provision of technical assistance, education and outreach, and strategic market analysis and support for decision-makers helped advance the market for CETs in the Northeast thereby helping the region move towards the following outcomes: • Reduction of greenhouse gas emissions and criteria pollutants • Improvements in energy efficiency resulting in lower costs of doing business • Productivity gains in industry and efficiency gains in buildings • Lower regional energy costs • Strengthened energy security • Enhanced consumer choice • Reduced price risks for end-users • Economic development effects keeping more jobs and more income in our regional economy Over the contract period, NE-CEAC provided technical assistance to approximately 56 different potential end-users that were interested in CHP and other CETs for their facility or facilities. Of these 56 potential end-users, five new CHP projects totaling over 60 MW of install capacity became operational during the contract period. The NE-CEAC helped host numerous target market workshops, trainings, and webinars; and NE-CEAC staff delivered presentations at many other workshops and conferences. In total, over 60 different workshops, conferences, webinars, and presentation were hosted or delivered during the contract period. The NE-CEAC also produced publically available educational materials such as CHP project profiles. Finally, the NE-CEAC worked closely with the relevant state agencies involved with CHP development. In New York, the NE-CEAC played an important role in securing and maintaining funding for CHP incentive programs administered by the New York State Energy Research Development Authority. NE-CEAC was also involved in the NYC Mayor's Office DG Collaborative. The NECEAC was also named a strategic resource for the Connecticut Department of Energy and Environmental Protection’s innovative Microgrid Pilot Program.

  8. PHOTOMETRY OF VARIABLE STARS FROM DOME A, ANTARCTICA: RESULTS FROM THE 2010 OBSERVING SEASON

    SciTech Connect (OSTI)

    Wang, Lingzhi; Zhu, Zonghong; Macri, Lucas M.; Wang, Lifan; Ashley, Michael C. B.; Lawrence, Jon S.; Luong-Van, Daniel; Storey, John W. V.; Cui, Xiangqun; Feng, Long-Long; Gong, Xuefei; Liu, Qiang; Shang, Zhaohui; Yang, Huigen; Yang, Ji; Yuan, Xiangyan; Zhou, Xu; Zhu, Zhenxi; Pennypacker, Carl R.; York, Donald G.

    2013-12-01

    We present results from a season of observations with the Chinese Small Telescope ARray, obtained over 183 days of the 2010 Antarctic winter. We carried out high-cadence time-series aperture photometry of 9125 stars with i ∼< 15.3 mag located in a 23 deg{sup 2} region centered on the south celestial pole. We identified 188 variable stars, including 67 new objects relative to our 2008 observations, thanks to broader synoptic coverage, a deeper magnitude limit, and a larger field of view. We used the photometric data set to derive site statistics from Dome A. Based on two years of observations, we find that extinction due to clouds at this site is less than 0.1 and 0.4 mag during 45% and 75% of the dark time, respectively.

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

    Energy Savers [EERE]

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

  10. LANL/Green Star Tests of the Green Star SBS-60 Spectrometer

    SciTech Connect (OSTI)

    T. E. Sampson; D. T. Vo; T. L. Cremers; P. A. Hypes; Y. P. Seldiakov; A. B. Dorin; M. V. Kondrashov; V. I. Timoshin

    2001-06-01

    We report on joint testing of the Russian-designed and manufactured single board spectrometer SBS-60 from Green Star Ltd. of Moscow. The SBS-60 will be used to make material control and accountability measurements on plutonium in the Russian plutonium disposition program. We compared three SBS-60 units of two different designs with three commonly used commercial US data acquisition systems by making measurements with three different HPGe detector systems. The measurements were performed to test if the gamma-ray spectral data of plutonium samples from the SBS-60 was suitable for analysis for the isotopic composition of plutonium using the Los Alamos FRAM isotopic analysis software. Each detector fed its signal to two data acquisition systems, one SBS-60 and one commercial US system. The data from the two systems were analyzed by FRAM and compared. In addition, we characterized the throughput, resolution, and stability of the SBS-60 data acquisition system in comparison with the commercial US systems. This report presents detailed results of all the tests performed.

  11. Abundances of presolar graphite and SiC from supernovae and AGB stars in the Murchison meteorite

    SciTech Connect (OSTI)

    Amari, Sachiko; Zinner, Ernst; Gallino, Roberto

    2014-05-02

    Pesolar graphite grains exhibit a range of densities (1.65 – 2.20 g/cm{sup 3}). We investigated abundances of presolar graphite grains formed in supernovae and in asymptotic giant branch (AGB) stars in the four density fractions KE3, KFA1, KFB1 and KFC1 extracted from the Murchison meteorite to probe dust productions in these stellar sources. Seventy-six and 50% of the grains in the low-density fractions KE3 and KFA1, respectively, are supernova grains, while only 7.2% and 0.9% of the grains in the high-density fractions KFB1 and KFC1 have a supernova origin. Grains of AGB star origin are concentrated in the high-density fractions KFB1 and KFC1. From the C isotopic distributions of these fractions and the presence of s-process Kr with {sup 86}Kr/{sup 82}Kr = 4.43±0.46 in KFC1, we estimate that 76% and 80% of the grains in KFB1 and KFC1, respectively, formed in AGB stars. From the abundance of graphite grains in the Murchison meteorite, 0.88 ppm, the abundances of graphite from supernovae and AGB stars are 0.24 ppm and 0.44 ppm, respectively: the abundances of graphite in supernovae and AGB stars are comparable. In contrast, it has been known that 1% of SiC grains formed in supernovae and 95% formed in AGB stars in meteorites. Since the abundance of SiC grains is 5.85 ppm in the Murchison meteorite, the abundances of SiC from supernovae and AGB stars are 0.063 ppm and 5.6 ppm, respectively: the dominant source of SiC grains is AGB stars. Since SiC grains are harder and likely to survive better in space than graphite grains, the abundance of supernova graphite grains, which is higher than that of supernova SiC grains, indicates that supernovae proficiently produce graphite grains. Graphite grains from AGB stars are, in contrast, less abundant that SiC grains from AGB stars (0.44 ppm vs. 5.6 ppm). It is difficult to derive firm conclusions for graphite and SiC formation in AGB stars due to the difference in susceptibility to grain destruction. Metallicity of the parent AGB stars of graphite grains is much lower than that of SiC grains and the difference in metallicity might also have affected to the difference in the abundances in the Murchison meteorite.

  12. STARS MDT-II targets mission

    SciTech Connect (OSTI)

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

    1997-08-01

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

  13. THE CLASSIFICATION OF KEPLER B-STAR VARIABLES

    SciTech Connect (OSTI)

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

    2012-04-15

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

  14. EERE: Alternative Fuels Data Center Home Page

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

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  15. Alternative Fuels Data Center: Case Studies

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

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  16. Alternative Fuels Data Center: Emerging Fuels

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

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  17. Alternative Fuels Data Center: Flexible Fuel Vehicles

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

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  18. Alternative Fuels Data Center: Idle Reduction

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

    Idle Reduction to someone by E-mail Share Alternative Fuels Data Center: Idle Reduction on Facebook Tweet about Alternative Fuels Data Center: Idle Reduction on Twitter Bookmark Alternative Fuels Data Center: Idle Reduction on Google Bookmark Alternative Fuels Data Center: Idle Reduction on Delicious Rank Alternative Fuels Data Center: Idle Reduction on Digg Find More places to share Alternative Fuels Data Center: Idle Reduction on AddThis.com... More in this section... Idle Reduction Benefits

  19. Alternative Fuels Data Center: Natural Gas

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

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

  20. Alternative Fuels Data Center: Natural Gas Vehicles

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

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  1. Alternative Fuels Data Center: Project Assistance

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

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  2. Alternative Fuels Data Center: Propane Vehicles

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

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  3. Alternative Fuels Data Center: Spanish Resources

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

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  4. Alternative Fuels Data Center: State Information

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

    State Information to someone by E-mail Share Alternative Fuels Data Center: State Information on Facebook Tweet about Alternative Fuels Data Center: State Information on Twitter Bookmark Alternative Fuels Data Center: State Information on Google Bookmark Alternative Fuels Data Center: State Information on Delicious Rank Alternative Fuels Data Center: State Information on Digg Find More places to share Alternative Fuels Data Center: State Information on AddThis.com... Icon of a state map on a

  5. Alternative Fuels Data Center: Vehicle Cost Calculator

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

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  6. Alternative Fuels Data Center: Vehicle Search

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

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

  7. Alternative Fuels Data Center: Active Transit

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

    Active Transit to someone by E-mail Share Alternative Fuels Data Center: Active Transit on Facebook Tweet about Alternative Fuels Data Center: Active Transit on Twitter Bookmark Alternative Fuels Data Center: Active Transit on Google Bookmark Alternative Fuels Data Center: Active Transit on Delicious Rank Alternative Fuels Data Center: Active Transit on Digg Find More places to share Alternative Fuels Data Center: Active Transit on AddThis.com... More in this section... Idle Reduction Parts

  8. Alternative Fuels Data Center: Biodiesel Blends

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

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  9. Alternative Fuels Data Center: Biodiesel Fuel Basics

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

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  10. Alternative Fuels Data Center: Biodiesel Vehicle Emissions

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

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  11. Alternative Fuels Data Center: Diesel Vehicle Availability

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

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  12. Alternative Fuels Data Center: Dimethyl Ether

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

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  13. Alternative Fuels Data Center: Electricity Fuel Basics

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

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  14. Alternative Fuels Data Center: Ethanol Fuel Basics

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

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  15. Alternative Fuels Data Center: Ethanol Fueling Stations

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

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  16. Alternative Fuels Data Center: Hydrogen Basics

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

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  17. Alternative Fuels Data Center: Hydrogen Fueling Stations

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

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  18. Alternative Fuels Data Center: Latest Additions

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

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  19. Alternative Fuels Data Center: Mass Transit

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

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  20. Alternative Fuels Data Center: Natural Gas Benefits

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

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  1. Alternative Fuels Data Center: Natural Gas Distribution

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

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  2. Alternative Fuels Data Center: Propane Basics

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

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  3. Alternative Fuels Data Center: Propane Benefits

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

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  4. Alternative Fuels Data Center: Propane Fueling Stations

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

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  5. Alternative Fuels Data Center: Propane Vehicle Availability

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

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  6. Alternative Fuels Data Center: Propane Vehicle Conversions

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

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  7. Alternative Fuels Data Center: Propane Vehicle Emissions

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

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  8. Alternative Fuels Data Center: Vehicle Conversions

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

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  9. Alternative Fuels Data Center: Vehicle Search

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

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  10. Alternative Fuels Data Center: Biodiesel Related Links

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

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  11. Alternative Fuels Data Center: Blender Pump Dispensers

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

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  12. Alternative Fuels Data Center: Conversion Regulations

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

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  13. Alternative Fuels Data Center: E85 Specification

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

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  14. Alternative Fuels Data Center: Electricity Related Links

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

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  15. Alternative Fuels Data Center: Ethanol Blends

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

    Ethanol Blends to someone by E-mail Share Alternative Fuels Data Center: Ethanol Blends on Facebook Tweet about Alternative Fuels Data Center: Ethanol Blends on Twitter Bookmark Alternative Fuels Data Center: Ethanol Blends on Google Bookmark Alternative Fuels Data Center: Ethanol Blends on Delicious Rank Alternative Fuels Data Center: Ethanol Blends on Digg Find More places to share Alternative Fuels Data Center: Ethanol Blends on AddThis.com... More in this section... Ethanol Basics Blends E15

  16. Alternative Fuels Data Center: Ethanol Feedstocks

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

    Feedstocks to someone by E-mail Share Alternative Fuels Data Center: Ethanol Feedstocks on Facebook Tweet about Alternative Fuels Data Center: Ethanol Feedstocks on Twitter Bookmark Alternative Fuels Data Center: Ethanol Feedstocks on Google Bookmark Alternative Fuels Data Center: Ethanol Feedstocks on Delicious Rank Alternative Fuels Data Center: Ethanol Feedstocks on Digg Find More places to share Alternative Fuels Data Center: Ethanol Feedstocks on AddThis.com... More in this section...

  17. Alternative Fuels Data Center: Ethanol Production

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

    Production to someone by E-mail Share Alternative Fuels Data Center: Ethanol Production on Facebook Tweet about Alternative Fuels Data Center: Ethanol Production on Twitter Bookmark Alternative Fuels Data Center: Ethanol Production on Google Bookmark Alternative Fuels Data Center: Ethanol Production on Delicious Rank Alternative Fuels Data Center: Ethanol Production on Digg Find More places to share Alternative Fuels Data Center: Ethanol Production on AddThis.com... More in this section...

  18. Alternative Fuels Data Center: Ethanol Related Links

    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 Related Links to someone by E-mail Share Alternative Fuels Data Center: Ethanol Related Links on Facebook Tweet about Alternative Fuels Data Center: Ethanol Related Links on Twitter Bookmark Alternative Fuels Data Center: Ethanol Related Links on Google Bookmark Alternative Fuels Data Center: Ethanol Related Links on Delicious Rank Alternative Fuels Data Center: Ethanol Related Links on Digg Find

  19. Alternative Fuels Data Center: Hydrogen Related Links

    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 Related Links to someone by E-mail Share Alternative Fuels Data Center: Hydrogen Related Links on Facebook Tweet about Alternative Fuels Data Center: Hydrogen Related Links on Twitter Bookmark Alternative Fuels Data Center: Hydrogen Related Links on Google Bookmark Alternative Fuels Data Center: Hydrogen Related Links on Delicious Rank Alternative Fuels Data Center: Hydrogen Related Links on

  20. Alternative Fuels Data Center: Lifecycle Energy Balance

    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: Lifecycle Energy Balance to someone by E-mail Share Alternative Fuels Data Center: Lifecycle Energy Balance on Facebook Tweet about Alternative Fuels Data Center: Lifecycle Energy Balance on Twitter Bookmark Alternative Fuels Data Center: Lifecycle Energy Balance on Google Bookmark Alternative Fuels Data Center: Lifecycle Energy Balance on Delicious Rank Alternative Fuels Data Center: Lifecycle Energy