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Sample records for lone star wind

  1. Lone Star Wind Alliance LSWA | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I4Q07)Wind

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

    Open Energy Info (EERE)

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I (4Q07)Q3)

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I (4Q07) Wind

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I4Q07) Wind

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I (4Q07)Q3)II

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I

  8. 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,...

  9. Lone Star Transmission LLC | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I4Q07)

  10. Lone Star Healthy Streams Final Report 

    E-Print Network [OSTI]

    Wagner, Kevin; Redmon, Larry

    2011-01-01

    2010. The Lone Star Healthy Streams Bibliography was then converted into an online searchable database accessible from http://lshs.tamu.edu. As information was collected, it was incorporated into the LSHS Power Point presentation and guidance manual... bacteria from grazing lands has been identified as a significant source of bacterial contamination in need of reductions to improve water quality. Development of best management practices to address these bacterial issues is critical to the success...

  11. Lone Star Healthy Streams: Teaching best management practices statewide 

    E-Print Network [OSTI]

    Lee, Leslie

    2010-01-01

    ) using Clean Water Act Nonpoint Source Grant funding from the U.S. Environmental Protection Agency. Since its inception, LSHS has involved numerous collabo- rators, including TSSWCB, U.S. The Lone Star Healthy Streams Program teaches owners...

  12. Lone Star Healthy Streams: Teaching best managment practices statewide 

    E-Print Network [OSTI]

    Lee, Leslie

    2011-01-01

    ) using Clean Water Act Nonpoint Source Grant funding from the U.S. Environmental Protection Agency. Since its inception, LSHS has involved numerous collabo- rators, including TSSWCB, U.S. The Lone Star Healthy Streams Program teaches owners...

  13. Lone Star Reds: the Socialist Party and cotton tenancy in Texas, 1901-1917 

    E-Print Network [OSTI]

    Mellard, Jason Dean

    2000-01-01

    ideal, the party of Eugene Debs seized on the strong Texas tradition of agrarian revolt to build a formidable, if short-lived, Socialist movement in the Lone Star State. There were Socialist newspapers, unions, rural encampments, and a Socialist...

  14. Audit of Lone Star Gas Invoices and Billing Procedures, Task #3 

    E-Print Network [OSTI]

    Turner, W. D.; Liu, M.

    1997-01-01

    At the request of the TAMU Power Plant, the ESL staff audited the 1995 Lone Star Gas Company invoices. Gas consumption is measured and the measured volume is converted to standard volume (at T=60 °F, P= 14.65 psia) to determine the energy content...

  15. Development of a Synergistic, Comprehensive Statewide Lone Star Healthy Streams Program 

    E-Print Network [OSTI]

    Wagner, K.; Redmon, L.; Peterson, J.

    2013-01-01

    • October 19, 2010 • March 9, 2011 • June 23, 2011 • October 24, 2011 • February 15, 2012 Subtask 1.4: Development of Final Report The final report was compiled by TWRI staff and submitted on April 30, 2013. Task 2: LSHS Program Coordination... Technical Report 446 September 2013 Development of a Synergistic, Comprehensive Statewide Lone Star Healthy Streams Program 2 Executive Summary According to the 2008 Texas Water Quality Inventory and 303(d) List, 295 waterbodies...

  16. Spectral Modeling Hot Star Winds

    E-Print Network [OSTI]

    Cohen, David

    Spectral Modeling of X-Rays from Hot Star Winds Emma Wollman Advisor: David Cohen #12;Hot Stars ·· Short-livedShort-lived (~ 1-10 million yrs)(~ 1-10 million yrs) #12;Stellar Winds · Net momentum · More luminosity !"stronger wind · Mass-loss rate determines the fate of the star #12;X-ray Production

  17. LoneSTAR Program: Maximizing Energy Efficiency while Protecting the Envrionment 

    E-Print Network [OSTI]

    Trevino, E.

    2014-01-01

    iency whi le Protect ing the Envi ronment LoanSTAR PROGRAM ESL-KT-14-11-31 CATEE 2014: Clean Air Through Efficiency Conference, Dallas, Texas Nov. 18-20 ? Executed 240 loans totaling $407,923,762.32 ? 93 loans to publ ic schools distr icts ? 80 loans...-11-31 CATEE 2014: Clean Air Through Efficiency Conference, Dallas, Texas Nov. 18-20 BASICS ? I t ’s al l about the ut i l i ty dollar savings ? Loan must have a composite simple payback of 10 years or less ? The simple payback is the loan term ? Each loan...

  18. Money earmarked for cervid research at Texas Tech -Texas Hunting & Fishing | Lone Star Outdoor News http://www.lsonews.com/money-earmarked-cervid-research-texas-tech/[8/11/2014 8:25:26 AM

    E-Print Network [OSTI]

    Rock, Chris

    Money earmarked for cervid research at Texas Tech - Texas Hunting & Fishing | Lone Star Outdoor News http://www.lsonews.com/money-earmarked-cervid-research-texas-tech/[8/11/2014 8:25:26 AM] Money earmarked for cervid research at Texas Tech By Conor Harrison on August 8, 2014 in Texas Hunting 0 Texas

  19. X-ray Emission from the Winds of Massive Stars

    E-Print Network [OSTI]

    Cohen, David

    X-ray Emission from the Winds of Massive Stars David Cohen Department of Physics & Astronomy-driven stellar winds are a characteristic of massive stars NGC 6888 Crescent Nebula - Tony Hallas #12;NGC 6888 Crescent Nebula - Tony Hallas O star - source of wind bubble: ~1 arc second instrumental resolution; star

  20. NLTE wind models for SMC stars

    E-Print Network [OSTI]

    Jiri Krticka

    2005-09-15

    We study stellar wind properties of selected late O stars in the Small Magellanic Cloud (SMC). We calculate NLTE line-driven wind models for these stars and compare predicted wind parameters with observed values. We found satisfactory agreement between theoretical and observed terminal velocities. On the other hand, predicted and observed mass-loss rates are in a good agreement only for higher mass-loss rates. For mass-loss rates lower than approximately 10^{-7} M_sun / year we found large discrepancy between theoretical and observed values. We propose a new explanation of this effect based on dynamical decoupling of some atoms. Finally, we study the dependence of wind terminal velocities and mass-loss rates on metallicity.

  1. The Impulsive Heating Rate in Shocked O Star Winds

    E-Print Network [OSTI]

    Cohen, David

    The Impulsive Heating Rate in Shocked O Star Winds: Determined Directly from High-Resolution X; no corona #12;Radiation-driven O star winds Pup (O4 supergiant): M ~ few 10-6 Msun/yr UV spectrum: C IV with the stellar wind #12;Radiation-driven O star winds kinetic power in the wind = 1/2 Mv 2 (~10-3 Lbol) typically

  2. X-rays from magnetically channeled winds of OB stars

    E-Print Network [OSTI]

    David H. Cohen

    2008-01-30

    OB stars with strong radiation-driven stellar winds and large-scale magnetic fields generate strong and hard X-ray emission via the Magnetically Channeled Wind Shock (MCWS) mechanism. In this brief paper, I describe four separate X-ray diagnostics of the MCWS mechanism in OB stars, with applications to the prototype young O star, theta-1 Ori C.

  3. Magnetic Channeling of Radiatively Driven Hot-Star Winds

    E-Print Network [OSTI]

    Owocki, Stanley P.

    in magnetic Bp stars like sigma Ori C. We conclude with an outlook for the general role of magnetic fields that of the solar wind. Their high surface temperatures mean that such stars lack the hydrogen recombination convection zone that induces the magnetic dynamo cycle of cooler, solar type stars [e.g., 3]. Such stars have

  4. Pair Winds in Schwarzschild Spacetime with Application to Strange Stars

    E-Print Network [OSTI]

    A. G. Aksenov; M. Milgrom; V. V. Usov

    2007-01-09

    We present the results of numerical simulations of stationary, spherically outflowing, electron-positron pair winds, with total luminosities in the range 10^{34}--10^{42} ergs/s. In the concrete example described here, the wind injection source is a hot, bare, strange star, predicted to be a powerful source of pairs created by the Coulomb barrier at the quark surface. We find that photons dominate in the emerging emission, and the emerging photon spectrum is rather hard and differs substantially from the thermal spectrum expected from a neutron star with the same luminosity. This might help distinguish the putative bare strange stars from neutron stars.

  5. X-ray Spectroscopy of Massive Star Winds: Shocks, Mass-Loss Rates, and Clumping

    E-Print Network [OSTI]

    Cohen, David

    X-ray Spectroscopy of Massive Star Winds: Shocks, Mass-Loss Rates, and Clumping David Cohen X-rays A. wind-shock physics B. wind absorption: wind mass-loss rate C. with H-alpha: wind clumping Chandra resolved X-ray line profile spectroscopy of O star winds #12;Prior to 2000: only low-resolution X

  6. Spectral Modeling of X-rays from Hot Star Winds Emma E. Wollman, Swarthmore College `09

    E-Print Network [OSTI]

    Cohen, David

    and absorption. Consequently, the more luminous a star is, the stronger the wind it can support. This wind-driving1 Spectral Modeling of X-rays from Hot Star Winds Emma E. Wollman, Swarthmore College `09 Prof x-ray spectra from Chandra's archive. Models of x-ray production in hot star winds predict broad

  7. LIMB-DARKENED RADIATION-DRIVEN WINDS FROM MASSIVE STARS

    SciTech Connect (OSTI)

    Cure, M.; Cidale, L.

    2012-10-01

    We calculated the influence of the limb-darkened finite-disk correction factor in the theory of radiation-driven winds from massive stars. We solved the one-dimensional m-CAK hydrodynamical equation of rotating radiation-driven winds for all three known solutions, i.e., fast, {Omega}-slow, and {delta}-slow. We found that for the fast solution, the mass-loss rate is increased by a factor of {approx}10%, while the terminal velocity is reduced about 10%, when compared with the solution using a finite-disk correction factor from a uniformly bright star. For the other two slow solutions, the changes are almost negligible. Although we found that the limb darkening has no effects on the wind-momentum-luminosity relationship, it would affect the calculation of synthetic line profiles and the derivation of accurate wind parameters.

  8. Colliding Winds in Low-Mass Binary Star Systems: wind interactions and implications for habitable planets

    E-Print Network [OSTI]

    Johnstone, C P; Pilat-Lohinger, E; Bisikalo, D; Güdel, M; Eggl, S

    2015-01-01

    Context. In binary star systems, the winds from the two components impact each other, leading to strong shocks and regions of enhanced density and temperature. Potentially habitable circumbinary planets must continually be exposed to these interactions regions. Aims. We study, for the first time, the interactions between winds from low-mass stars in a binary system, to show the wind conditions seen by potentially habitable circumbinary planets. Methods. We use the advanced 3D numerical hydrodynamic code Nurgush to model the wind interactions of two identical winds from two solar mass stars with circular orbits and a binary separation of 0.5 AU. As input into this model, we use a 1D hydrodynamic simulation of the solar wind, run using the Versatile Advection Code. We derive the locations of stable and habitable orbits in this system to explore what wind conditions potentially habitable planets will be exposed to during their orbits. Results. Our wind interaction simulations result in the formation of two stron...

  9. Astrophysics Research Projects:Astrophysics Research Projects: massive star winds, x-ray emission, theoretical models,massive star winds, x-ray emission, theoretical models,

    E-Print Network [OSTI]

    Cohen, David

    Astrophysics Research Projects:Astrophysics Research Projects: massive star winds, x-ray emission, theoretical models,massive star winds, x-ray emission, theoretical models, spectroscopy, laboratory plasma-drivenhave powerful radiation-driven stellar windsstellar winds.. etaeta CarinaCarina #12;TheThe ChandraChandra X

  10. X-rayEmissionfromMassiveStars: UsingEmissionLineProfilestoConstrainWind

    E-Print Network [OSTI]

    Cohen, David

    X-rayEmissionfromMassiveStars: UsingEmissionLineProfilestoConstrainWind Kinematics? Pup:windX-rays,butlessabsorptionthanexpected OriandOri:similarsituation,verylittlewind absorption). Cyclicaland stochastic variabilityis seeninmost hotstars'winds #12

  11. Wind Circulation in Selected Rotating Magnetic Early-B Stars

    E-Print Network [OSTI]

    Myron A. Smith; Detlef Groote

    2001-04-03

    The rotating magnetic B stars have oblique dipolar magnetic fields and often anomalous helium and metallic compositions. These stars develop co-rotating torus-shaped clouds by channelling winds from their magnetic poles to an anchored planar disk over the magnetic equator. The line absorptions from the cloud can be studied as the complex rotates and periodically occults the star. We describe an analysis of the clouds of four stars (HD184927, beta Cep, sigma Ori E, and HR6684). From line synthesis models, we find that the metallic compositions are spatially uniform over the stars' surfaces. Next, using the Hubeny CIRCUS code, we demonstate that periodic UV continuum fluxes can be explained by the absorption of low-excitation lines. The analysis also quantifies the cloud temperatures, densities, and turbulences, which appear to increase inward toward the stars. The temperatures range from about 12,000K for the weak Fe lines up to temperatures of 33,000K for N V absorptions, which is in excess of temperatures expected from radiative equilibrium. The spectroscopic hallmark of this stellar class is the presence of strong C IV and N V resonance line absorptions at occultation phases and of redshifted emissions at magnetic pole-on phases. The emissions have characteristics which seem most compatible with the generation of high-energy shocks at the wind-cloud interface, as predicted by Babel.

  12. Star Point Wind Farm | Open Energy Information

    Open Energy Info (EERE)

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  13. Silver Star Wind Farm | Open Energy Information

    Open Energy Info (EERE)

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  14. NONTHERMAL HIGH-ENERGY EMISSION FROM COLLIDING WINDS OF MASSIVE STARS A. Reimer,1,2

    E-Print Network [OSTI]

    Pohl, Martin Karl Wilhelm

    NONTHERMAL HIGH-ENERGY EMISSION FROM COLLIDING WINDS OF MASSIVE STARS A. Reimer,1,2 M. Pohl,3 and O of high-energy photon production in colliding winds of long-period WR+OB systems. Analytical formulae. Reimer1 Received 2005 October 24; accepted 2006 February 20 ABSTRACT Colliding winds of massive star

  15. Wind accretion in binary stars II. Accretion rates

    E-Print Network [OSTI]

    Tom Theuns; Henri Boffin; Alain Jorissen

    1996-02-18

    Smoothed particle hydrodynamics (SPH) is used to estimate accretion rates of mass, linear and angular momentum in a binary system where one component undergoes mass loss through a wind. Physical parameters are chosen such as to model the alleged binary precursors of barium stars, whose chemical peculiarities are believed to result from the accretion of the wind from a companion formerly on the asymptotic giant branch (AGB). The binary system modelled consists of a 3 solar masses AGB star on the main sequence, in a 3AU circular orbit. Three-dimensional simulations are performed for gases with polytropic indices gamma=1, 1.1 and 1.5, to bracket more realistic situations that would include radiative cooling. Mass accretion rates are found to depend on resolution and we estimate typical values of 1-2% for the gamma=1.5 case and 8% for the other models. The highest resolution obtained (with 400k particles) corresponds to an accretor of linear size 16 solar radii. Despite being (in the gamma = 1.5 case) about ten times smaller than theoretical estimates based on the Bondi-Hoyle prescription, the SPH accretion rates remain large enough to explain the pollution of barium stars. Uncertainties in the current SPH rates remain however, due to the simplified treatment of the wind acceleration mechanism, as well as to the absence of any cooling prescription and to the limited numerical resolution. Angular momentum transfer leads to significant spin up of the accretor and can account for the rapid rotation of HD165141, a barium star with a young white dwarf companion and a rotation rate unusually large among K giants.

  16. BroadStar Wind Systems | Open Energy Information

    Open Energy Info (EERE)

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  17. Nucleosynthesis in neutrino-driven winds after neutron star mergers

    E-Print Network [OSTI]

    Martin, Dirk; Arcones, Almudena; Thielemann, Friedrich-Karl; Korobkin, Oleg; Rosswog, Stephan

    2015-01-01

    We present a comprehensive nucleosynthesis study of the neutrino-driven wind in the aftermath of a binary neutron star merger. Our focus is the initial remnant phase when a massive central neutron star is present. Using tracers from a recent hydrodynamical simulation, we determine total masses and integrated abundances to characterize the composition of unbound matter. We find that the nucleosynthetic yields depend sensitively on both the life time of the massive neutron star and the polar angle. Matter in excess of up to $9 \\cdot 10^{-3} M_\\odot$ becomes unbound until $\\sim 200~{\\rm ms}$. Due to electron fractions of $Y_{\\rm e} \\approx 0.2 - 0.4$ mainly nuclei with mass numbers $A < 130$ are synthesized, complementing the yields from the earlier dynamic ejecta. Mixing scenarios with these two types of ejecta can explain the abundance pattern in r-process enriched metal-poor stars. Additionally, we calculate heating rates for the decay of the freshly produced radioactive isotopes. The resulting light curve...

  18. Atomic physics of shocked plasma in winds of massive stars

    SciTech Connect (OSTI)

    Leutenegger, Maurice A.; Cohen, David H.; Owocki, Stanley P. [NASA/Goddard Space Flight Center, Greenbelt, MD 20771 (United States); CRESST/UMBC (United States); Swarthmore College, Swarthmore, PA 19081 (United States); Bartol Research Institute, University of Delaware, Newark, DE 19716 (United States)

    2012-05-25

    High resolution diffraction grating spectra of X-ray emission from massive stars obtained with Chandra and XMM-Newton have revolutionized our understanding of their powerful, radiation-driven winds. Emission line shapes and line ratios provide diagnostics on a number of key wind parameters. Modeling of resolved emission line velocity profiles allows us to derive independent constraints on stellar mass-loss rates, leading to downward revisions of a factor of a few from previous measurements. Line ratios in He-like ions strongly constrain the spatial distribution of Xray emitting plasma, confirming the expectations of radiation hydrodynamic simulations that X-ray emission begins moderately close to the stellar surface and extends throughout the wind. Some outstanding questions remain, including the possibility of large optical depths in resonance lines, which is hinted at by differences in line shapes of resonance and intercombination lines from the same ion. Resonance scattering leads to nontrivial radiative transfer effects, and modeling it allows us to place constraints on shock size, density, and velocity structure.

  19. Resolved X-ray emission line profiles Clumping in Hot Star Winds

    E-Print Network [OSTI]

    Cohen, David

    Resolved X-ray emission line profiles Clumping in Hot Star Winds W.-R. Hamann, A. Feldmeier & L and wind porosity. We find that reducing the mass-loss rate of Pup by roughly a factor of four, to 1.5 × 10-6 M yr-1 , enables simple non-porous wind models to provide good fits to the data. If

  20. Resonance scattering in X-ray line profiles of Pup Clumping in Hot Star Winds

    E-Print Network [OSTI]

    Cohen, David

    Resonance scattering in X-ray line profiles of Pup Clumping in Hot Star Winds W.-R. Hamann, A the same wind parameters. We show that the differences in profile shape can be accounted for in a model its effect is difficult to distinguish from a low effective continuum optical depth in the wind. Thus

  1. Line formation in the inner winds of classical T Tauri stars: testing the conical wind solution

    E-Print Network [OSTI]

    Kurosawa, Ryuichi

    2012-01-01

    We present the emission line profile models of hydrogen and helium based on the results from axisymmetric magnetohydrodynamics (MHD) simulations of the wind formed near the disk-magnetosphere boundary of classical T Tauri stars (CTTSs). We extend the previous outflow models of `the conical wind' by Romanova et al. to include a well defined magnetospheric accretion funnel flow which is essential for modelling the optical and near-infrared hydrogen and helium lines of CTTSs. Our MHD model shows outflows in conical shape with a half opening angle about 35 degrees. The flow properties such as the maximum outflow speed in the conical wind, maximum inflow speed in the accretion funnel, mass-accretion and mass-loss rates are comparable to those found in a typical CTTS. The density, velocity and temperature from the MHD simulations are used in a separate radiative transfer model to predict the line profiles and test the consistency of the MHD models with observations. The line profiles are computed with various combi...

  2. ON THE WEAK-WIND PROBLEM IN MASSIVE STARS: X-RAY SPECTRA REVEAL A MASSIVE HOT WIND IN ? COLUMBAE

    E-Print Network [OSTI]

    Huenemoerder, David P.

    ? Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. This allows us, for the first time, ...

  3. Modeling X-ray Emission Line Profiles from Massive Star Winds - A Review

    E-Print Network [OSTI]

    Ignace, Richard

    2016-01-01

    The Chandra and XMM-Newton X-ray telescopes have led to numerous advances in the study and understanding of astrophysical X-ray sources. Particularly important has been the much increased spectral resolution of modern X-ray instrumentation. Wind-broadened emission lines have been spectroscopically resolved for many massive stars. This contribution reviews approaches to the modeling of X-ray emission line profile shapes from single stars, including smooth winds, winds with clumping, optically thin versus thick lines, and the effect of a radius-dependent photoabsorption coefficient.

  4. X-ray Spectral Measurements of the Most Massive Stars: Stellar Wind Mass-Loss Rates and Shock Physics

    E-Print Network [OSTI]

    Cohen, David

    X-ray Spectral Measurements of the Most Massive Stars: Stellar Wind Mass-Loss Rates and Shock, and their winds (the site of X-ray production). From the basic question of how the X-rays are produced, I have branched out to questions of wind structure and wind mass-loss rates that the X-ray observations can

  5. Multiple Molecular Winds in Evolved Stars I. A Survey of CO(2-1) and CO(3-2) Emission from 45 Nearby AGB Stars

    E-Print Network [OSTI]

    G. R. Knapp; K. Young; E. Lee; A. Jorissen

    1997-11-12

    This paper describes observations of a new phenomenon in evolved mass-losing AGB stars: the presence of two winds with different expansion velocities. CO(2-1) and CO(3-2) line emission was observed for 45 AGB stars at high velocity resolution and double winds found in 20% of the sample. Highly asymmetric lines were found in six other stars. The data tentatively suggest that double winds occur when the star undergoes a change (pulsational mode, chemical composition) and that the very narrow components represent the onset of a new phase of mass loss.

  6. SPIN EVOLUTION OF ACCRETING YOUNG STARS. II. EFFECT OF ACCRETION-POWERED STELLAR WINDS

    SciTech Connect (OSTI)

    Matt, Sean P.; Greene, Thomas P.; Pudritz, Ralph E. E-mail: thomas.p.greene@nasa.gov E-mail: pudritz@physics.mcmaster.ca

    2012-01-20

    We present a model for the rotational evolution of a young, solar-mass star interacting magnetically with an accretion disk. As in a previous paper (Paper I), the model includes changes in the star's mass and radius as it descends the Hayashi track, a decreasing accretion rate, and a prescription for the angular momentum transfer between the star and disk. Paper I concluded that, for the relatively strong magnetic coupling expected in real systems, additional processes are necessary to explain the existence of slowly rotating pre-main-sequence stars. In the present paper, we extend the stellar spin model to include the effect of a spin-down torque that arises from an accretion-powered stellar wind (APSW). For a range of magnetic field strengths, accretion rates, initial spin rates, and mass outflow rates, the modeled stars exhibit rotation periods within the range of 1-10 days in the age range of 1-3 Myr. This range coincides with the bulk of the observed rotation periods, with the slow rotators corresponding to stars with the lowest accretion rates, strongest magnetic fields, and/or highest stellar wind mass outflow rates. We also make a direct, quantitative comparison between the APSW scenario and the two types of disk-locking models (namely, the X-wind and Ghosh and Lamb type models) and identify some remaining theoretical issues for understanding young star spins.

  7. ON THE WEAK-WIND PROBLEM IN MASSIVE STARS: X-RAY SPECTRA REVEAL A MASSIVE HOT WIND IN {mu} COLUMBAE

    SciTech Connect (OSTI)

    Huenemoerder, David P.; Oskinova, Lidia M.; Todt, Helge; Ignace, Richard; Waldron, Wayne L.; Hamaguchi, Kenji

    2012-09-10

    {mu} Columbae is a prototypical weak-wind O star for which we have obtained a high-resolution X-ray spectrum with the Chandra LETG/ACIS instrument and a low-resolution spectrum with Suzaku. This allows us, for the first time, to investigate the role of X-rays on the wind structure in a bona fide weak-wind system and to determine whether there actually is a massive hot wind. The X-ray emission measure indicates that the outflow is an order of magnitude greater than that derived from UV lines and is commensurate with the nominal wind-luminosity relationship for O stars. Therefore, the {sup w}eak-wind problem{sup -}identified from cool wind UV/optical spectra-is largely resolved by accounting for the hot wind seen in X-rays. From X-ray line profiles, Doppler shifts, and relative strengths, we find that this weak-wind star is typical of other late O dwarfs. The X-ray spectra do not suggest a magnetically confined plasma-the spectrum is soft and lines are broadened; Suzaku spectra confirm the lack of emission above 2 keV. Nor do the relative line shifts and widths suggest any wind decoupling by ions. The He-like triplets indicate that the bulk of the X-ray emission is formed rather close to the star, within five stellar radii. Our results challenge the idea that some OB stars are 'weak-wind' stars that deviate from the standard wind-luminosity relationship. The wind is not weak, but it is hot and its bulk is only detectable in X-rays.

  8. O Star X-ray Line Profiles Explained by Radiation Transfer in Inhomogeneous Stellar Wind

    E-Print Network [OSTI]

    L. M. Oskinova; A. Feldmeier; W. -R. Hamann

    2005-11-01

    It is commonly adopted that X-rays from O stars are produced deep inside the stellar wind, and transported outwards through the bulk of the expanding matter which attenuates the radiation and affects the shape of emission line profiles. The ability of Chandra and XMM-Newton to resolve these lines spectroscopically provided a stringent test for the theory of X-ray production. It turned out that none of the existing models was able to reproduce the observations consistently. The major caveat of these models was the underlying assumption of a smooth stellar wind. Motivated by the various observational evidence that the stellar winds are in fact structured, we present a 2-D model of a stochastic, inhomogeneous wind. The X-ray radiative transfer is derived for such media. It is shown that profiles from a clumped wind differ drastically from those predicted by conventional homogeneous models. We review the up-to-date observations of X-ray line profiles from stellar winds and present line fits obtained from the inhomogeneous wind model. The necessity to account for inhomogeneities in calculating the X-ray transport in massive star winds, including for HMXB is highlighted.

  9. Corotating Interaction Regions in 2D HotStar Wind Models with LineDriven Instability

    E-Print Network [OSTI]

    Owocki, Stanley P.

    in the wind from a rotating star. CIRs have long been observed and studied in the solar wind, but Mullan (1984, this is of order v=v th AE 1 larger than the Sobolev length L j v th =(dv=dr), over which the mean flow speed v an artifact of the (artificially?) fast inward wave propagation obtained in a Sobolev treatment (cf. Owocki

  10. Radio Detections of Stellar Winds from the Pistol Star and Other Stars in the Galactic Center Quintuplet Cluster

    E-Print Network [OSTI]

    Lang, C C; Goss, W M; Morris, M; Lang, Cornelia C.; Figer, Don F.

    1999-01-01

    VLA images of the Sickle and Pistol H II regions near the Galactic center at 3.6 and 6 cm reveal six point sources in the region where the dense Quintuplet stellar cluster is located. The spectral indices of five of these sources between 6 cm and 3.6 cm have values of alpha = +0.5 to +0.8, consistent with the interpretation that the radio sources correspond to ionized stellar winds of the massive stars in this cluster. The radio source associated with the Pistol Star shows alpha = -0.4 +/- 0.2, consistent with a flat or slightly non-thermal spectrum.

  11. Radio Detections of Stellar Winds from the Pistol Star and Other Stars in the Galactic Center Quintuplet Cluster

    E-Print Network [OSTI]

    Cornelia C. Lang; Don F. Figer; W. M. Goss; Mark Morris

    1999-07-13

    VLA images of the Sickle and Pistol H II regions near the Galactic center at 3.6 and 6 cm reveal six point sources in the region where the dense Quintuplet stellar cluster is located. The spectral indices of five of these sources between 6 cm and 3.6 cm have values of alpha = +0.5 to +0.8, consistent with the interpretation that the radio sources correspond to ionized stellar winds of the massive stars in this cluster. The radio source associated with the Pistol Star shows alpha = -0.4 +/- 0.2, consistent with a flat or slightly non-thermal spectrum.

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

    SciTech Connect (OSTI)

    Garcia, Miriam; Najarro, Francisco [Centro de Astrobiología, CSIC-INTA. Ctra. Torrejón a Ajalvir km.4, E-28850 Torrejón de Ardoz, Madrid (Spain); Herrero, Artemio [Instituto de Astrofísica de Canarias. Vía Láctea s/n, E-38200 La Laguna (S. C. Tenerife) (Spain); Lennon, Daniel J. [European Space Astronomy Centre, Camino Bajo del Castillo, E-28692 Villanueva de la Cañada, Madrid (Spain); Urbaneja, Miguel Alejandro [Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25/8, A-6020 Innsbruck (Austria)

    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 Å 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.

  13. X-rays from A stars -Coronae and wind-shocks Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029

    E-Print Network [OSTI]

    Robrade, Jan

    1 X-rays from A stars - Coronae and wind-shocks Robrade J. Hamburger Sternwarte, University of Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany, email: jrobrade@hs.uni-hamburg.de Abstract The X the regimes of cool and hot stars and they exhibit diverse high-energy phenomena; notably, among A stars we

  14. Long Island New York City Offshore Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone Star I4Q07)WindNew

  15. A Search for Intrinsic Polarization in O Stars with Variable Winds

    E-Print Network [OSTI]

    David McDavid

    1999-09-28

    New observations of 9 of the brightest northern O stars have been made with the Breger polarimeter on the 0.9~m telescope at McDonald Observatory and the AnyPol polarimeter on the 0.4~m telescope at Limber Observatory, using the Johnson-Cousins UBVRI broadband filter system. Comparison with earlier measurements shows no clearly defined long-term polarization variability. For all 9 stars the wavelength dependence of the degree of polarization in the optical range can be fit by a normal interstellar polarization law. The polarization position angles are practically constant with wavelength and are consistent with those of neighboring stars. Thus the simplest conclusion is that the polarization of all the program stars is primarily interstellar. The O stars chosen for this study are generally known from ultraviolet and optical spectroscopy to have substantial mass loss rates and variable winds, as well as occasional circumstellar emission. Their lack of intrinsic polarization in comparison with the similar Be stars may be explained by the dominance of radiation as a wind driving force due to higher luminosity, which results in lower density and less rotational flattening in the electron scattering inner envelopes where the polarization is produced. However, time series of polarization measurements taken simultaneously with H-alpha and UV spectroscopy during several coordinated multiwavelength campaigns suggest two cases of possible small-amplitude, periodic short-term polarization variability, and therefore intrinsic polarization, which may be correlated with the more widely recognized spectroscopic variations.

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsourceII JumpQuarterly SmartDB-2, BluePoulsen Hybrid, LLCBiofuelsEthanol LLC Jump8) Wind

  17. The colliding-wind WC9+OB system WR 65 and dust formation by WR stars

    E-Print Network [OSTI]

    Williams, P M

    2015-01-01

    Observations of the WC9+OB system WR 65 in the infrared show variations of its dust emission consistent with a period near 4.8~yr, suggesting formation in a colliding-wind binary (CWB) having an elliptical orbit. If we adopt the IR maximum as zero phase, the times of X-ray maximum count and minimum extinction to the hard component measured by Oskinova & Hamann fall at phases 0.4--0.5, when the separation of the WC9 and OB stars is greatest. We consider WR 65 in the context of other WC8-9+OB stars showing dust emission.

  18. Structure of pair winds from compact objects with application to emission from hot bare strange stars

    E-Print Network [OSTI]

    A. G. Aksenov; M. Milgrom; V. V. Usov

    2004-03-15

    We consider a stationary, spherically outflowing wind consisting of electron-positron pairs and photons. We do not assume thermal equilibrium, and include the two-body processes that occur in such a wind: Moller and Bhaba scattering of pairs, Compton scattering, two-photon pair annihilation, and two-photon pair production, together with their radiative three-body variants: bremsstrahlung, double Compton scattering, and three-photon pair annihilation, with their inverse processes. In the concrete example described here, the wind injection source is a hot, bare, strange star. Such stars are thought to be powerful sources of pairs created by the Coulomb barrier at the quark surface. We present a new, finite-difference scheme for solving the relativistic kinetic Boltzmann equations for pairs and photons. Using this method we study the kinetics of the wind particles and the emerging emission for total luminosities of L=10^{34}-10^{42} ergs/s. We find the rates of particle number and energy outflows, outflow velocities, number densities, energy spectra, and other parameters for both photons and pairs as functions of the distance. We find that for L>2x10^{35} ergs/s, photons dominate the emerging emission. As L increases from ~ 10^{34} to 10^{42} ergs/s, the mean energy of emergent photons decreases from ~400-500 keV to 40 keV, as the spectrum changes in shape from that of a wide annihilation line to nearly a blackbody spectrum with a high energy (> 100 keV) tail. These results are pertinent to the deduction of the outside appearance of hot bare strange stars, which might help discern them from neutron stars.

  19. Joint spectral and polarimetric analysis of hot star wind transients This article has been downloaded from IOPscience. Please scroll down to see the full text article.

    E-Print Network [OSTI]

    Bertero, Mario

    Joint spectral and polarimetric analysis of hot star wind transients This article has been Problems 11 (1995) 79-96. Primed in the UK Joint spectral and polarimetricanalysisof hot star wind. Some of these stellar winds are very weak. That of the sun, for example, is driven by the gas pressure

  20. Grand Unification of Solutions of Accretion and Winds around Black Holes and Neutron Stars

    E-Print Network [OSTI]

    Sandip K. Chakrabarti

    1996-06-22

    We provide the complete set of global solutions of viscous transonic flows (VTFs) around black holes and neutron stars. These solutions describe the optically thick and optically thin flows from the horizon of the black hole or from the neutron star surface to the location where the flow joins with a Keplerian disk. We study the nature of the multiple sonic points as functions of advection, rotation, viscosity, heating and cooling. Stable shock waves, which join two transonic solutions, are found to be present in a large region of the parameter space. We classify the solutions in terms of whether or not the flow can have a standing shock wave. We find no new topology of solutions other than what are observed in our previous studies of isothermal VTFs. We particularly stress the importance of the boundary conditions and argue that we have the most complete solution of accretion and winds around black holes and neutron stars.

  1. ON THE RADIAL ONSET OF CLUMPING IN THE WIND OF THE B0I MASSIVE STAR QV NOR

    E-Print Network [OSTI]

    Oskinova, L.

    We present an analysis of a 78 ks Chandra high-energy transmission gratings observation of the B0I star QV Nor, the massive donor of the wind-accreting pulsar 4U1538?52. The neutron star (NS) orbits its companion in a very ...

  2. X-ray Emission from Ionized Wind-Bubbles around Wolf-Rayet Stars

    E-Print Network [OSTI]

    Dwarkadas, Vikram V

    2015-01-01

    Using a code that employs a self-consistent method for computing the effects of photoionization on circumstellar gas dynamics, we model the formation of wind-driven nebulae around massive Wolf-Rayet (W-R) stars. Our algorithm incorporates a simplified model of the photo-ionization source, computes the fractional ionization of hydrogen due to the photoionizing flux and recombination, and determines self-consistently the energy balance due to ionization, photo-heating and radiative cooling. We take into account changes in stellar properties and mass-loss over the star's evolution. Our multi-dimensional simulations clearly reveal the presence of strong ionization front instabilities. Using various X-ray emission models, and abundances consistent with those derived for W-R nebulae, we compute the X-ray flux and spectra from our wind bubble models. We show the evolution of the X-ray spectral features with time over the evolution of the star, taking the absorption of the X-rays by the ionized bubble into account. O...

  3. Winds from Neutron Stars and Strong Type I X--Ray Bursts

    E-Print Network [OSTI]

    Luciano Nobili; Roberto Turolla; Iosif Lapidus

    1994-05-27

    A model for stationary, radiatively driven winds from X--ray bursting neutron stars is presented. General relativistic hydrodynamical and radiative transfer equations are integrated from the neutron star surface outwards, taking into account for helium nuclear burning in the inner, dense, nearly hydrostatic shells. Radiative processes include both bremsstrahlung emission--absorption and Compton scattering; only the frequency--integrated transport is considered here. It is shown that each solution is characterized by just one parameter: the mass loss rate $\\Mdot$, or, equivalently, the envelope mass $\\Menv$. We found that, owing to the effects of Comptonization, steady, supersonic winds can exist only for $\\Mdot$ larger than a limiting value $\\Mdot_{min} \\approx\\Mdot_{E}$. Several models, covering about two decades in mass loss rate, have been computed for given neutron star parameters. We discuss how the sequence of our solutions with decreasing $\\Menv$ can be used to follow the time evolution of a strong X--ray burst during the expansion/contraction phase near to the luminosity maximum. The comparison between our numerical results and the observational data of Haberl {\\it et al.\\/} (1987) for the bursts in 4U/MXB 1820-30 gives an estimate for both the spectral hardening factor and the accretion rate in this source.

  4. Analytical solutions for radiation-driven winds in massive stars. I. The fast regime

    SciTech Connect (OSTI)

    Araya, I.; Curé, M.; Cidale, L. S.

    2014-11-01

    Accurate mass-loss rate estimates are crucial keys in the study of wind properties of massive stars and for testing different evolutionary scenarios. From a theoretical point of view, this implies solving a complex set of differential equations in which the radiation field and the hydrodynamics are strongly coupled. The use of an analytical expression to represent the radiation force and the solution of the equation of motion has many advantages over numerical integrations. Therefore, in this work, we present an analytical expression as a solution of the equation of motion for radiation-driven winds in terms of the force multiplier parameters. This analytical expression is obtained by employing the line acceleration expression given by Villata and the methodology proposed by Müller and Vink. On the other hand, we find useful relationships to determine the parameters for the line acceleration given by Müller and Vink in terms of the force multiplier parameters.

  5. Neutrino-driven winds in the aftermath of a neutron star merger: nucleosynthesis and electromagnetic transients

    E-Print Network [OSTI]

    Dirk Martin; Albino Perego; Almudena Arcones; Friedrich-Karl Thielemann; Oleg Korobkin; Stephan Rosswog

    2015-09-24

    We present a comprehensive nucleosynthesis study of the neutrino-driven wind in the aftermath of a binary neutron star merger. Our focus is the initial remnant phase when a massive central neutron star is present. Using tracers from a recent hydrodynamical simulation, we determine total masses and integrated abundances to characterize the composition of unbound matter. We find that the nucleosynthetic yields depend sensitively on both the life time of the massive neutron star and the polar angle. Matter in excess of up to $9 \\cdot 10^{-3} M_\\odot$ becomes unbound until $\\sim 200~{\\rm ms}$. Due to electron fractions of $Y_{\\rm e} \\approx 0.2 - 0.4$ mainly nuclei with mass numbers $A < 130$ are synthesized, complementing the yields from the earlier dynamic ejecta. Mixing scenarios with these two types of ejecta can explain the abundance pattern in r-process enriched metal-poor stars. Additionally, we calculate heating rates for the decay of the freshly produced radioactive isotopes. The resulting light curve peaks in the blue band after about $4~{\\rm h}$. Furthermore, high opacities due to heavy r-process nuclei in the dynamic ejecta lead to a second peak in the infrared after $3-4~{\\rm d}$.

  6. Non-thermal high-energy emission from colliding winds of massive stars

    E-Print Network [OSTI]

    A. Reimer; M. Pohl; O. Reimer

    2005-10-25

    Colliding winds of massive star binary systems are considered as potential sites of non-thermal high-energy photon production. This is motivated merely by the detection of synchrotron radio emission from the expected colliding wind location. Here we investigate the properties of high-energy photon production in colliding winds of long-period WR+OB-systems. We found that in the dominating leptonic radiation process anisotropy and Klein-Nishina effects may yield spectral and variability signatures in the gamma-ray domain at or above the sensitivity of current or upcoming gamma-ray telescopes. Analytical formulae for the steady-state particle spectra are derived assuming diffusive particle acceleration out of a pool of thermal wind particles, and taking into account adiabatic and all relevant radiative losses. For the first time we include their advection/convection in the wind collision zone, and distinguish two regions within this extended region: the acceleration region where spatial diffusion is superior to convective/advective motion, and the convection region defined by the convection time shorter than the diffusion time scale. The calculation of the Inverse Compton radiation uses the full Klein-Nishina cross section, and takes into account the anisotropic nature of the scattering process. This leads to orbital flux variations by up to several orders of magnitude which may, however, be blurred by the geometry of the system. The calculations are applied to the typical WR+OB-systems WR 140 and WR 147 to yield predictions of their expected spectral and temporal characteristica and to evaluate chances to detect high-energy emission with the current and upcoming gamma-ray experiments. (abridged)

  7. Massive stars and the energy balance of the interstellar medium. II. The 35 solar mass star and a solution to the "missing wind problem"

    E-Print Network [OSTI]

    Tim Freyer; Gerhard Hensler; Harold W. Yorke

    2005-12-05

    We continue our numerical analysis of the morphological and energetic influence of massive stars on their ambient interstellar medium for a 35 solar mass star that evolves from the main sequence through red supergiant and Wolf-Rayet phases, until it ultimately explodes as a supernova. We find that structure formation in the circumstellar gas during the early main-sequence evolution occurs as in the 60 solar mass case but is much less pronounced because of the lower mechanical wind luminosity of the star. Since on the other hand the shell-like structure of the HII region is largely preserved, effects that rely on this symmetry become more important. At the end of the stellar lifetime 1% of the energy released as Lyman continuum radiation and stellar wind has been transferred to the circumstellar gas. From this fraction 10% is kinetic energy of bulk motion, 36% is thermal energy, and the remaining 54% is ionization energy of hydrogen. The sweeping up of the slow red supergiant wind by the fast Wolf-Rayet wind produces remarkable morphological structures and emission signatures, which are compared with existing observations of the Wolf-Rayet bubble S308. Our model reproduces the correct order of magnitude of observed X-ray luminosity, the temperature of the emitting plasma as well as the limb brightening of the intensity profile. This is remarkable, because current analytical and numerical models of Wolf-Rayet bubbles fail to consistently explain these features. A key result is that almost the entire X-ray emission in this stage comes from the shell of red supergiant wind swept up by the shocked Wolf-Rayet wind rather than from the shocked Wolf-Rayet wind itself as hitherto assumed and modeled. This offers a possible solution to what is called the ``missing wind problem'' of Wolf-Rayet bubbles.

  8. Lone Star Healthy Streams: Keeping Texas streams clean 

    E-Print Network [OSTI]

    Boutwell, Kathryn S.

    2013-01-01

    ,? said Jennifer Peterson, LSHS statewide coordinator. ?For each bacterial contributor, we created a manual and a presentation outlining BMPs that are operation- speci?c.? ?e program published manuals for poultry, beef ca?le, feral hogs, horses.... Dairy Cattle: Construct a waste treatment lagoon by building an embankment and/or excavating a pit or dugout to biologically treat waste. Feral Hogs: Although they require more effort to install and maintain, using corral traps is extremely...

  9. Co-rotating Interaction Regions in 2D Hot-Star Wind Models with Line-Driven Instability

    E-Print Network [OSTI]

    Owocki, Stanley P.

    in the wind from a rotating star. CIRs have long been observed and studied in the solar wind, but Mullan 1984a=vth 1 larger than the Sobolev length L vth=dv=dr, over which the mean ow speed v increases by a ion, but it is still not clear whether they might in fact be just an artifact of the arti cially? fast inward wave

  10. R-Process Nucleosynthesis In Neutrino-Driven Winds From A Typical Neutron Star With M = 1.4 Msun

    E-Print Network [OSTI]

    M. Terasawa; K. Sumiyoshi; S. Yamada; H. Suzuki; T. Kajino

    2002-06-18

    We study the effects of the outer boundary conditions in neutrino-driven winds on the r-process nucleosynthesis. We perform numerical simulations of hydrodynamics of neutrino-driven winds and nuclear reaction network calculations of the r-process. As an outer boundary condition of hydrodynamic calculations, we set a pressure upon the outermost layer of the wind, which is approaching toward the shock wall. Varying the boundary pressure, we obtain various asymptotic thermal temperature of expanding material in the neutrino-driven winds for resulting nucleosynthesis. We find that the asymptotic temperature slightly lower than those used in the previous studies of the neutrino-driven winds can lead to a successful r-process abundance pattern, which is in a reasonable agreement with the solar system r-process abundance pattern even for the typical proto-neutron star mass Mns ~ 1.4 Msun. A slightly lower asymptotic temperature reduces the charged particle reaction rates and the resulting amount of seed elements and lead to a high neutron-to-seed ratio for successful r-process. This is a new idea which is different from the previous models of neutrino-driven winds from very massive (Mns ~ 2.0 Msun) and compact (Rns ~ 10 km) neutron star to get a short expansion time and a high entropy for a successful r-process abundance pattern. Although such a large mass is sometimes criticized from observational facts on a neutron star mass, we dissolve this criticism by reconsidering the boundary condition of the wind. We also explore the relation between the boundary condition and neutron star mass, which is related to the progenitor mass, for successful r-process.

  11. The magnetic field and confined wind of the O star $?^1$~Orionis~C

    E-Print Network [OSTI]

    G. A. Wade; A. W. Fullerton; J. -F. Donati; J. D. Landstreet; P. Petit; S. Strasser

    2006-01-26

    In this paper we confirm the presence of a globally-ordered, kG-strength magnetic field in the photosphere of the young O star $\\theta^1$~Orionis~C, and examine the properties of its optical line profile variations. A new series of high-resolution MuSiCoS Stokes $V$ and $I$ spectra has been acquired which samples approximately uniformly the rotational cycle of $\\theta^1$~Orionis~C. Using the Least-Squares Deconvolution (LSD) multiline technique, we have succeeded in detecting variable Stokes $V$ Zeeman signatures associated with the LSD mean line profile. These signatures have been modeled to determine the magnetic field geometry. We have furthermore examined the profi le variations of lines formed in both the wind and photosphere using dynamic spectra. Based on spectrum synthesis fitting of the LSD profiles, we determine that the polar strength of the magnetic dipole component is $1150 \\la B_{\\rm d}\\la 1800$~G and that the magnetic obliquity is $27\\degr \\la \\beta \\la 68\\degr$, assuming $i=45\\pm 20\\degr$. The best-fit values for $i=45\\degr$ are $B_{\\rm d} = 1300 \\pm 150 (1\\sigma)$~G and $\\beta = 50\\degr \\pm 6\\degr (1\\sigma)$. Our data confirm the previous detection of a magnetic field in this star, and furthermore demonstrate the sinusoidal variability of the longitudinal field and accurately determine the phases and intensities of the magnetic extrema. The analysis of ``photospheric'' and ``wind'' line profile variations supports previous reports of the optical spectroscopic characteristics, and provides evidence for infall of material within the magnetic equatorial plane.

  12. The soft and hard X-rays thermal emission from star cluster winds with a supernova explosion

    E-Print Network [OSTI]

    Castellanos-Ramirez, A; Esquivel, A; Toledo-Roy, J C; Olivares, J; Velazquez, P F

    2015-01-01

    Massive young star clusters contain dozens or hundreds of massive stars that inject mechanical energy in the form of winds and supernova explosions, producing an outflow which expands into their surrounding medium, shocking it and forming structures called superbubbles. The regions of shocked material can have temperatures in excess of 10$^6$ K, and emit mainly in thermal X-rays (soft and hard). This X-ray emission is strongly affected by the action of thermal conduction, as well as by the metallicity of the material injected by the massive stars. We present three-dimensional numerical simulations exploring these two effects, metallicity of the stellar winds and supernova explosions, as well as thermal conduction.

  13. Galactic Winds and Structure of z~2 Star-forming Galaxies

    E-Print Network [OSTI]

    Newman, Sarah

    2013-01-01

    inconsistent with a purely energy-driven wind unless none ofcould be explained by energy-driven winds. In addition, themassive SFGs and with energy-driven winds. The scaling with

  14. The Properties of the Progenitor Supernova, Pulsar Wind, and Neutron Star inside PWN G54.1+0.3

    E-Print Network [OSTI]

    Gelfand, Joseph D; Temim, Tea

    2015-01-01

    The evolution of a pulsar wind nebula (PWN) inside a supernova remnant (SNR) is sensitive to properties of the central neutron star, pulsar wind, progenitor supernova, and interstellar medium. These properties are both difficult to measure directly and critical for understanding the formation of neutron stars and their interaction with the surrounding medium. In this paper, we determine these properties for PWN G54.1+0.3 by fitting its observed properties with a model for the dynamical and radiative evolution of a PWN inside an SNR. Our modeling suggests that the progenitor of G54.1+0.3 was an isolated ~15-20 Solar Mass star which exploded inside a massive star cluster, creating a neutron star initially spinning with period ~30-80ms. We also find that >99.9% of the pulsar's rotational energy is injected into the PWN as relativistic electrons and positrons whose energy spectrum is well characterized by a broken power-law. Lastly, we propose future observations which can both test the validity of this model and...

  15. FIRST INVESTIGATION OF THE COMBINED IMPACT OF IONIZING RADIATION AND MOMENTUM WINDS FROM A MASSIVE STAR ON A SELF-GRAVITATING CORE

    SciTech Connect (OSTI)

    Ngoumou, Judith; Hubber, David; Dale, James E.; Burkert, Andreas

    2015-01-01

    Massive stars shape the surrounding interstellar matter (ISM) by emitting ionizing photons and ejecting material through stellar winds. To study the impact of the momentum from the wind of a massive star on the surrounding neutral or ionized material, we implemented a new HEALPix-based momentum-conserving wind scheme in the smoothed particle hydrodynamics (SPH) code SEREN. A qualitative study of the impact of the feedback from an O7.5-like star on a self-gravitating sphere shows that on its own, the transfer of momentum from a wind onto cold surrounding gas has both a compressing and dispersing effect. It mostly affects gas at low and intermediate densities. When combined with a stellar source's ionizing ultraviolet (UV) radiation, we find the momentum-driven wind to have little direct effect on the gas. We conclude that during a massive star's main sequence, the UV ionizing radiation is the main feedback mechanism shaping and compressing the cold gas. Overall, the wind's effects on the dense gas dynamics and on the triggering of star formation are very modest. The structures formed in the ionization-only simulation and in the combined feedback simulation are remarkably similar. However, in the combined feedback case, different SPH particles end up being compressed. This indicates that the microphysics of gas mixing differ between the two feedback simulations and that the winds can contribute to the localized redistribution and reshuffling of gas.

  16. The Interaction of Venus-like, M-dwarf Planets with the Stellar Wind of Their Host Star

    E-Print Network [OSTI]

    Cohen, O; Drake, J J; Glocer, A; Garraffo, C; Bell, J M; Gombosi, T I

    2015-01-01

    We study the interaction between the atmospheres of Venus-like, non-magnetized exoplanets orbiting an M-dwarf star, and the stellar wind using a multi-species Magnetohydrodynaic (MHD) model. We focus our investigation on the effect of enhanced stellar wind and enhanced EUV flux as the planetary distance from the star decreases. Our simulations reveal different topologies of the planetary space environment for sub- and super-Alfvenic stellar wind conditions, which could lead to dynamic energy deposition in to the atmosphere during the transition along the planetary orbit. We find that the stellar wind penetration for non-magnetized planets is very deep, up to a few hundreds of kilometers. We estimate a lower limit for the atmospheric mass-loss rate and find that it is insignificant over the lifetime of the planet. However, we predict that when accounting for atmospheric ion acceleration, a significant amount of the planetary atmosphere could be eroded over the course of a billion years.

  17. Asterospheric magnetic fields and winds of cool stars1 Carolus J. Schrijver, Marc L. DeRosa, and Alan M. Title

    E-Print Network [OSTI]

    Schrijver, Karel

    -like magnetically active stars, by combining empirical relationships between rotation rate and mass loss, angular-star wind scales linearly with the unsigned surface magnetic flux density, as does that needed to heat magnetic field with the embedded coronal plasma, which is heated throughout the corona, and accelerated

  18. X-RAY EMISSION-LINE PROFILE MODELING OF O STARS: FITTING A SPHERICALLY SYMMETRIC ANALYTIC WIND-SHOCK MODEL TO THE CHANDRA SPECTRUM OF PUPPIS

    E-Print Network [OSTI]

    Cohen, David

    X-RAY EMISSION-LINE PROFILE MODELING OF O STARS: FITTING A SPHERICALLY SYMMETRIC ANALYTIC WIND Received 2002 November 22; accepted 2003 March 17 ABSTRACT X-ray emission-line profiles provide the most. INTRODUCTION The nature of the copious soft X-ray emission from hot stars has been a long-standing controversy

  19. Line-driven winds revisited in the context of Be stars: ?-slow solutions with high k values

    SciTech Connect (OSTI)

    Silaj, J.; Jones, C. E.; Curé, M.

    2014-11-01

    The standard, or fast, solutions of m-CAK line-driven wind theory cannot account for slowly outflowing disks like the ones that surround Be stars. It has been previously shown that there exists another family of solutions—the ?-slow solutions—that is characterized by much slower terminal velocities and higher mass-loss rates. We have solved the one-dimensional m-CAK hydrodynamical equation of rotating radiation-driven winds for this latter solution, starting from standard values of the line force parameters (?, k, and ?), and then systematically varying the values of ? and k. Terminal velocities and mass-loss rates that are in good agreement with those found in Be stars are obtained from the solutions with lower ? and higher k values. Furthermore, the equatorial densities of such solutions are comparable to those that are typically assumed in ad hoc models. For very high values of k, we find that the wind solutions exhibit a new kind of behavior.

  20. The interplay of disk wind and dynamical ejecta in the aftermath of neutron star - black hole mergers

    E-Print Network [OSTI]

    Rodrigo Fernández; Eliot Quataert; Josiah Schwab; Daniel Kasen; Stephan Rosswog

    2015-02-04

    We explore the evolution of the different ejecta components generated during the merger of a neutron star (NS) and a black hole (BH). Our focus is the interplay between material ejected dynamically during the merger, and the wind launched on a viscous timescale by the remnant accretion disk. These components are expected to contribute to an electromagnetic transient and to produce r-process elements, each with a different signature when considered separately. Here we introduce a two-step approach to investigate their combined evolution, using two- and three-dimensional hydrodynamic simulations. Starting from the output of a merger simulation, we identify each component in the initial condition based on its phase space distribution, and evolve the accretion disk in axisymmetry. The wind blown from this disk is injected into a three-dimensional computational domain where the dynamical ejecta is evolved. We find that the wind can suppress fallback accretion on timescales longer than ~100 ms. Due to self-similar viscous evolution, the disk accretion at late times nevertheless approaches a power-law time dependence $\\propto t^{-2.2}$. This can power some late-time GRB engine activity, although the available energy is significantly less than in traditional fallback models. Inclusion of radioactive heating due to the r-process does not significantly affect the fallback accretion rate or the disk wind. We do not find any significant modification to the wind properties at large radius due to interaction with the dynamical ejecta. This is a consequence of the different expansion velocities of the two components.

  1. Shape and evolution of wind-blown bubbles of massive stars: on the effect of the interstellar magnetic field

    E-Print Network [OSTI]

    van Marle, Allard Jan; Marcowith, Alexandre

    2015-01-01

    The winds of massive stars create large (>10 pc) bubbles around their progenitors. As these bubbles expand they encounter the interstellar coherent magnetic field which, depending on its strength, can influence the shape of the bubble. We wish to investigate if, and how much, the interstellar magnetic field can contribute to the shape of an expanding circumstellar bubble around a massive star. We use the MPI-AMRVAC code to make magneto-hydrodynamical simulations of bubbles, using a single star model, combined with several different field strengths: B=5, 10, and 20 muG for the interstellar magnetic field. This covers the typical field strengths of the interstellar magnetic fields found in the galactic disk and bulge. Furthermore, we present two simulations that include both a 5 muG interstellar magnetic field and a 10,000 K interstellar medium and two different ISM densities to demonstrate how the magnetic field can combine with other external factors to influnece the morphology of the circumstellar bubbles. O...

  2. For an electronic version of this poster, paper preprints, and updates, visit http://www.sccs.swarthmore.edu/~roban/x-ray/ or http://astro.swarthmore.edu/~cohen/ X-ray Emission Line Profile Modeling of O stars: Puppis as a Wind-Shock Source

    E-Print Network [OSTI]

    Cohen, David

    ://www.sccs.swarthmore.edu/~roban/x-ray/ or http://astro.swarthmore.edu/~cohen/ X-ray Emission Line Profile Modeling of O stars: Puppis as a Wind and Astronomy; £ Bartol Research Institute, University of Delaware Hot-star winds ¤ Massive (up to 60 ¥ ¦ ), hot (§©¨ K) stars are extremely luminous (up to !"¦ ). ¤ Their intense radiation drives massive winds (up to

  3. Neutrino signatures and the neutrino-driven wind in Binary Neutron Star Mergers

    E-Print Network [OSTI]

    Luc Dessart; Christian Ott; Adam Burrows; Stefan Rosswog; Eli Livne

    2008-06-26

    We present VULCAN/2D multi-group flux-limited-diffusion radiation hydrodynamics simulations of binary neutron star (BNS) mergers, using the Shen equation of state, covering ~100 ms, and starting from azimuthal-averaged 2D slices obtained from 3D SPH simulations of Rosswog & Price for 1.4 Msun (baryonic) neutron stars with no initial spins, co-rotating spins, and counter-rotating spins. Snapshots are post-processed at 10 ms intervals with a multi-angle neutrino-transport solver. We find polar-enhanced neutrino luminosities, dominated by $\\bar{\

  4. MAGNETICALLY DRIVEN WINDS FROM DIFFERENTIALLY ROTATING NEUTRON STARS AND X-RAY AFTERGLOWS OF SHORT GAMMA-RAY BURSTS

    SciTech Connect (OSTI)

    Siegel, Daniel M.; Ciolfi, Riccardo; Rezzolla, Luciano [Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, D-14476 Potsdam-Golm (Germany)

    2014-04-10

    Besides being among the most promising sources of gravitational waves, merging neutron star binaries also represent a leading scenario to explain the phenomenology of short gamma-ray bursts (SGRBs). Recent observations have revealed a large subclass of SGRBs with roughly constant luminosity in their X-ray afterglows, lasting 10-10{sup 4} s. These features are generally taken as evidence of a long-lived central engine powered by the magnetic spin-down of a uniformly rotating, magnetized object. We propose a different scenario in which the central engine powering the X-ray emission is a differentially rotating hypermassive neutron star (HMNS) that launches a quasi-isotropic and baryon-loaded wind driven by the magnetic field, which is built-up through differential rotation. Our model is supported by long-term, three-dimensional, general-relativistic, and ideal magnetohydrodynamic simulations, showing that this isotropic emission is a very robust feature. For a given HMNS, the presence of a collimated component depends sensitively on the initial magnetic field geometry, while the stationary electromagnetic luminosity depends only on the magnetic energy initially stored in the system. We show that our model is compatible with the observed timescales and luminosities and express the latter in terms of a simple scaling relation.

  5. Large-scale environments of binary AGB stars probed by Herschel. II: Two companions interacting with the wind of pi1 Gruis

    E-Print Network [OSTI]

    Mayer, A; Paladini, C; Kerschbaum, F; Pourbaix, D; Siopis, C; Ottensamer, R; Me?ina, M; Cox, N L J; Groenewegen, M A T; Klotz, D; Sadowski, G; Spang, A; Cruzalèbes, P; Waelkens, C

    2014-01-01

    Context. The Mass loss of Evolved StarS (MESS) sample observed with PACS on board the Herschel Space Observatory revealed that several asymptotic giant branch (AGB) stars are surrounded by an asymmetric circumstellar envelope (CSE) whose morphology is most likely caused by the interaction with a stellar companion. The evolution of AGB stars in binary systems plays a crucial role in understanding the formation of asymmetries in planetary nebul{\\ae} (PNe), but at present, only a handful of cases are known where the interaction of a companion with the stellar AGB wind is observed. Aims. We probe the environment of the very evolved AGB star $\\pi^1$ Gruis on large and small scales to identify the triggers of the observed asymmetries. Methods. Observations made with Herschel/PACS at 70 $\\mu$m and 160 $\\mu$m picture the large-scale environment of $\\pi^1$ Gru. The close surroundings of the star are probed by interferometric observations from the VLTI/AMBER archive. An analysis of the proper motion data of Hipparcos a...

  6. Physiological Ageing as it is Related to Gene Function in the Lone Star Tick, Amblyomma americanum 

    E-Print Network [OSTI]

    Catena, Amanda M.

    2010-07-14

    and appeared to remain at those low levels for the duration of the study. The female experimental group differed from the other three groups by gradually upregulating tick actin during the study. 19 Fig. 7. Four graphs plotting electrophoresis gel band...

  7. "Climate Wise" in the Lone Star State: A Successful Partnership for Energy Efficiency in Austin, Texas 

    E-Print Network [OSTI]

    Allen, S. J.; Schare, S.

    1997-01-01

    The City of Austin, Texas is forming partnerships with local companies to lower energy consumption and improve environmental performance within the industrial sector. As a local government participant in the federal Climate Wise program, Austin...

  8. Policy Recommendations for Establishing the LoneSTAR Monitoring and Analysis Program 

    E-Print Network [OSTI]

    Claridge, D. E.; O'Neal, D. L.; Turner, W. D.

    1989-01-01

    The major objectives of the Monitoring and Analysis Program (MAP) should be to: Verify energy and dollar savings of the retrofits; Reduce energy costs by identifying operational and maintenance improvements at facilities receiving retrofits; Improve...

  9. Water content and wind acceleration in the envelope around the oxygen-rich AGB star IK Tau as seen by Herschel/HIFI

    E-Print Network [OSTI]

    Decin, L; De Beck, E; Lombaert, R; de Koter, A; Waters, L B F M

    2010-01-01

    During their asymptotic giant branch, evolution low-mass stars lose a significant fraction of their mass through an intense wind, enriching the interstellar medium with products of nucleosynthesis. We observed the nearby oxygen-rich asymptotic giant branch star IK Tau using the high-resolution HIFI spectrometer onboard Herschel. We report on the first detection of H_2^{16}O and the rarer isotopologues H_2^{17}O and H_2^{18}O in both the ortho and para states. We deduce a total water content (relative to molecular hydrogen) of 6.6x10^{-5}, and an ortho-to-para ratio of 3:1. These results are consistent with the formation of H_2O in thermodynamical chemical equilibrium at photospheric temperatures, and does not require pulsationally induced non-equilibrium chemistry, vaporization of icy bodies or grain surface reactions. High-excitation lines of 12CO, 13CO, 28SiO, 29SiO, 30SiO, HCN, and SO have also been detected. From the observed line widths, the acceleration region in the inner wind zone can be characterized...

  10. X-ray spectral residuals in NGC 5408 X-1: diffuse emission from star formation, or the signature of a super-Eddington wind?

    E-Print Network [OSTI]

    Sutton, Andrew D; Middleton, Matthew J

    2015-01-01

    If ultraluminous X-ray sources (ULXs) are powered by accretion onto stellar remnant black holes, then many must be accreting at super-Eddington rates. It is predicted that such high accretion rates should give rise to massive, radiatively-driven winds. However, observational evidence of a wind, in the form of absorption or emission features, has remained elusive. As such, the reported detection of X-ray spectral residuals in XMM-Newton spectra of NGC 5408 X-1, which could be related to absorption in a wind is potentially very exciting. However, it has previously been assumed by several authors that these features simply originate from background diffuse plasma emission related to star-formation in the ULX's host galaxy. In this work we utilise the spatial resolving power of Chandra to test whether we can rule out this latter interpretation. We demonstrate that the majority of the luminosity in these spectral features is emitted from a highly localised region close to the ULX, and appears point-like even with ...

  11. HIGH-RESOLUTION X-RAY SPECTROSCOPY REVEALS THE SPECIAL NATURE OF WOLF-RAYET STAR WINDS

    E-Print Network [OSTI]

    Oskinova, L. M.

    We present the first high-resolution X-ray spectrum of a putatively single Wolf-Rayet (WR) star. 400 ks observations of WR 6 by the XMM-Newton telescope resulted in a superb quality high-resolution X-ray spectrum. Spectral ...

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

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room News PublicationsAudits & InspectionsBeryllium and ChronicBestBeyond the Lone-Pair Model

  13. Wind Power

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

    Wind Power Bioenergy Power Systems Wind Power Wind Power Main Page Outreach Programs Image Gallery FAQs Links Software Hydro Power INL Home Wind Power Introduction The Wind Power...

  14. X-ray Spectroscopy of O Supergiant Winds: Shock Physics, Clumping, and Mass-Loss Rates

    E-Print Network [OSTI]

    Cohen, David

    X-ray Spectroscopy of O Supergiant Winds: Shock Physics, Clumping, and Mass-Loss Rates David Cohen-ray emission: wind shocks 1. X-ray constraints on the shocked wind plasma 2. X-ray absorption as a mass. Adiabatic shocks Open questions: very dense winds (WR stars); low density winds (B stars); magnetic OB stars

  15. X-rays from Hot Stars: Stellar Astronomy Research with

    E-Print Network [OSTI]

    Cohen, David

    emission lines Hot stars*: massive outflows ("stellar winds") ­ are the x-rays associated with these winds can actually take an image of its "wind nebula" ­ in all other cases, we infer the presence of a wind a model for fitting the detailed shapes of x-ray emission line profiles from hot star winds The very hot

  16. Lookout Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLone

  17. CONSTRAINTS ON POROSITY AND MASS LOSS IN O-STAR WINDS FROM THE MODELING OF X-RAY EMISSION LINE PROFILE SHAPES

    SciTech Connect (OSTI)

    Leutenegger, Maurice A.; Sundqvist, Jon O.; Owocki, Stanley P.

    2013-06-10

    We fit X-ray emission line profiles in high resolution XMM-Newton and Chandra grating spectra of the early O supergiant {zeta} Pup with models that include the effects of porosity in the stellar wind. We explore the effects of porosity due to both spherical and flattened clumps. We find that porosity models with flattened clumps oriented parallel to the photosphere provide poor fits to observed line shapes. However, porosity models with isotropic clumps can provide acceptable fits to observed line shapes, but only if the porosity effect is moderate. We quantify the degeneracy between porosity effects from isotropic clumps and the mass-loss rate inferred from the X-ray line shapes, and we show that only modest increases in the mass-loss rate ({approx}< 40%) are allowed if moderate porosity effects (h{sub {infinity}} {approx}< R{sub *}) are assumed to be important. Large porosity lengths, and thus strong porosity effects, are ruled out regardless of assumptions about clump shape. Thus, X-ray mass-loss rate estimates are relatively insensitive to both optically thin and optically thick clumping. This supports the use of X-ray spectroscopy as a mass-loss rate calibration for bright, nearby O stars.

  18. FORMATION OF SiC GRAINS IN PULSATION-ENHANCED DUST-DRIVEN WIND AROUND CARBON-RICH ASYMPTOTIC GIANT BRANCH STARS

    SciTech Connect (OSTI)

    Yasuda, Yuki; Kozasa, Takashi, E-mail: yuki@antares-a.sci.hokudai.ac.jp [Department of Natural History Sciences, Faculty of Science, Hokkaido University, Sapporo 060-0810 (Japan)

    2012-02-01

    We investigate the formation of silicon carbide (SiC) grains in the framework of dust-driven wind around pulsating carbon-rich asymptotic giant branch (C-rich AGB) stars to reveal not only the amount but also the size distribution. Two cases are considered for the nucleation process: one is the local thermal equilibrium (LTE) case where the vibration temperature of SiC clusters T{sub v} is equal to the gas temperature as usual, and another is the non-LTE case in which T{sub v} is assumed to be the same as the temperature of small SiC grains. The results of the hydrodynamical calculations for a model with stellar parameters of mass M{sub *} = 1.0 M{sub Sun }, luminosity L{sub *} = 10{sup 4} L{sub Sun }, effective temperature T{sub eff} = 2600 K, C/O ratio = 1.4, and pulsation period P = 650 days show the following: in the LTE case, SiC grains condense in accelerated outflowing gas after the formation of carbon grains, and the resulting averaged mass ratio of SiC to carbon grains of {approx}10{sup -8} is too small to reproduce the value of 0.01-0.3, which is inferred from the radiative transfer models. On the other hand, in the non-LTE case, the formation region of the SiC grains is more internal and/or almost identical to that of the carbon grains due to the so-called inverse greenhouse effect. The mass ratio of SiC to carbon grains averaged at the outer boundary ranges from 0.098 to 0.23 for the sticking probability {alpha}{sub s} = 0.1-1.0. The size distributions with the peak at {approx}0.2-0.3 {mu}m in radius cover the range of size derived from the analysis of the presolar SiC grains. Thus, the difference between the temperatures of the small cluster and gas plays a crucial role in the formation process of SiC grains around C-rich AGB stars, and this aspect should be explored for the formation process of dust grains in astrophysical environments.

  19. Wind anisotropy and stellar evolution

    E-Print Network [OSTI]

    Cyril Georgy; Georges Meynet; André Maeder

    2008-07-31

    Mass loss is a determinant factor which strongly affects the evolution and the fate of massive stars. At low metallicity, stars are supposed to rotate faster than at the solar one. This favors the existence of stars near the critical velocity. In this rotation regime, the deformation of the stellar surface becomes important, and wind anisotropy develops. Polar winds are expected to be dominant for fast rotating hot stars. These polar winds allow the star to lose large quantities of mass and still retain a high angular momentum, and they modifie the evolution of the surface velocity and the final angular momentum kept in the star's core. We show here how these winds affect the final stages of massive stars, according to our knowledge about Gamma Ray Bursts. Computation of theoretical Gamma Ray Bursts rate indicates that our models have too fast rotating cores, and that we need to include an additional effect to spin them down. Magnetic fields in stars act in this direction, and we show how they modify the evolution of massive star up to the final stages.

  20. Massive Stars as Cosmic Engines Proceedings IAU Symposium No. 250, 2008

    E-Print Network [OSTI]

    Cohen, David

    wind shock scenario. After their magnetic fields dissipate, older O stars produce X-rays via shock heating in their unstable stellar winds. Here too I will use X-ray spectroscopy and numerical modeling ­ magnetic fields ­ MHD ­ shock waves ­ stars: early type ­ stars: mass loss ­ stars: winds, outflows ­ x

  1. Massive Stars as Cosmic Engines Proceedings IAU Symposium No. 250, 2007

    E-Print Network [OSTI]

    Cohen, David

    wind shock scenario. After their magnetic fields dissipate, older O stars produce X- rays via shock heating in their unstable stellar winds. Here too I will use X-ray spectroscopy and numerical modeling ­ magnetic fields ­ MHD ­ shock waves ­ stars: early type ­ stars: mass loss ­ stars: winds, outflows ­ X

  2. Wind Tunnel 

    E-Print Network [OSTI]

    Unknown

    2011-08-17

    The increased interest in the offshore wind resource in both industry and academic and the extension of the wind field where offshore wind turbine can be deployed has stimulated quite a number of offshore wind turbines concepts. This thesis presents...

  3. Evaluation and Demonstration of BMPs for Cattle on Grazing Lands for the Lone Star Healthy Streams Program 

    E-Print Network [OSTI]

    Wagner, K.; Redmon, L.; Gentry, T.; Clary, C.

    2013-01-01

    Committee .......................................................... 9 Subtask 1.8 Development of the final project report ........................................................................... 9 Task 2: Quality Assurance... Report ? November 15, 2010 TWRI Submitted Quarter 2 Progress Report ? March 14, 2011 TWRI Submitted Quarter 3 Progress Report ? June 14, 2011 TWRI Submitted Quarter 4 Progress Report ? September 15, 2011 TWRI Submitted Quarter 5 Progress Report...

  4. WIND ENERGY Wind Energ. (2014)

    E-Print Network [OSTI]

    Peinke, Joachim

    2014-01-01

    to generate in this way wind speed fluctuations with similar statistics as observed in nature. Forces wereWIND ENERGY Wind Energ. (2014) Published online in Wiley Online Library (wileyonlinelibrary wind inflow conditions M. R. Luhur, J. Peinke, J. Schneemann and M. Wächter ForWind-Center for Wind

  5. Loranger Power Generation Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History ViewInformationWindsCompressedListguided wavesLoneLorain County,2

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

    E-Print Network [OSTI]

    Barnes, Joshua Edward

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

  7. Collegiate Wind Competition Wind Tunnel Specifications | Department...

    Energy Savers [EERE]

    Wind Tunnel Specifications Collegiate Wind Competition Wind Tunnel Specifications Collegiate Wind Competition Wind Tunnel Specifications Teams competing in the U.S. Department of...

  8. WIND ENERGY Wind Energ. (2014)

    E-Print Network [OSTI]

    2014-01-01

    , wind power has been expanding globally in recent years and it has become a dominant renewable energy the turbulent atmosphere and the wind turbine wake in order to optimize the design of the wind turbine as wellWIND ENERGY Wind Energ. (2014) Published online in Wiley Online Library (wileyonlinelibrary

  9. wind energy

    National Nuclear Security Administration (NNSA)

    5%2A en Pantex to Become Wind Energy Research Center http:nnsa.energy.govfieldofficesnponpopressreleasespantex-become-wind-energy-research-center

  10. Carina Nebula: star formation region, d ~ 7000 light years HST: Carina Nebula

    E-Print Network [OSTI]

    Cohen, David

    to the Galaxy via their stellar winds eta Carina #12;The massive stars are also strong X-ray sources Carina: HST already yielded new information about this star's wind Tr 14 in Carina: Chandra X-ray Observatory #12;1. How do massive stars produce their strong X-ray emission? 2. How strong are their stellar winds (what

  11. Carina Nebula: star formation region, d ~ 7000 light years HST: Carina Nebula

    E-Print Network [OSTI]

    Cohen, David

    produce heavy elements and return them to the Galaxy via their stellar winds eta Carina #12;The massive an astrophysicist HST: Carina Nebula I work mainly on massive stars, especially their radiation-driven winds I star in the cluster provides new information about this star's wind Tr 14 in Carina: Chandra X

  12. Cool Stars in Hot Places

    E-Print Network [OSTI]

    S. T. Megeath; E. Gaidos; J. J. Hester; F. C. Adams; J. Bally; J. -E. Lee; S. Wolk

    2007-04-08

    During the last three decades, evidence has mounted that star and planet formation is not an isolated process, but is influenced by current and previous generations of stars. Although cool stars form in a range of environments, from isolated globules to rich embedded clusters, the influences of other stars on cool star and planet formation may be most significant in embedded clusters, where hundreds to thousands of cool stars form in close proximity to OB stars. At the cool stars 14 meeting, a splinter session was convened to discuss the role of environment in the formation of cool stars and planetary systems; with an emphasis on the ``hot'' environment found in rich clusters. We review here the basic results, ideas and questions presented at the session. We have organized this contribution into five basic questions: what is the typical environment of cool star formation, what role do hot star play in cool star formation, what role does environment play in planet formation, what is the role of hot star winds and supernovae, and what was the formation environment of the Sun? The intention is to review progress made in addressing each question, and to underscore areas of agreement and contention.

  13. Wind Farm

    Broader source: Energy.gov [DOE]

    The wind farm in Greensburg, Kansas, was completed in spring 2010, and consists of ten 1.25 megawatt (MW) wind turbines that supply enough electricity to power every house, business, and municipal...

  14. EVIDENCE FOR A WEAK WIND FROM THE YOUNG SUN

    SciTech Connect (OSTI)

    Wood, Brian E.; Müller, Hans-Reinhard; Redfield, Seth; Edelman, Eric

    2014-02-01

    The early history of the solar wind has remained largely a mystery due to the difficulty of detecting winds around young stars that can serve as analogs for the young Sun. Here we report on the detection of a wind from the 500 Myr old solar analog ?{sup 1} UMa (G1.5 V), using spectroscopic observations from the Hubble Space Telescope. We detect H I Ly? absorption from the interaction region between the stellar wind and interstellar medium, i.e., the stellar astrosphere. With the assistance of hydrodynamic models of the ?{sup 1} UMa astrosphere, we infer a wind only half as strong as the solar wind for this star. This suggests that the Sun and solar-like stars do not have particularly strong coronal winds in their youth.

  15. Nucleosynthesis in neutrino-driven winds in hypernovae

    E-Print Network [OSTI]

    Fujibayashi, Sho; Sekiguchi, Yuichiro

    2015-01-01

    We investigate the nucleosynthesis in the neutrino-driven winds blown off from a $3M_\\odot$ massive proto-neutron star temporarily formed during the collapse of a $100M_\\odot$ star. Such massive proto-neutron stars would be formed in hypernovae. We construct steady and spherically symmetric wind solutions. We set large neutrino luminosities of $\\sim 10^{53}\\ {\\rm erg\\ s^{-1}}$ and average energies of electron neutrinos and antineutrinos in the ranges of $\\epsilon_{\

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

    SciTech Connect (OSTI)

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

    2014-11-10

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

  17. Wind Power Forecasting Data

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

    Operations Call 2012 Retrospective Reports 2012 Retrospective Reports 2011 Smart Grid Wind Integration Wind Integration Initiatives Wind Power Forecasting Wind Projects Email...

  18. Idaho_Wind_Data

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

    Site Bryans Run Cell Tower Site Wilson Peak Eckert Site Loertscher Boise State's Wind Data Link Wind Power Idaho Wind Data See also: Idaho Energy Resources - Wind, American...

  19. Neutrino-driven wind and wind termination shock in supernova cores

    E-Print Network [OSTI]

    A. Arcones; L. Scheck; H. -Th. Janka

    2006-12-22

    The neutrino-driven wind from a nascent neutron star at the center of a supernova expands into the earlier ejecta of the explosion. Upon collision with this slower matter the wind material is decelerated in a wind termination shock. By means of hydrodynamic simulations in spherical symmetry we demonstrate that this can lead to a large increase of the wind entropy, density, and temperature, and to a strong deceleration of the wind expansion. The consequences of this phenomenon for the possible r-process nucleosynthesis in the late wind still need to be explored in detail. Two-dimensional models show that the wind-ejecta collision is highly anisotropic and could lead to a directional dependence of the nucleosynthesis even if the neutrino-driven wind itself is spherically symmetric.

  20. Carina Nebula: star formation region, d ~ 7000 light years HST: Carina Nebula

    E-Print Network [OSTI]

    Cohen, David

    and return them to the Galaxy via their stellar winds eta Carina #12;The massive stars are also strong X in the cluster has already yielded new information about this star's wind Tr 14 in Carina: Chandra X produce their strong X-ray emission? What's the physics of the wind shocks? 2. How strong

  1. Wind anisotropies and GRB progenitors

    E-Print Network [OSTI]

    Georges Meynet; Andre Maeder

    2007-01-17

    We study the effect of wind anisotropies on the stellar evolution leading to collapsars. Rotating models of a 60 M$_\\odot$ star with $\\Omega/\\Omega_{\\rm crit}=0.75$ on the ZAMS, accounting for shellular rotation and a magnetic field, with and without wind anisotropies, are computed at $Z$=0.002 until the end of the core He-burning phase. Only the models accounting for the effects of the wind anisotropies retain enough angular momentum in their core to produce a Gamma Ray Burst (GRB). The chemical composition is such that a type Ic supernova event occurs. Wind anisotropies appear to be a key physical ingredient in the scenario leading to long GRBs.

  2. Wind Tunnel 

    E-Print Network [OSTI]

    Unknown

    2011-08-17

    Simulation of Cooling Effect of Wind Tower on Passively Ventilated Building John Seryak Kelly Kissock Project Engineer Associate Professor Department of Mechanical and Aerospace Engineering University of Dayton... Dayton, Ohio ABSTRACT Traditional buildings are cooled and ventilated by mechanically induced drafts. Natural ventilation aspires to cool and ventilate a building by natural means, such as cross ventilation or wind towers, without mechanical...

  3. X-ray emission from O stars

    E-Print Network [OSTI]

    David H. Cohen

    2008-02-01

    Young O stars are strong, hard, and variable X-ray sources, properties which strongly affect their circumstellar and galactic environments. After ~1 Myr, these stars settle down to become steady sources of soft X-rays. I use high-resolution X-ray spectroscopy and MHD modeling to show that young O stars like theta-1 Ori C are well explained by the magnetically channeled wind shock scenario. After their magnetic fields dissipate, older O stars produce X-rays via shock heating in their unstable stellar winds. Here too I use X-ray spectroscopy and numerical modeling to confirm this scenario. In addition to elucidating the nature and cause of the O star X-ray emission, modeling of the high-resolution X-ray spectra of O supergiants provides strong evidence that mass-loss rates of these O stars have been overestimated.

  4. Offshore Wind Power USA

    Broader source: Energy.gov [DOE]

    The Offshore Wind Power USA conference provides the latest offshore wind market updates and forecasts.

  5. X-rays from Massive StarsX-rays from Massive Stars David CohenDavid Cohen

    E-Print Network [OSTI]

    Cohen, David

    star wind Radiation line driving is inherently unstable:Radiation line driving is inherently unstable Owocki (U. Del.) #12;continuum absorption in the bulk wind preferentially absorbs redcontinuum absorption in the bulk wind preferentially absorbs red shifted photons from the far side of the windshifted photons from

  6. WINDS, B-FIELDS, AND MAGNETOTAILS OF PULSARS M. M. Romanova, G. A. Chulsky, and R. V. E. Lovelace

    E-Print Network [OSTI]

    WINDS, B-FIELDS, AND MAGNETOTAILS OF PULSARS M. M. Romanova, G. A. Chulsky, and R. V. E. Lovelace to the acceleration and radiation of particles in the relativistic wind and in the magnetotail of the star. We cylinder, the star's rotation acts to wind up the magnetic field to form a predominantly azimuthal, slowly

  7. Wind Energy Leasing Handbook

    E-Print Network [OSTI]

    Balasundaram, Balabhaskar "Baski"

    Wind Energy Leasing Handbook Wind Energy Leasing Handbook E-1033 Oklahoma Cooperative Extension?..................................................................................................................... 31 What do wind developers consider in locating wind energy projects?............................................................................................ 37 How do companies and individuals invest in wind energy projects?....................................................................

  8. Quantitative Analysis of the Resolved X-ray Emission Line Profiles of O Stars

    E-Print Network [OSTI]

    Cohen, David

    -rays in context 3. Hot-star winds 4. Emission line shapes: constraints on hot plasma distribution and wind mass-resolution X-ray observations: not enough attenuation of soft X-rays by the overlying wind to accommodate a corona #12;#12;Radiation-driven winds of O and early-B stars blue velocity (km/s) red wavelength O4 I B0

  9. NEW X-RAY DETECTIONS OF WNL STARS

    SciTech Connect (OSTI)

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

    2012-05-15

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

  10. The Be Phenomenon in Early-Type Stars, IAU Colloquium 175 ASP Conference Series, Vol. 214, 2000

    E-Print Network [OSTI]

    Cohen, David

    . The Be X-ray properties are discussed in the context of wind-shock X-ray emission from normal OB stars are thought to come from shocks in the massive winds of these stars. The generally accepted shock mechanism can understood in terms of the wind-shock emission that is invoked to explain the X-rays emitted by O

  11. HighResolution Spectroscopic Diagnostics of the Hot Plasma in the Stellar Wind of ee Canis Majoris (B2 II) David H. Cohen, Stanley P. Owocki, Joseph P. Cassinelli, & Joseph J. MacFarlane

    E-Print Network [OSTI]

    Cohen, David

    High­Resolution Spectroscopic Diagnostics of the Hot Plasma in the Stellar Wind of ee Canis Majoris structure in the shocked winds of hot stars. OB stars are characterized by fast line­driven winds, and our­ray spectroscopy is vital for determining in what part of the wind the X­rays are produced, for quantifying

  12. Wind Vision: Impacts

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

    Wind Vision: Impacts Rich Tusing New West Technologies, LLC For EERE's Wind and Water Power Technologies Office July 15, 2015 2 | Wind and Water Power Technologies Office...

  13. Wind Program News

    SciTech Connect (OSTI)

    2012-01-06

    Stay current on the news about the wind side of the Wind and Water Power Program and important wind energy events around the U.S.

  14. Wind Power Link

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

    Wind Power Links These other web sites may provide additional information of interest: American Wind Energy Association Idaho Department of Energy Wind Power Information Utah...

  15. Energy 101: Wind Turbines

    ScienceCinema (OSTI)

    None

    2013-05-29

    See how wind turbines generate clean electricity from the power of the wind. Highlighted are the various parts and mechanisms of a modern wind turbine.

  16. Energy 101: Wind Turbines

    SciTech Connect (OSTI)

    None

    2011-01-01

    See how wind turbines generate clean electricity from the power of the wind. Highlighted are the various parts and mechanisms of a modern wind turbine.

  17. Vandenberg_Wind_Data

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

    Air Force and other branches of the Department of Defense for several years doing wind data collection and assessment, wind power feasibility studies, and wind farm design....

  18. WIND VARIABILITY IN BZ CAMELOPARDALIS

    SciTech Connect (OSTI)

    Honeycutt, R. K.; Kafka, S.; Robertson, J. W. E-mail: skafka@dtm.ciw.edu

    2013-02-01

    Sequences of spectra of the nova-like cataclysmic variable (CV) BZ Cam were acquired on nine nights in 2005-2006 in order to study the time development of episodes of wind activity known to occur frequently in this star. We confirm the results of Ringwald and Naylor that the P-Cygni absorption components of the lines mostly evolve from higher expansion velocity to lower velocity as an episode progresses. We also commonly find blueshifted emission components in the H{alpha} line profile, whose velocities and durations strongly suggest that they are also due to the wind. Curiously, Ringwald and Naylor reported common occurrences of redshifted H{alpha} emission components in their BZ Cam spectra. We have attributed these emission components in H{alpha} to occasions when gas concentrations in the bipolar wind (both front side and back side) become manifested as emission lines as they move beyond the disk's outer edge. We also suggest, based on changes in the P-Cygni profiles during an episode, that the progression from larger to smaller expansion velocities is due to the higher velocity portions of a wind concentration moving beyond the edge of the continuum light of the disk first, leaving a net redward shift of the remaining absorption profile. We derive a new orbital ephemeris for BZ Cam, using the radial velocity of the core of the He I {lambda}5876 line, finding P = 0.15353(4). Using this period, the wind episodes in BZ Cam are found to be concentrated near the inferior conjunction of the emission line source. This result helps confirm that the winds in nova-like CVs are often phase dependent, in spite of the puzzling implication that such winds lack axisymmetry. We argue that the radiation-driven wind in BZ Cam receives an initial boost by acting on gas that has been lifted above the disk by the interaction of the accretion stream with the disk, thereby imposing flickering timescales onto the wind events, as well as leading to an orbital modulation of the wind due to the non-axisymmetric nature of the stream/disk interaction. Simultaneous photometry and spectroscopy were acquired on three nights in order to test the possible connection between flickering continuum light and the strength of the front-side wind. We found strong agreement on one night, some agreement on another, and no agreement on the third. We suggest that some flickering events lead to only back-side winds which will not have associated P-Cygni profiles.

  19. Wind emission of OB supergiants and the influence of clumping

    E-Print Network [OSTI]

    Michaela Kraus; Jiri Kubat; Jiri Krticka

    2007-08-06

    The influence of the wind to the total continuum of OB supergiants is discussed. For wind velocity distributions with \\beta > 1.0, the wind can have strong influence to the total continuum emission, even at optical wavelengths. Comparing the continuum emission of clumped and unclumped winds, especially for stars with high \\beta values, delivers flux differences of up to 30% with maximum in the near-IR. Continuum observations at these wavelengths are therefore an ideal tool to discriminate between clumped and unclumped winds of OB supergiants.

  20. Wind turbine

    DOE Patents [OSTI]

    Cheney, Jr., Marvin C. (Glastonbury, CT)

    1982-01-01

    A wind turbine of the type having an airfoil blade (15) mounted on a flexible beam (20) and a pitch governor (55) which selectively, torsionally twists the flexible beam in response to wind turbine speed thereby setting blade pitch, is provided with a limiter (85) which restricts unwanted pitch change at operating speeds due to torsional creep of the flexible beam. The limiter allows twisting of the beam by the governor under excessive wind velocity conditions to orient the blades in stall pitch positions, thereby preventing overspeed operation of the turbine. In the preferred embodiment, the pitch governor comprises a pendulum (65,70) which responds to changing rotor speed by pivotal movement, the limiter comprising a resilient member (90) which engages an end of the pendulum to restrict further movement thereof, and in turn restrict beam creep and unwanted blade pitch misadjustment.

  1. Wind Program: Wind Vision | Department of Energy

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

    Wind Vision: A New Era for Wind Power in the United States With more than 4.5% of the nation's electricity supplied by wind energy today, the Department of Energy has collaborated...

  2. Wind | Department of Energy

    Office of Environmental Management (EM)

    Science & Innovation Energy Sources Renewable Energy Wind Wind Wind The United States is home to one of the largest and fastest growing wind markets in the world. To stay...

  3. Danehy Park Wind Turbine Project Preliminary Assessment Report

    E-Print Network [OSTI]

    Danehy Park Wind Turbine Project Preliminary Assessment Report Danehy Park Project Group Wind turbine. Katherine Dykes and Sungho Lee for their leadership, guidance, and feedback. #12;1 Introduction sensors were mounted is marked with a yellow star. #12;2 Turbine Evaluation Set This report evaluates

  4. Wind Integration National Dataset (WIND) Toolkit

    Office of Energy Efficiency and Renewable Energy (EERE)

    For utility companies, grid operators and other stakeholders interested in wind energy integration, collecting large quantities of high quality data on wind energy resources is vitally important....

  5. Matter & Energy Wind Energy

    E-Print Network [OSTI]

    Shepelyansky, Dima

    intuitive experience of a small wind not creating a storm, and that wind needs to reach a certain threshold

  6. Accretion-Powered Stellar Winds II: Numerical Solutions for Stellar Wind Torques

    E-Print Network [OSTI]

    Sean Matt; Ralph E. Pudritz

    2008-01-18

    [Abridged] In order to explain the slow rotation observed in a large fraction of accreting pre-main-sequence stars (CTTSs), we explore the role of stellar winds in torquing down the stars. For this mechanism to be effective, the stellar winds need to have relatively high outflow rates, and thus would likely be powered by the accretion process itself. Here, we use numerical magnetohydrodynamical simulations to compute detailed 2-dimensional (axisymmetric) stellar wind solutions, in order to determine the spin down torque on the star. We explore a range of parameters relevant for CTTSs, including variations in the stellar mass, radius, spin rate, surface magnetic field strength, the mass loss rate, and wind acceleration rate. We also consider both dipole and quadrupole magnetic field geometries. Our simulations indicate that the stellar wind torque is of sufficient magnitude to be important for spinning down a ``typical'' CTTS, for a mass loss rate of $\\sim 10^{-9} M_\\odot$ yr$^{-1}$. The winds are wide-angle, self-collimated flows, as expected of magnetic rotator winds with moderately fast rotation. The cases with quadrupolar field produce a much weaker torque than for a dipole with the same surface field strength, demonstrating that magnetic geometry plays a fundamental role in determining the torque. Cases with varying wind acceleration rate show much smaller variations in the torque suggesting that the details of the wind driving are less important. We use our computed results to fit a semi-analytic formula for the effective Alfv\\'en radius in the wind, as well as the torque. This allows for considerable predictive power, and is an improvement over existing approximations.

  7. Accretion-powered Stellar Winds as a Solution to the Stellar Angular Momentum Problem

    E-Print Network [OSTI]

    Sean Matt; Ralph E. Pudritz

    2005-10-03

    We compare the angular momentum extracted by a wind from a pre-main-sequence star to the torques arising from the interaction between the star and its Keplerian accretion disk. We find that the wind alone can counteract the spin-up torque from mass accretion, solving the mystery of why accreting pre-main-sequence stars are observed to spin at less than 10% of break-up speed, provided that the mass outflow rate in the stellar winds is ~10% of the accretion rate. We suggest that such massive winds will be driven by some fraction $\\epsilon$ of the accretion power. For observationally constrained typical parameters of classical T-Tauri stars, $\\epsilon$ needs to be between a few and a few tens of percent. In this scenario, efficient braking of the star will terminate simultaneously with accretion, as is usually assumed to explain the rotation velocities of stars in young clusters.

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

    SciTech Connect (OSTI)

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

    2014-05-05

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

  9. The r-Process in Black Hole Winds

    E-Print Network [OSTI]

    Shinya Wanajo; Hans-Thomas Janka

    2010-06-11

    All the current r-process scenarios relevant to core-collapse supernovae are facing severe difficulties. In particular, recent core-collapse simulations with neutrino transport show no sign of a neutron-rich wind from the proto-neutron star. In this paper, we discuss nucleosynthesis of the r-process in an alternative astrophysical site, "black hole winds", which are the neutrino-driven outflow from the accretion torus around a black hole. This condition is assumed to be realized in double neutron star mergers, neutron star - black hole mergers, or hypernovae.

  10. Wolf-Rayet stars in the Small Magellanic Cloud: I. Analysis of the single WN stars

    E-Print Network [OSTI]

    Hainich, R; Todt, H; Shenar, T; Sander, A; Hamann, W -R

    2015-01-01

    Wolf-Rayet (WR) stars have a severe impact on their environments owing to their strong ionizing radiation fields and powerful stellar winds. Since these winds are considered to be driven by radiation pressure, it is theoretically expected that the degree of the wind mass-loss depends on the initial metallicity of WR stars. Following our comprehensive studies of WR stars in the Milky Way, M31, and the LMC, we derive stellar parameters and mass-loss rates for all seven putatively single WN stars known in the SMC. Based on these data, we discuss the impact of a low-metallicity environment on the mass loss and evolution of WR stars. The quantitative analysis of the WN stars is performed with the Potsdam Wolf-Rayet (PoWR) model atmosphere code. The physical properties of our program stars are obtained from fitting synthetic spectra to multi-band observations. In all SMC WN stars, a considerable surface hydrogen abundance is detectable. The majority of these objects have stellar temperatures exceeding 75 kK, while ...

  11. Wind Technologies & Evolving Opportunities (Presentation)

    SciTech Connect (OSTI)

    Robichaud, R.

    2014-07-01

    This presentation covers opportunities for wind technology; wind energy market trends; an overview of the National Wind Technology Center near Boulder, Colorado; wind energy price and cost trends; wind turbine technology improvements; and wind resource characterization improvements.

  12. Hydrodynamics and High-Energy Physics of WR Colliding Winds

    E-Print Network [OSTI]

    Vladimir V. Usov

    1994-05-29

    One of the main properties of Wolf-Rayet (WR) stars is a very intense outflow of gas. No less than 40\\% \\ of WR stars belong to binary systems. Young massive O and B stars are the secondary components of such systems. OB stars also have an intense stellar wind. If the intensities of the stellar winds of WR and OB stars are more or less comparable or if the distance between the components of the binary is large enough, the winds flowing out of WR and OB stars can collide and the shock waves are formed. In the shock the gas is heated to temperature $\\sim 10^7$ K and generates X-ray emission. Stellar wind collision may be responsible not only for the X-ray emission of WR + OB binaries and for their radio, IR and $\\gamma$-ray emision as well. Stellar wind collision, gas heating, particle acceleration, and generation of X-ray, $\\gamma$-ray, radio and IR emission in WR + OB binaries are discussed.

  13. Sequentially Triggered Star Formation in OB Associations

    E-Print Network [OSTI]

    Thomas Preibisch; Hans Zinnecker

    2006-10-27

    We discuss observational evidence for sequential and triggered star formation in OB associations. We first review the star formation process in the Scorpius-Centaurus OB association, the nearest OB association to the Sun, where several recent extensive studies have allowed us to reconstruct the star formation history in a rather detailed way. We then compare the observational results with those obtained for other OB associations and with recent models of rapid cloud and star formation in the turbulent interstellar medium. We conclude that the formation of whole OB subgroups (each consisting of several thousand stars) requires large-scale triggering mechanisms such as shocks from expanding wind and supernova driven superbubbles surrounding older subgroups. Other triggering mechanisms, like radiatively driven implosion of globules, also operate, but seem to be secondary processes, forming only small stellar groups rather than whole OB subgroups with thousands of stars.

  14. Sandia Energy - Grid System Planning for Wind: Wind Generator...

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

    Grid System Planning for Wind: Wind Generator Modeling Home Stationary Power Energy Conversion Efficiency Wind Energy Siting and Barrier Mitigation Grid System Planning for Wind:...

  15. 2015 Iowa Wind Power Conference and Iowa Wind Energy Association...

    Office of Environmental Management (EM)

    2015 Iowa Wind Power Conference and Iowa Wind Energy Association Midwest Regional Energy Job Fair 2015 Iowa Wind Power Conference and Iowa Wind Energy Association Midwest Regional...

  16. Wind tunnel performance data for the Darrieus wind turbine with...

    Office of Scientific and Technical Information (OSTI)

    Wind tunnel performance data for the Darrieus wind turbine with NACA 0012 blades Citation Details In-Document Search Title: Wind tunnel performance data for the Darrieus wind...

  17. A National Offshore Wind Strategy: Creating an Offshore Wind...

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

    A National Offshore Wind Strategy: Creating an Offshore Wind Energy Industry in the United States A National Offshore Wind Strategy: Creating an Offshore Wind Energy Industry in...

  18. 20% Wind Energy by 2030 - Chapter 2: Wind Turbine Technology...

    Office of Environmental Management (EM)

    - Chapter 2: Wind Turbine Technology Summary Slides 20% Wind Energy by 2030 - Chapter 2: Wind Turbine Technology Summary Slides Summary slides for wind turbine technology, its...

  19. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    AWEA). 2009b. AWEA Small Wind Turbine Global Market Study:will ultimately benefit wind. Small Wind ITC: EESA 2008

  20. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    Public Service Wind Integration Cost Impact Study. Preparedequipment-related wind turbine costs, the overall importinstalled wind power project costs, wind turbine transaction

  1. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    Public Service Wind Integration Cost Impact Study. Preparedequipment-related wind turbine costs, the overall importinstalled wind power project costs, wind turbine transaction

  2. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    land- based wind energy technology. 2009 Wind TechnologiesRenewable Energy 2009 WIND TECHNOLOGIES MARKET REPORT AUGUSTfor a variety of energy technologies, including wind energy.

  3. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    land-based wind energy technology. 2011 Wind Technologiesfor a variety of energy technologies, including wind energy.Renewable Energy Laboratory’s National Wind Technology

  4. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    land-based wind energy technology. 2010 Wind Technologiesfor a variety of energy technologies, including wind energy.2010 Wind Technologies Market Report Federal Energy

  5. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    land-based wind energy technology. 2012 Wind Technologiesfor a variety of energy technologies, including wind energy.of Energy (DOE) Wind & Water Power Technology Office team

  6. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    wind power project costs, wind turbine transaction prices,increases in the cost of wind turbines over the last severaland components and wind turbine costs. Excluded from all

  7. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    A. 2010. Impact of Wind Energy Installations on DomesticJanuary 31, 2011. American Wind Energy Association (AWEA).D.C. : American Wind Energy Association. American Wind

  8. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    A. 2010. Impact of Wind Energy Installations on DomesticUniversity. American Wind Energy Association (AWEA). 2012a.D.C. : American Wind Energy Association. American Wind

  9. Wind Power Software

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

    Wind Analysis ms - 3.0MB Excel Excel Wind Analysis Presentation - 8.2MB PowerPoint Excel Wind Analysis With Power Curves Included - 3.7MB Excel WindR.exe - 44kB Weibull Excel Wind...

  10. Wind Integration

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home RoomPreservationBio-Inspired SolarAbout /Two0Photos andSeminarsDesign » DesignMay »helpWind

  11. Wind Power

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorking WithTelecentricNCubicthe FOIA?ResourceMeasurement Buoy AdvancesWind

  12. Theoretical mass loss rates of cool main-sequence stars

    E-Print Network [OSTI]

    V. Holzwarth; M. Jardine

    2006-11-14

    We develop a model for the wind properties of cool main-sequence stars, which comprises their wind ram pressures, mass fluxes, and terminal wind velocities. The wind properties are determined through a polytropic magnetised wind model, assuming power laws for the dependence of the thermal and magnetic wind parameters on the stellar rotation rate. We use empirical data to constrain theoretical wind scenarios, which are characterised by different rates of increase of the wind temperature, wind density, and magnetic field strength. Scenarios based on moderate rates of increase yield wind ram pressures in agreement with most empirical constraints, but cannot account for some moderately rotating targets, whose high apparent mass loss rates are inconsistent with observed coronal X-ray and magnetic properties. For fast magnetic rotators, the magneto-centrifugal driving of the outflow can produce terminal wind velocities far in excess of the surface escape velocity. Disregarding this aspect in the analyses of wind ram pressures leads to overestimations of stellar mass loss rates. The predicted mass loss rates of cool main-sequence stars do not exceed about ten times the solar value. Our results are in contrast with previous investigations, which found a strong increase of the stellar mass loss rates with the coronal X-ray flux. Owing to the weaker dependence, we expect the impact of stellar winds on planetary atmospheres to be less severe and the detectability of magnetospheric radio emission to be lower then previously suggested. Considering the rotational evolution of a one solar-mass star, the mass loss rates and the wind ram pressures are highest during the pre-main sequence phase.

  13. Carina Nebula: star formation region, d ~ 7000 lt yr HST: Carina Nebula

    E-Print Network [OSTI]

    Cohen, David

    and return them to the Galaxy via their stellar winds HST: Carina Nebula #12;The massive stars are also their strong X-ray emission? 2. How strong are their stellar winds (what are their mass-loss rates)? Two spectra #12;we make models #12;#12;models make predictions #12;wind mass-loss rate #12;we compare

  14. Quantitative Analysis of the Resolved X-ray Emission Line Profiles of O Stars

    E-Print Network [OSTI]

    Cohen, David

    Department of Physics & Astronomy Swarthmore College June 21, 2007 - Potsdam - Clumping in Hot-Star Winds with Maurice Leutenegger (Columbia University) #12;1. The wind profile model and quantitative model fitting 2. Smooth wind models: constraints on mass-loss rates 3. Models with porosity: the * - h trade-off 4. A note

  15. The Surprisingly Dynamic LastYears in the Lives of Massive Stars

    E-Print Network [OSTI]

    Wurtele, Jonathan

    Powered by Interaction with Ambient Gas (Type IIn SNe) · Interacting SNe: SN shock runs into dense wind closer to the star with stellar wind not ISM #12;diff R2 `mfpc exp R vsh R Mvsh 4c 1/2 100 AU · Interacting SNe: SN shock runs into dense wind at ~ 102-3 AU and KE thermal energy, radiation Supernovae

  16. X-ray emission line profile modeling of hot stars Roban H. Kramer

    E-Print Network [OSTI]

    Cohen, David

    stars. These outflows, or winds, are driven by radiation pressure and carry a tremendous amount of kinetic energy, which can be converted to x rays by shock-heating even a small fraction of the wind plasma. The unshocked, cold wind is a source of continuum opacity to the x rays generated in the shock-heated portion

  17. Wind Power Today

    SciTech Connect (OSTI)

    Not Available

    2006-05-01

    Wind Power Today is an annual publication that provides an overview of the wind energy research conducted by the U.S. Department of Energy Wind and Hydropower Technologies Program.

  18. The evolution of very massive stars

    E-Print Network [OSTI]

    H. Belkus; J. Van Bever; D. Vanbeveren

    2007-01-11

    Core collapse of dense massive star clusters is unavoidable and this leads to the formation of massive objects, with a mass up to 1000 $\\msun$ and even larger. When these objects become stars, stellar wind mass loss determines their evolution and final fate, and decides upon whether they form black holes (with normal mass or with intermediate mass) or explode as a pair instability supernova. In the present paper, we discuss the evolution of very massive stars and we present a convenient evolution recipe that can be implemented in a gravitational N-body code to study the dynamics of dense massive clusters.

  19. Scale Models & Wind Turbines

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

    Turbines * Readings about Cape Wind and other offshore and onshore siting debates for wind farms * Student Worksheet * A number of scale model items: Ken, Barbie or other dolls...

  20. Wind Power Outreach Campaign

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

    Wind Power Wind Power Main Page Outreach Programs Image Gallery FAQs Links Software Hydro Power INL Home Outreach Programs A team of educators and scientists from the Idaho...

  1. Wind/Hydro Study

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

    WindHydro Integration Feasibility Study Announcements (Updated July 8, 2010) The Final WindHydro Integration Feasibility Study Report, dated June 2, 2009, has been submitted to...

  2. Wind for Schools (Poster)

    SciTech Connect (OSTI)

    Baring-Gould, I.

    2010-05-01

    As the United States dramatically expands wind energy deployment, the industry is challenged with developing a skilled workforce and addressing public resistance. Wind Powering America's Wind for Schools project addresses these issues by developing Wind Application Centers (WACs) at universities; WAC students assist in implementing school wind turbines and participate in wind courses, by installing small wind turbines at community "host" schools, by implementing teacher training with interactive curricula at each host school. This poster provides an overview of the first two years of the Wind for Schools project, primarily supporting activities in Colorado, Kansas, Nebraska, South Dakota, Montana, and Idaho.

  3. Wind energy bibliography

    SciTech Connect (OSTI)

    1995-05-01

    This bibliography is designed to help the reader search for information on wind energy. The bibliography is intended to help several audiences, including engineers and scientists who may be unfamiliar with a particular aspect of wind energy, university researchers who are interested in this field, manufacturers who want to learn more about specific wind topics, and librarians who provide information to their clients. Topics covered range from the history of wind energy use to advanced wind turbine design. References for wind energy economics, the wind energy resource, and environmental and institutional issues related to wind energy are also included.

  4. Small Wind Conference 2015

    Broader source: Energy.gov [DOE]

    The Small Wind Conference brings together small wind installers, site assessors, manufacturers, dealers and distributors, supply chain stakeholders, educators, public benefits program managers, and...

  5. Wind Turbine Tribology Seminar

    Broader source: Energy.gov [DOE]

    Wind turbine reliability issues are often linked to failures of contacting components, such as bearings, gears, and actuators. Therefore, special consideration to tribological design in wind...

  6. For Cape Wind, Summer Breeze Makes Offshore Wind Feel Fine |...

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

    For Cape Wind, Summer Breeze Makes Offshore Wind Feel Fine For Cape Wind, Summer Breeze Makes Offshore Wind Feel Fine July 1, 2014 - 8:44am Addthis For Cape Wind, Summer Breeze...

  7. the risk issue of wind measurement for wind turbine operation

    E-Print Network [OSTI]

    Leu, Tzong-Shyng "Jeremy"

    Sciences, National Taiwan University #12;outline · Wind measurement in meteorology and wind farm design-related issues on wind turbine operation 3/31/2011 2 #12;WIND MEASUREMENT IN METEOROLOGY & WIND FARM DESIGN 3://www.atm.ncu.edu.tw/93/wind/ MM5 simulation (1996~2000 database) Wind speed (m/s) at 50mWind power (100W/m2) at 50m http://wind.itri.org.tw/wind

  8. 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.

  9. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    of Energy’s (DOE) Wind & Water Power Program. For reviewingwere funded by the Wind & Water Power Program, Office ofWind Technologies Market Report Wind Energy Web Sites U.S. Department of Energy Wind and Water Power

  10. Stellar feedback efficiencies: supernovae versus stellar winds

    E-Print Network [OSTI]

    Fierlinger, Katharina M; Ntormousi, Evangelia; Fierlinger, Peter; Schartmann, Marc; Ballone, Alessandro; Krause, Martin G H; Diehl, Roland

    2015-01-01

    Stellar winds and supernova (SN) explosions of massive stars ("stellar feedback") create bubbles in the interstellar medium (ISM) and insert newly produced heavy elements and kinetic energy into their surroundings, possibly driving turbulence. Most of this energy is thermalized and immediately removed from the ISM by radiative cooling. The rest is available for driving ISM dynamics. In this work we estimate the amount of feedback energy retained as kinetic energy when the bubble walls have decelerated to the sound speed of the ambient medium. We show that the feedback of the most massive star outweighs the feedback from less massive stars. For a giant molecular cloud (GMC) mass of 1e5 solar masses (as e.g. found in the Orion GMCs) and a star formation efficiency of 8% the initial mass function predicts a most massive star of approximately 60 solar masses. For this stellar evolution model we test the dependence of the retained kinetic energy of the cold GMC gas on the inclusion of stellar winds. In our model w...

  11. Estimation of Wind Speed in Connection to a Wind Turbine

    E-Print Network [OSTI]

    Estimation of Wind Speed in Connection to a Wind Turbine X. Ma #3; , N. K. Poulsen #3; , H. Bindner y December 20, 1995 Abstract The wind speed varies over the rotor plane of wind turbine making the wind speed on the rotor plane will be estimated by using a wind turbine as a wind measuring device

  12. Wind energy offers considerable promise; the wind itself is free,

    E-Print Network [OSTI]

    Langendoen, Koen

    Wind energy offers considerable promise; the wind itself is free, wind power is clean. One of these sources, wind energy, offers considerable promise; the wind itself is free, wind power is clean, and it is virtually inexhaustible. In recent years, research on wind energy has accelerated

  13. Wind Resource Maps (Postcard)

    SciTech Connect (OSTI)

    Not Available

    2011-07-01

    The U.S. Department of Energy's Wind Powering America initiative provides high-resolution wind maps and estimates of the wind resource potential that would be possible from development of the available windy land areas after excluding areas unlikely to be developed. This postcard is a marketing piece that stakeholders can provide to interested parties; it will guide them to Wind Powering America's online wind energy resource maps.

  14. Magnetically Confined Wind Shocks in X-rays - a Review

    E-Print Network [OSTI]

    ud-Doula, Asif

    2015-01-01

    A subset (~ 10%) of massive stars present strong, globally ordered (mostly dipolar) magnetic fields. The trapping and channeling of their stellar winds in closed magnetic loops leads to magnetically confined wind shocks (MCWS), with pre-shock flow speeds that are some fraction of the wind terminal speed. These shocks generate hot plasma, a source of X-rays. In the last decade, several developments took place, notably the determination of the hot plasma properties for a large sample of objects using XMM-Newton and Chandra, as well as fully self-consistent MHD modelling and the identification of shock retreat effects in weak winds. Despite a few exceptions, the combination of magnetic confinement, shock retreat and rotation effects seems to be able to account for X-ray emission in massive OB stars. Here we review these new observational and theoretical aspects of this X-ray emission and envisage some perspectives for the next generation of X-ray observatories.

  15. Sinomatech Wind Power Blade aka Sinoma Science Technology Wind...

    Open Energy Info (EERE)

    Sinomatech Wind Power Blade aka Sinoma Science Technology Wind Turbine Blade Co Ltd Jump to: navigation, search Name: Sinomatech Wind Power Blade (aka Sinoma Science & Technology...

  16. Wind energy offers considerable promise

    E-Print Network [OSTI]

    Langendoen, Koen

    Wind energy offers considerable promise: the wind itself is free, wind power is clean: the wind itself is free, wind power is clean, and it is inexhaustible. In recent years, research on wind · Wind farm aerodynamics Rotor Design · Aerodynamics · Structure and design · Composite design, material

  17. Wind energy offers considerable promise

    E-Print Network [OSTI]

    Langendoen, Koen

    Wind energy offers considerable promise: the wind itself is free, wind power is clean, wind power is clean, and it is inexhaustible. In recent years, research on wind energy has accelerated that are offered are: Wind Physics · Atmospheric aerodynamics and turbulence · Wind farm aerodynamics Rotor Design

  18. Massive Stars in the Arches Cluster

    E-Print Network [OSTI]

    Figer, D F; Gilmore, D; Morris, M; Kim, S S; Serabyn, E; McLean, I S; Gilbert, A M; Graham, J R; Larkin, J E; Levenson, N A; Teplitz, H I; Figer, Donald F.; Najarro, Francisco; Gilmore, Diane; Morris, Mark; Kim, Sungsoo S.; Serabyn, Eugene; Lean, Ian S. Mc; Gilbert, Andrea M.; Graham, James R.; Larkin, James E.; Teplitz, Harry I.

    2002-01-01

    We present and use new spectra and narrow-band images, along with previously published broad-band images, of stars in the Arches cluster to extract photometry, astrometry, equivalent width, and velocity information. The data are interpreted with a wind/atmosphere code to determine stellar temperatures, luminosities, mass-loss rates, and abundances. We have doubled the number of known emission-line stars, and we have also made the first spectroscopic identification of the main sequence for any population in the Galactic Center. We conclude that the most massive stars are bona-fide Wolf-Rayet (WR) stars and are some of the most massive stars known, having M_{initial} > 100 Msun, and prodigious winds, Mdot > 10^{-5} Msun yr^{-1}, that are enriched with helium and nitrogen; with these identifications, the Arches cluster contains about 5% of all known WR stars in the Galaxy. We find an upper limit to the velocity dispersion of 22 kms^{-1}, implying an upper limit to the cluster mass of 7(10^4) Msun within a radius...

  19. Period change and stellar evolution of $\\beta$ Cephei stars

    E-Print Network [OSTI]

    Neilson, Hilding R

    2015-01-01

    The $\\beta$ Cephei stars represent an important class of massive star pulsators probing the evolution of B-type stars and the transition from main sequence to hydrogen-shell burning evolution. By understanding $\\beta$ Cep stars, we gain insights into the detailed physics of massive star evolution such as rotational mixing, convective core overshooting, magnetic fields and stellar winds, all of which play important roles. Similarly, modeling their pulsation provides additional information into their interior structures. Furthermore, measurements of the rate of change of pulsation period offer a direct measure of $\\beta$ Cephei stellar evolution. In this work, we compute state-of-the-art stellar evolution models assuming different amounts of initial rotation and convective core overshoot and measure theoretical rates of period change for which we compare to rates previously measured for a sample of $\\beta$ Cephei stars. The results of this comparison are mixed. For three stars, the rates are too small to infer ...

  20. WIND DATA REPORT Presque Isle

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Presque Isle June 1, 2005 ­ August 31, 2005 Prepared for United States Department...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distributions

  1. WIND DATA REPORT Presque Isle

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Presque Isle December 1, 2004 ­ February 28, 2005 Prepared for United States.................................................................................................................... 10 Wind Speed Time Series........................................................................................................... 10 Wind Speed Distributions

  2. WIND DATA REPORT Presque Isle

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Presque Isle December 1, 2004 ­ December 1, 2005 Prepared for United States ......................................................................................................... 9 Wind Speed Time Series........................................................................................................... 10 Wind Speed Distributions

  3. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island June 1, 2003 ­ August 31, 2003 Prepared for Massachusetts...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distribution

  4. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island December 1, 2003 ­ February 29, 2004 Prepared for Massachusetts.................................................................................................................... 11 Wind Speed Time Series........................................................................................................... 11 Wind Speed Distribution

  5. WIND DATA REPORT Presque Isle

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Presque Isle March 1, 2005 ­ May 31, 2005 Prepared for United States Department.................................................................................................................... 10 Wind Speed Time Series........................................................................................................... 10 Wind Speed Distributions

  6. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island March 1, 2003 ­ May 31, 2003 Prepared for Massachusetts Technology...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distributions

  7. WIND DATA REPORT FALMOUTH, MA

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT FALMOUTH, MA June1, 2004 to August 31, 2004. Prepared for Massachusetts Technology...................................................................................................................... 8 Wind Speed Time Series............................................................................................................. 8 Wind Speed Distributions

  8. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island September 1, 2003 ­ November 30, 2003 Prepared for Massachusetts...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distribution

  9. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island March 1, 2004 ­ May 31, 2004 Prepared for Massachusetts Technology...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distribution

  10. WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Thompson Island June 1, 2004 ­ August 31, 2004 Prepared for Massachusetts...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distribution

  11. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    with the section on offshore wind; Donna Heimiller and Billyof 2012, global cumulative offshore wind capacity stood ats (DOE’s) investments in offshore wind energy research and

  12. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    11 “advanced-stage” offshore wind project proposals totalingcontinued in 2008 (see Offshore Wind Development Activities,Market Report Offshore Wind Development Activities In

  13. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    for deepwater offshore wind and tidal energy demonstrationand Minnesota (12%). Offshore Wind Power Project and Policythe emergence of an offshore wind power market still faces

  14. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    and Minnesota (12%). Offshore Wind Power Project and Policythe emergence of an offshore wind power market still facesexists in developing offshore wind energy in several parts

  15. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    of Energy?s (DOE) Wind & Water Power Program. For reviewingfor offshore wind power development in federal waters fromof Water and Power (LADWP). 2011. Completion of Wind Power

  16. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    Table 8 Figure 30. Wind Integration Costs at Various LevelsOperations and Maintenance Costs Wind project operations andPublic Service Wind Integration Cost Impact Study. Prepared

  17. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    charging wind power projects for balancing services. 81 BPA,in balancing reserves with increased wind power penetrationin balancing reserves with increased wind power penetration

  18. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    charging wind power projects for balancing services. 88 BPA,in balancing reserves with increased wind power penetrationin balancing reserves with increased wind power penetration

  19. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    Xcel Energy. 2011. Wind Induced Coal Plant Cyclingand the Implications of Wind Curtailment for Public Serviceof Colorado 2 GW and 3 GW Wind Integration Cost Study.

  20. Wind Farms in North America

    E-Print Network [OSTI]

    Hoen, Ben

    2014-01-01

    Opinion About Large Offshore Wind Power: Underlying Factors.Delaware Opinion on Offshore Wind Power - Interim Report.Newark, DE. 16 pages. Global Wind Energy Council (GWEC) (

  1. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    be provided by wind power generators to provide frequencyof wind power capacity in that state) because generatorsgenerators to provide the needed flexibility to integrate wind power.

  2. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    2010. Status of Centralized Wind Power Forecasting in NorthInterconnection Policies and Wind Power: A Discussion ofLADWP). 2011. Completion of Wind Power Project Brings More

  3. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    and K. Porter. 2011. Wind Power and Electricity Markets.The Effects of Integrating Wind Power on Transmission System41 6. Wind Power Price

  4. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    exists in developing offshore wind energy in several partsexclusively on offshore wind energy will be published laterexclusively on offshore wind energy will be published later

  5. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    assistance with the offshore wind energy discussion; Donnaactivity in the offshore wind energy sector. Data fromexpanded discussion of offshore wind energy development, and

  6. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    exists in developing offshore wind energy in several partsstrides relating to offshore wind energy have been madeactivity in the offshore wind energy sector. Data from

  7. WIND DATA REPORT Nantucket, MA

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Nantucket, MA March 1st 2006 to May 31th 2006 Prepared for Massachusetts.................................................................................................................... 11 Wind Speed Time Series........................................................................................................... 11 Wind Speed Distribut

  8. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    2010. International Wind Energy Development: World MarketUniversity. American Wind Energy Association (AWEA). 2010a.Washington, DC: American Wind Energy Association. American

  9. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    2008. Washington, DC: American Wind Energy Association.American Wind Energy Association ( AWEA). 2009b. AWEA SmallWashington, DC: American Wind Energy Association. Bolinger,

  10. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    2008. Washington, DC: American Wind Energy Association.American Wind Energy Association ( AWEA).2009b. AWEA Small Wind Turbine Global Market Study: Year

  11. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    Prepared for the Utility Wind Integration Group. Arlington,Consult. 2010. International Wind Energy Development: WorldUBS Global I/O: Global Wind Sector. UBS Investment Research.

  12. AWEA Wind Energy Fall Symposium

    Broader source: Energy.gov [DOE]

    The AWEA Wind Energy Fall Symposium gathers wind energy professionals for informal yet productive interactions with industry peers. Jose Zayas, Director, Wind & Water Power Technologies Office,...

  13. Star Power

    ScienceCinema (OSTI)

    None

    2014-11-18

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

  14. 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.

  15. Quantitative Analysis of Resolved X-ray Emission Line Profiles of O Stars: Profile Symmetry: Clumping and

    E-Print Network [OSTI]

    Cohen, David

    snapshot from a 1-D rad-hydro simulation of an O star wind. Note the discontinuities in velocity. These are shock fronts, compressing and heating the wind, producing x-rays. There are dense inter-shock regions, containing most of the wind mass, in which cold material provides a source of photoelectric absorption #12

  16. Wind Power Career Chat

    SciTech Connect (OSTI)

    L. Flowers

    2011-01-01

    This document will teach students about careers in the wind energy industry. Wind energy, both land-based and offshore, is expected to provide thousands of new jobs in the next several decades. Wind energy companies are growing rapidly to meet America's demand for clean, renewable, and domestic energy. These companies need skilled professionals. Wind power careers will require educated people from a variety of areas. Trained and qualified workers manufacture, construct, operate, and manage wind energy facilities. The nation will also need skilled researchers, scientists, and engineers to plan and develop the next generation of wind energy technologies.

  17. Wind energy information guide

    SciTech Connect (OSTI)

    1996-04-01

    This book is divided into nine chapters. Chapters 1--8 provide background and annotated references on wind energy research, development, and commercialization. Chapter 9 lists additional sources of printed information and relevant organizations. Four indices provide alphabetical access to authors, organizations, computer models and design tools, and subjects. A list of abbreviations and acronyms is also included. Chapter topics include: introduction; economics of using wind energy; wind energy resources; wind turbine design, development, and testing; applications; environmental issues of wind power; institutional issues; and wind energy systems development.

  18. X-ray Emission from Isolated Be Stars

    E-Print Network [OSTI]

    David H. Cohen

    2000-08-22

    I discuss the X-ray observations of Be stars, and how their properties compare to non-emission B stars. I focus on several specific stars that show high flux levels and variability but also report on several interesting survey results. The Be X-ray properties are discussed in the context of wind-shock X-ray emission from normal OB stars as well as in the context of general mechanisms that have been proposed to explain the Be phenomenon. Finally, I conclude with a discussion of the spectral diagnostics that will be available from the new generation of X-ray telescopes.

  19. EERE 2014 Wind Technologies Market Report Finds Wind Power at...

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

    2014 Wind Technologies Market Report Finds Wind Power at Record Low Prices EERE 2014 Wind Technologies Market Report Finds Wind Power at Record Low Prices August 10, 2015 - 11:00am...

  20. 20% Wind Energy by 2030: Increasing Wind Energy's Contribution...

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

    20% Wind Energy by 2030: Increasing Wind Energy's Contribution to U.S. Electricity Supply 20% Wind Energy by 2030: Increasing Wind Energy's Contribution to U.S. Electricity Supply...

  1. 2008 Wind Energy Projects, Wind Powering America (Poster)

    SciTech Connect (OSTI)

    Not Available

    2009-01-01

    The Wind Powering America program produces a poster at the end of every calendar year that depicts new U.S. wind energy projects. The 2008 poster includes the following projects: Stetson Wind Farm in Maine; Dutch Hill Wind Farm in New York; Grand Ridge Wind Energy Center in Illinois; Hooper Bay, Alaska; Forestburg, South Dakota; Elbow Creek Wind Project in Texas; Glacier Wind Farm in Montana; Wray, Colorado; Smoky Hills Wind Farm in Kansas; Forbes Park Wind Project in Massachusetts; Spanish Fork, Utah; Goodland Wind Farm in Indiana; and the Tatanka Wind Energy Project on the border of North Dakota and South Dakota.

  2. Eruptive Mass Loss in Very Massive Stars and Population III Stars

    E-Print Network [OSTI]

    Nathan Smith

    2006-07-24

    I discuss the role played by short-duration eruptive mass loss in the evolution of very massive stars. Giant eruptions of Luminous Blue Variables (LBVs) like the 19th century event of eta Carinae can remove large quantities of mass almost instantaneously, making them significant in stellar evolution. They can potentially remove much more mass from the star than line-driven winds, especially if stellar winds are highly clumped such that previous estimates of O star mass-loss rates need to be revised downward. When seen in other galaxies as ``supernova impostors'', these LBV eruptions typically last for less than a decade, and they can remove of order 10 Msun as indicated by massive nebulae around LBVs. Such extreme mass-loss rates cannot be driven by radiation pressure on spectral lines, because the lines will completely saturate during the events. Instead, these outbursts must either be continuum-driven super-Eddington winds or outright hydrodynamic explosions, both of which are insensitive to metallicity. As such, this eruptive mode of mass loss could also play a pivotal role in the evolution and ultimate fate of massive metal-poor stars in the early universe. If they occur in these Population III stars, such eruptions would also profoundly affect the chemical yield and types of remnants from early supernovae and hypernovae thought to be the origin of long gamma ray bursts.

  3. Massive stars and the energy balance of the ISM. I. The impact of an isolated 60 Msun star

    E-Print Network [OSTI]

    Tim Freyer; Gerhard Hensler; Harold W. Yorke

    2003-06-25

    We present results of numerical simulations carried out with a 2D radiation hydrodynamics code in order to study the impact of massive stars on their surrounding interstellar medium. This first paper deals with the evolution of the circumstellar gas around an isolated 60 Msun star. The interaction of the photoionized HII region with the stellar wind bubble forms a variety of interesting structures like shells, clouds, fingers, and spokes. These results demonstrate that complex structures found in HII regions are not necessarily relics from the time before the gas became ionized but may result from dynamical processes during the course of the HII region evolution. We have also analyzed the transfer and deposit of the stellar wind and radiation energy into the circumstellar medium until the star explodes as a supernova. Although the total mechanical wind energy supplied by the star is negligible compared to the accumulated energy of the Lyman continuum photons, the kinetic energy imparted to the circumstellar gas over the star's lifetime is 4 times higher than for a comparable windless simulation. Furthermore, the thermal energy of warm photoionized gas is lower by some 55%. Our results document the necessity to consider both ionizing radiation and stellar winds for an appropriate description of the interaction of OB stars with their circumstellar environment.

  4. Distributed Wind 2015

    Broader source: Energy.gov [DOE]

    Distributed Wind 2015 is committed to the advancement of both distributed and community wind energy. This two day event includes a Business Conference with sessions focused on advancing the...

  5. Wind Power FAQ

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

    Power Frequently Asked Questions QUESTION: Why was the time stamp on my first wind explorer data chip incorrect? ANSWER: You need to program the proper date and time in the wind...

  6. Airplane and the wind

    E-Print Network [OSTI]

    Airplane and the wind. An airplane starts from the point A and flies to B. The speed of the airplane with respect to the air is v (constant). There is also a wind of

  7. NREL: Wind Research - Events

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

    Events Below are upcoming events related to wind energy technology. December 2015 Wind and Water Power Small Business Voucher Open House December 2, 2015, 9:00 - 1:00 MST Boulder,...

  8. WINDExchange: Learn About Wind

    Wind Powering America (EERE)

    wind turbines in a row at sunset. The sky is varying hues of orange and the sun is halfway past the horizon. Wind power comes in many sizes. Here, several...

  9. Residential Wind Power

    E-Print Network [OSTI]

    Willis, Gary

    2011-12-16

    This research study will explore the use of residential wind power and associated engineering and environmental issues. There is various wind power generating devices available to the consumer. The study will discuss the dependencies of human...

  10. After the Wind Storm 

    E-Print Network [OSTI]

    Unknown

    2011-09-05

    Accidents and hazards continue to plague the construction industry. One often overlooked hazard to workers is the potential for flying debris and materials during high winds. This research was designed to evaluate the wind velocity required...

  11. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    AWEA). 2009b. AWEA Small Wind Turbine Global Market Study:will ultimately benefit wind. Small Wind ITC: EESA 2008to be relatively small, whereas the impacts of wind on load-

  12. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    AWEA). 2010. AWEA Small Wind Turbine Global Market Survey,levels. Small Wind Turbines Small wind turbines can providebelow summarizes sales of small wind turbines, 100 kW and

  13. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    wind project costs, wind turbine transaction prices, projectincreases in the cost of wind turbines over the last severalO&M costs given the dramatic changes in wind turbine

  14. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    AWEA’s Wind Energy Weekly, DOE/EPRI’s Turbine Verification10% Wind Energy Penetration New large-scale 8 wind turbines100 wind turbine installed at the National Renewable Energy

  15. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    Sites U.S. Department of Energy Wind Program wind.energy.govA. 2010. Impact of Wind Energy Installations on DomesticUniversity. American Wind Energy Association (AWEA). 2012a.

  16. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    AWEA). 2012b. 2011 U.S. Small Wind Turbine Market Report.a brief discussion on Small Wind This 100 kW thresholdAnnual Capacity (GW) Small Wind Turbines Small wind turbines

  17. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    a brief discussion on Small Wind Turbines is provided onO&M costs. 2012 Wind Technologies Market Report Small WindTurbines Small wind turbines can provide power directly to

  18. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    AWEA). 2010. AWEA Small Wind Turbine Global Market Survey,a brief discussion on Small Wind Turbines is provided onat 2008 and 2009 levels. Small Wind Turbines Small wind

  19. The magnetic field and wind confinement of b Cephei: new clues for interpreting the Be phenomenon?

    E-Print Network [OSTI]

    Donati, Jean-François

    The magnetic field and wind confinement of b Cephei: new clues for interpreting the Be phenomenon of the weakest detected to date, this magnetic field is strong enough to magnetically confine the wind of b Cep collected by Henrichs et al. and propose for this star a consistent model of the large-scale magnetic field

  20. The Fermi Bubbles as Starburst Wind Termination Shocks

    E-Print Network [OSTI]

    Lacki, Brian C

    2013-01-01

    The enhanced star formation in the inner 100 pc of the Galaxy launches a superwind, reaching ~1600 km/s for M82-like parameters. The ram pressure of the wind is very low compared to more powerful starburst winds. I show that halo gas stops the wind a few kpc from the Galactic Center. I argue that the termination shock accelerates cosmic rays, and that the resulting Inverse Compton gamma-rays are visible as the Fermi Bubbles. The Bubbles are thus wind bubbles, which the starburst can inflate within 10 Myr. They remain in steady state as long as the starburst lasts. The shock may accelerate PeV electrons and ultra-high energy protons. The Bubbles may be analogs of galactic wind termination shocks in the intergalactic medium. I discuss the advantages and problems of this model.

  1. Wind Webinar Text Version

    Broader source: Energy.gov [DOE]

    Download the text version of the audio from the DOE Office of Indian Energy webinar on wind renewable energy.

  2. Wind Tunnel Building - 7 

    E-Print Network [OSTI]

    Unknown

    2005-06-30

    or gravitational energy to some extent. Moreover, wave energy provides “15-20 times more available energy per square meter than either wind or solar” [1]. Of these the most commercially viable resources studied so far are ocean currents and waves. Some... limited commercial development and is therefore of more interest. Ocean waves arise from the transfer of energy from the sun to wind then water. Solar energy creates wind, which then blows over the ocean, converting wind energy to wave energy. Once...

  3. Wind powering America: Vermont

    SciTech Connect (OSTI)

    NREL

    2000-04-11

    Wind resources in the state of Vermont show great potential for wind energy development according to the wind resource assessment conducted by the state, its utilities, and NREL. This fact sheet provides a brief description of the resource assessment and a link to the resulting wind resource map produced by NREL. The fact sheet also provides a description of the state's net metering program, its financial incentives, and green power programs as well as a list of contacts for more information.

  4. WP2 IEA Wind Task 26:The Past and Future Cost of Wind Energy

    E-Print Network [OSTI]

    Lantz, Eric

    2014-01-01

    Prospects for Offshore Wind Farms. ” Wind Engineering, 28:Techniques for Offshore Wind Farms. ” Journal of Solar

  5. Wind Farms in North America

    E-Print Network [OSTI]

    Hoen, Ben

    2014-01-01

    Opinion About Large Offshore Wind Power: Underlying Factors.Delaware Opinion on Offshore Wind Power - Interim Report.

  6. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    by Canada (76%) and Mexico (17%). Wind turbine component30%), Mexico (21%), and China (21%)). Total wind turbine

  7. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    of larger balancing areas, the use of regional wind powerbalancing areas. The successful use of regional wind power

  8. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    directly charging wind power projects for balancing servicesin smaller balancing areas. The successful use of wind power

  9. Wind Farms in North America

    E-Print Network [OSTI]

    Hoen, Ben

    2014-01-01

    Public Opinion About Large Offshore Wind Power: UnderlyingA. (2007) Delaware Opinion on Offshore Wind Power - Interim

  10. Wind Farms in North America

    E-Print Network [OSTI]

    Hoen, Ben

    2014-01-01

    Renewable Energy (Wind and Water Technologies Program) ofWind Farms in North America 1 Ben Hoen Environmental Energy Technologies

  11. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    regulation and frequency response services charge to wind energyRegulation and Frequency Response Service rate for wind energy

  12. Wind for Schools Curriculum Brief

    SciTech Connect (OSTI)

    None

    2010-08-01

    This fact sheet provides an overview of wind energy curricula as it relates to the Wind for Schools project.

  13. Wind farm electrical system

    DOE Patents [OSTI]

    Erdman, William L.; Lettenmaier, Terry M.

    2006-07-04

    An approach to wind farm design using variable speed wind turbines with low pulse number electrical output. The output of multiple wind turbines are aggregated to create a high pulse number electrical output at a point of common coupling with a utility grid network. Power quality at each individual wind turbine falls short of utility standards, but the aggregated output at the point of common coupling is within acceptable tolerances for utility power quality. The approach for aggregating low pulse number electrical output from multiple wind turbines relies upon a pad mounted transformer at each wind turbine that performs phase multiplication on the output of each wind turbine. Phase multiplication converts a modified square wave from the wind turbine into a 6 pulse output. Phase shifting of the 6 pulse output from each wind turbine allows the aggregated output of multiple wind turbines to be a 24 pulse approximation of a sine wave. Additional filtering and VAR control is embedded within the wind farm to take advantage of the wind farm's electrical impedence characteristics to further enhance power quality at the point of common coupling.

  14. CONGRESSIONAL BRIEFING Offshore Wind

    E-Print Network [OSTI]

    Firestone, Jeremy

    CONGRESSIONAL BRIEFING Offshore Wind Lessons Learned from Europe: Reducing Costs and Creating Jobs Thursday, June 12, 2014 Capitol Visitors Center, Room SVC 215 Enough offshore wind capacity to power six the past decade. What has Europe learned that is applicable to a U.S. effort to deploy offshore wind off

  15. Wind Economic Development (Postcard)

    SciTech Connect (OSTI)

    Not Available

    2011-08-01

    The U.S. Department of Energy's Wind Powering America initiative provides information on the economic development benefits of wind energy. This postcard is a marketing piece that stakeholders can provide to interested parties; it will guide them to the economic development benefits section on the Wind Powering America website.

  16. Offshore Wind Geoff Sharples

    E-Print Network [OSTI]

    Kammen, Daniel M.

    Offshore Wind Geoff Sharples geoff@clearpathenergyllc.com #12;Frequently Unanswered Ques?ons · Why don't "they" build more offshore wind? · Why not make States Cape Wind PPA at 18 c/kWh #12;The cycle of non-innova?on Offshore

  17. Wind power outlook 2006

    SciTech Connect (OSTI)

    anon.

    2006-04-15

    This annual brochure provides the American Wind Energy Association's up-to-date assessment of the wind industry in the United States. This 2006 general assessment shows positive signs of growth, use and acceptance of wind energy as a vital component of the U.S. energy mix.

  18. Why do meteorologists use wind vanes? Wind vanes are used to determine the direction of the wind. Wind

    E-Print Network [OSTI]

    Nebraska-Lincoln, University of

    Fun Facts Why do meteorologists use wind vanes? Wind vanes are used to determine the direction of the wind. Wind· vanes are also called weather vanes. What do wind vanes look like on a weather station? Wind vanes that are on weather stations look a lot like the one you· made! The biggest differences

  19. On the nature of WO stars: a quantitative analysis of the WO3 star DR1 in IC 1613

    E-Print Network [OSTI]

    Tramper, F; Hartoog, O E; Sana, H; de Koter, A; Vink, J S; Ellerbroek, L E; Langer, N; Garcia, M; Kaper, L; de Mink, S E

    2013-01-01

    Context. Oxygen sequence Wolf-Rayet (WO) stars are thought to represent the final evolutionary stage of the most massive stars. The characteristic strong O vi emission possibly originates from an enhanced oxygen abundance in the stellar wind. Alternatively, the O vi emission can be caused by the high temperature of these stars, in which case the WO stars are the high-temperature extension of the more common carbon sequence Wolf-Rayet (WC) stars. Aims. By constraining the physical properties and evolutionary status of DR1, a WO star in the low-metallicity Local Group dwarf galaxy IC 1613 and one of only two objects of its class known in a SMC-like metallicity environment, we aim to investigate the nature of WO stars and their evolutionary connection with WC stars. Methods. We use the non-LTE atmosphere code cmfgen to model the observed spectrum of DR1 and to derive its stellar and wind parameters. We compare our values with other studies of WC and WO stars, as well as with the predictions of evolutionary model...

  20. Planet Migration and Disk Destruction due to Magneto-Centrifugal Stellar Winds

    E-Print Network [OSTI]

    R. V. E. Lovelace; M. M. Romanova; A. W. Barnard

    2008-06-25

    This paper investigates the influence of magneto-centrifugally driven or simply magnetic winds of rapidly-rotating, strongly-magnetized T Tauri stars in causing the inward or outward migration of close-in giant planets. The azimuthal ram pressure of the magnetized wind acting on the planet tends to increase the planet's angular momentum and cause outward migration if the star's rotation period $P_*$ is less than the planet's orbital period $P_p$. In the opposite case, $P_* > P_p$, the planet migrates inward. Thus, planets orbiting at distances larger (smaller) than $0.06 {\\rm AU}(P_*/5{\\rm d})^{2/3}$ tend to be pushed outward (inward), where $P_*$ is the rotation period of the star assumed to have the mass of the sun. The magnetic winds are likely to occur in T Tauri stars where the thermal speed of the gas close to the star is small, where the star's magnetic field is strong, and where the star rotates rapidly. The time-scale for appreciable radial motion of the planet is estimated as $\\sim 2 - 20$ Myr. A sufficiently massive close-in planet may cause tidal locking and once this happens the radial migration due to the magnetic wind ceases. The magnetic winds are expected to be important for planet migration for the case of a multipolar magnetic field rather than a dipole field where the wind is directed away from the equatorial plane and where a magnetospheric cavity forms. The influence of the magnetic wind in eroding and eventually destroying the accretion disk is analyzed. A momentum integral is derived for the turbulent wind/disk boundary layer and this is used to estimate the disk erosion time-scale as $\\sim 1-10^2$ Myr, with the lower value favored.

  1. Spectrum and light curve of a supernova shock breakout through a thick Wolf-Rayet wind

    SciTech Connect (OSTI)

    Svirski, Gilad; Nakar, Ehud

    2014-06-20

    Wolf-Rayet stars are known to eject winds. Thus, when a Wolf-Rayet star explodes as a supernova, a fast (? 40, 000 km s{sup –1}) shock is expected to be driven through a wind. We study the signal expected from a fast supernova shock propagating through an optically thick wind and find that the electrons behind the shock driven into the wind are efficiently cooled by inverse Compton over soft photons that were deposited by the radiation-mediated shock that crossed the star. Therefore, the bolometric luminosity is comparable to the kinetic energy flux through the shock, and the spectrum is found to be a power law, whose slope and frequency range depend on the number flux of soft photons available for cooling. Wolf-Rayet supernovae that explode through a thick wind have a high flux of soft photons, producing a flat spectrum, ?F {sub ?} = Const, in the X-ray range of 0.1 ? T ? 50 keV. As the shock expands into an optically thin wind, the soft photons are no longer able to cool the shock that plows through the wind, and the bulk of the emission takes the form of a standard core-collapse supernova (without a wind). However, a small fraction of the soft photons is upscattered by the shocked wind and produces a transient unique X-ray signature.

  2. Wind energy applications guide

    SciTech Connect (OSTI)

    anon.

    2001-01-01

    The brochure is an introduction to various wind power applications for locations with underdeveloped transmission systems, from remote water pumping to village electrification. It includes an introductory section on wind energy, including wind power basics and system components and then provides examples of applications, including water pumping, stand-alone systems for home and business, systems for community centers, schools, and health clinics, and examples in the industrial area. There is also a page of contacts, plus two specific example applications for a wind-diesel system for a remote station in Antarctica and one on wind-diesel village electrification in Russia.

  3. Thermal Wind The thermal wind is defined as the vector difference between the geostrophic winds at

    E-Print Network [OSTI]

    Hennon, Christopher C.

    ATMS 310 Thermal Wind The thermal wind is defined as the vector difference between the geostrophic winds at two levels. It is not really a wind at all, just a measure of the shear of the geostrophic wind. But there are good reasons for considering the geostrophic wind; mainly, it provides a convenient way of connecting

  4. Wind energy conversion system

    DOE Patents [OSTI]

    Longrigg, Paul (Golden, CO)

    1987-01-01

    The wind energy conversion system includes a wind machine having a propeller connected to a generator of electric power, the propeller rotating the generator in response to force of an incident wind. The generator converts the power of the wind to electric power for use by an electric load. Circuitry for varying the duty factor of the generator output power is connected between the generator and the load to thereby alter a loading of the generator and the propeller by the electric load. Wind speed is sensed electro-optically to provide data of wind speed upwind of the propeller, to thereby permit tip speed ratio circuitry to operate the power control circuitry and thereby optimize the tip speed ratio by varying the loading of the propeller. Accordingly, the efficiency of the wind energy conversion system is maximized.

  5. Wind tower service lift

    DOE Patents [OSTI]

    Oliphant, David; Quilter, Jared; Andersen, Todd; Conroy, Thomas

    2011-09-13

    An apparatus used for maintaining a wind tower structure wherein the wind tower structure may have a plurality of legs and may be configured to support a wind turbine above the ground in a better position to interface with winds. The lift structure may be configured for carrying objects and have a guide system and drive system for mechanically communicating with a primary cable, rail or other first elongate member attached to the wind tower structure. The drive system and guide system may transmit forces that move the lift relative to the cable and thereby relative to the wind tower structure. A control interface may be included for controlling the amount and direction of the power into the guide system and drive system thereby causing the guide system and drive system to move the lift relative to said first elongate member such that said lift moves relative to said wind tower structure.

  6. Magnetic field studies of massive main sequence stars

    E-Print Network [OSTI]

    Schoeller, M; Ilyin, I; Kharchenko, N V; Briquet, M; Langer, N; Oskinova, L M

    2011-01-01

    We report on the status of our spectropolarimetric observations of massive stars. During the last years, we have discovered magnetic fields in many objects of the upper main sequence, including Be stars, beta Cephei and Slowly Pulsating B stars, and a dozen O stars. Since the effects of those magnetic fields have been found to be substantial by recent models, we are looking into their impact on stellar rotation, pulsation, stellar winds, and chemical abundances. Accurate studies of the age, environment, and kinematic characteristics of the magnetic stars are also promising to give us new insight into the origin of the magnetic fields. Furthermore, longer time series of magnetic field measurements allow us to observe the temporal variability of the magnetic field and to deduce the stellar rotation period and the magnetic field geometry. Studies of the magnetic field in massive stars are indispensable to understand the conditions controlling the presence of those fields and their implications on the stellar phy...

  7. Shocks, Star Formation, and the JWST

    E-Print Network [OSTI]

    Gusdorf, Antoine

    2015-01-01

    The interstellar medium (ISM) is constantly evolving due to unremitting injection of energy in various forms. Energetic radiation transfers energy to the ISM: from the UV photons, emitted by the massive stars, to X- and $\\gamma$-ray ones. Cosmic rays are another source of energy. Finally, mechanical energy is injected through shocks or turbulence. Shocks are ubiquitous in the interstellar medium of galaxies. They are associated to star formation (through jets and bipolar outflows), life (via stellar winds), and death (in AGB stellar winds or supernovae explosion). The dynamical processes leading to the formation of molecular clouds also generate shocks where flows of interstellar matter collide. Because of their ubiquity, the study of interstellar shocks is also a useful probe to the other mechanisms of energy injection in the ISM. This study must be conducted in order to understand the evolution of the ISM as a whole, and to address various questions: what is the peculiar chemistry associated to shocks, and ...

  8. Superbubble Activity in Star-Forming Galaxies

    E-Print Network [OSTI]

    M. S. Oey

    2002-12-03

    Mechanical feedback from massive stars, primarily from supernovae, can dominate ISM structuring and phase balance, thereby profoundly affecting galactic evolutionary processes. Our understanding of mechanical feedback is based on the adiabatic, wind-driven bubble model, applied on size scales ranging over three decades. Tests of the model, and our consequent understanding of feedback, are reviewed. While the model is broadly successful, critical unknowns still prevent a comprehensive understanding of the consequences of feedback.

  9. The r-Process in Supersonic Neutrino-Driven Winds: The Roll of Wind Termination Shock

    E-Print Network [OSTI]

    Takami Kuroda; Shinya Wanajo; Ken'ichi Nomoto

    2007-09-17

    Recent hydrodynamic studies of core-collapse supernovae imply that the neutrino-heated ejecta from a nascent neutron star develops to supersonic outflows. These supersonic winds are influenced by the reverse shock from the preceding supernova ejecta, forming the wind termination shock. We investigate the effects of the termination shock in neutrino-driven winds and its roll on the r-process. Supersonic outflows are calculated with a semi-analytic neutrino-driven wind model. Subsequent termination-shocked, subsonic outflows are obtained by applying the Rankine-Hugoniot relations. We find a couple of effects that can be relevant for the r-process. First is the sudden slowdown of the temperature decrease by the wind termination. Second is the entropy jump by termination-shock heating, up to several 100NAk. Nucleosynthesis calculations in the obtained winds are performed to examine these effects on the r-process. We find that 1) the slowdown of the temperature decrease plays a decisive roll to determine the r-process abundance curves. This is due to the strong dependences of the nucleosynthetic path on the temperature during the r-process freezeout phase. Our results suggest that only the termination-shocked winds with relatively small shock radii (~500km) are relevant for the bulk of the solar r-process abundances (A~100-180). The heaviest part in the solar r-process curve (A~180-200), however, can be reproduced both in shocked and unshocked winds. These results may help to constrain the mass range of supernova progenitors relevant for the r-process. We find, on the other hand, 2) negligible roles of the entropy jump on the r-process. This is a consequence that the sizable entropy increase takes place only at a large shock radius (~10,000km) where the r-process has already ceased.

  10. Torque on an exoplanet from an anisotropic evaporative wind

    E-Print Network [OSTI]

    Teyssandier, Jean; Adams, Fred C; Quillen, Alice C

    2015-01-01

    Winds from short-period Earth and Neptune mass exoplanets, driven by high energy radiation from a young star, may evaporate a significant fraction of a planet's mass. If the momentum flux from the evaporative wind is not aligned with the planet/star axis, then it can exert a torque on the planet's orbit. Using steady-state one-dimensional evaporative wind models we estimate this torque using a lag angle that depends on the product of the speed of the planet's upper atmosphere and a flow timescale for the wind to reach its sonic radius. We also estimate the momentum flux from time-dependent one-dimensional hydrodynamical simulations. We find that only in a very narrow regime in planet radius, mass and stellar radiation flux is a wind capable of exerting a significant torque on the planet's orbit. Similar to the Yarkovsky effect, the wind causes the planet to drift outward if atmospheric circulation is prograde (super-rotating) and in the opposite direction if the circulation is retrograde. A close-in super Ear...

  11. AGN Jet Mass Loading and Truncation by Stellar Winds

    E-Print Network [OSTI]

    Alexander Hubbard; Eric G. Blackman

    2006-04-28

    Active Galactic Nuclei can produce extremely powerful jets. While tightly collimated, the scale of these jets and the stellar density at galactic centers implies that there will be many jet/star interactions, which can mass-load the jet through stellar winds. Previous work employed modest wind mass outflow rates, but this does not apply when mass loading is provided by a small number of high mass-loss stars. We construct a framework for jet mass-loading by stellar winds for a broader spectrum of wind mass-loss rates than has been previously considered. Given the observed stellar mass distributions in galactic centers, we find that even highly efficient (0.1 Eddington luminosity) jets from supermassive black holes of masses $M_{BH} \\la 10^4M_{\\odot}$ are rapidly mass loaded and quenched by stellar winds. For $10^4 M_{\\odot}jets is independent of the jet's mechanical luminosity. Stellar wind mass-loading is unable to quench efficient jets from more massive engines, but can account for the observed truncation of the inefficient M87 jet, and implies a baryon dominated composition on scales $\\ga 2$ kpc therein even if the jet is initially pair plasma dominated.

  12. Social networks for lonely objects

    E-Print Network [OSTI]

    Kestner, John Anthony

    2010-01-01

    Visions of ubiquitous computing describe a network of devices that quietly supports human goals, but this may also add complexity to an already frustrating relationship between humans and their electronic objects. As we ...

  13. Nucleosynthesis in barium stars

    E-Print Network [OSTI]

    Trimble, V; Trimble, V

    1984-01-01

    problem of apparent nucleosynthesis in barium stars, thoughSE24 9JF. Astronomy Nucleosynthesis in barium stars fromopportunity to see that nucleosynthesis really is taking

  14. Gansu Xinhui Wind Power | Open Energy Information

    Open Energy Info (EERE)

    Xinhui Wind Power Jump to: navigation, search Name: Gansu Xinhui Wind Power Place: China Sector: Wind energy Product: China-based joint venture engaged in developing wind projects....

  15. Wind Tunnel Building - 3 

    E-Print Network [OSTI]

    Unknown

    2005-06-30

    1 Energy Systems Laboratory 1 A METHODOLOGY FOR CALCULATING EMISSIONS REDUCTIONS FROM RENEWABLE ENERGY PROGRAMS AND ITS APPLICATION TO THE WIND FARMS IN THE TEXAS ERCOT REGION Zi Liu, Jeff Haberl, Juan-Carlos Baltazar, Kris Subbarao, Charles... on Sweetwater I Wind Farm Capacity Factor Analysis Application to All Wind Farms Uncertainty Analysis Emissions Reduction Summary Energy Systems Laboratory 3 SUMMARYEMISSIONS REDUCTION UNCERTAINTY ANALYSIS APPLICATIONMETHODOLOGYINTRODUCTION Background...

  16. When Stars Blow Up What Stars Explode?

    E-Print Network [OSTI]

    Walter, Frederick M.

    When Stars Blow Up #12;What Stars Explode? ·Cataclysmic variables ·Novae ·Supernovae #12;Cataclysmic Variables ·Binary star systems incorporating a white dwarf ·Outbursts due to disk instabilities the temperature reaches a few MK, fusion begins ·Degenerate fusion is a runaway. ·All the H fuses to He

  17. High-Speed Optical Spectroscopy of a Cataclysmic Variable Wind BZ Camelopardalis

    E-Print Network [OSTI]

    Ringwald, F A

    1997-01-01

    BZ Cam is the first cataclysmic variable star with an accretion disk wind evident in its optical spectrum. The wind was found by Thorstensen, who discovered intermittent P Cygni profiles occurring simultaneously in He I 5876 Angstroms and H alpha. We have since obtained spectra with 0.4-Angstroms/pixel dispersion and 60-s time resolution. We find a wind much faster and more rapidly variable than the radiatively accelerated winds of OB stars, Wolf-Rayet stars, or luminous blue variables. Instead of showing blob ejection, the whole wind of BZ Cam appears to turn on and off. We use this to measure the acceleration law of a CV wind for the first time. The velocity increases linearly with time, attaining blue edge velocities near -3000 km/s, and absorption velocities near -1700 km/s, in 6 to 8 min after starting near rest. We also find a subsequent linear deceleration to nearly rest in 30 to 40 min, perhaps an effect of dilution as the wind expands. No periodicity from rotational outflow is obvious. This wind is e...

  18. Proceedings Nordic Wind Power Conference

    E-Print Network [OSTI]

    Estimation of Possible Power for Wind Plant Control Power Fluctuations from Offshore Wind Farms; Model Validation System grounding of wind farm medium voltage cable grids Faults in the Collection Grid of Offshore systems of wind turbines and wind farms. NWPC presents the newest research results related to technical

  19. Wind Energy and Spatial Technology

    E-Print Network [OSTI]

    Schweik, Charles M.

    2/3/2011 1 Wind Energy and Spatial Technology Lori Pelech Why Wind Energy? A clean, renewable 2,600 tons of carbon emissions annually ­ The economy · Approximately 85,000 wind energy workers to Construct a Wind Farm... Geo-Spatial Components of Wind Farm Development Process Selecting a Project Site

  20. Module Handbook Specialisation Wind Energy

    E-Print Network [OSTI]

    Habel, Annegret

    Module Handbook Specialisation Wind Energy 2nd Semester for the Master Programme REMA/EUREC Course 2008/2009 NTU Athens Specialisation Provider: Wind Energy #12;Specialisation Wind Energy, NTU Athens, 2nd Semester Module 1/Wind Energy: Wind potential, Aerodynamics & Loading

  1. Wind Engineering & Natural Disaster Mitigation

    E-Print Network [OSTI]

    Lennard, William N.

    Wind Engineering & Natural Disaster Mitigation For more than 45 years, Western University has been internationally recognized as the leading university for wind engineering and wind- related research. Its of environmental disaster mitigation, with specific strengths in wind and earthquake research. Boundary Layer Wind

  2. Accelerating Offshore Wind Development

    Broader source: Energy.gov [DOE]

    Today the Energy Department announced investments in seven offshore wind demonstration projects. Check out our map to see where these projects will be located.

  3. Wind/Water Nexus

    SciTech Connect (OSTI)

    Not Available

    2006-04-01

    Nobel laureate Richard Smalley cited energy and water as among humanity's top problems for the next 50 years as the world's population increases from 6.3 billion to 9 billion. The U.S. Department of Energy's Wind and Hydropower Program has initiated an effort to explore wind energy's role as a technical solution to this critically important issue in the United States and the world. This four-page fact sheet outlines five areas in which wind energy can contribute: thermoelectric power plant/water processes, irrigation, municipal water supply, desalination, and wind/hydropower integration.

  4. Vertical axis wind turbines

    DOE Patents [OSTI]

    Krivcov, Vladimir (Miass, RU); Krivospitski, Vladimir (Miass, RU); Maksimov, Vasili (Miass, RU); Halstead, Richard (Rohnert Park, CA); Grahov, Jurij (Miass, RU)

    2011-03-08

    A vertical axis wind turbine is described. The wind turbine can include a top ring, a middle ring and a lower ring, wherein a plurality of vertical airfoils are disposed between the rings. For example, three vertical airfoils can be attached between the upper ring and the middle ring. In addition, three more vertical airfoils can be attached between the lower ring and the middle ring. When wind contacts the vertically arranged airfoils the rings begin to spin. By connecting the rings to a center pole which spins an alternator, electricity can be generated from wind.

  5. Talkin’ Bout Wind Generation

    Office of Energy Efficiency and Renewable Energy (EERE)

    The amount of electricity generated by the wind industry started to grow back around 1999, and since 2007 has been increasing at a rapid pace.

  6. Millimeter Continuum Observations of Stars Roberto Pallavicini 1 and Stephen M. White 2

    E-Print Network [OSTI]

    topics including millimeter observations of the Sun, winds of hot stars, circumstel­ lar disks of pre chromosphere of the Sun and stars; they have an advantage over UV and optical observations in that they measure wavelengths is produced by much higher energy electrons than are typically rel­ evant at microwave frequencies

  7. The Lunar L1 Gateway: Portal to the Stars and Beyond

    E-Print Network [OSTI]

    Ross, Shane

    1 The Lunar L1 Gateway: Portal to the Stars and Beyond Martin W. Lo Navigation and Mission Design-30, 2001 #12;2 The Lunar L1 Gateway: Portal to the Stars and Beyond Martin Lo1 , Shane Ross2 Abstract Our Solar System is interconnected by a vast system of tunnels winding around the Sun generated

  8. DOE Offers Conditional Commitment to Cape Wind Offshore Wind...

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

    step toward issuing a 150 million loan guarantee to support the construction of the Cape Wind offshore wind project with a conditional commitment to Cape Wind Associates, LLC. The...

  9. Wind Power Today, 2010, Wind and Water Power Program (WWPP)

    SciTech Connect (OSTI)

    Not Available

    2010-05-01

    Wind Power Today is an annual publication that provides an overview of the wind energy research conducted by the U.S. Department of Energy Wind and Water Power Program.

  10. Wind Powering America's Wind for Schools Team Honored with Wirth...

    Office of Environmental Management (EM)

    Powering America's Wind for Schools Team Honored with Wirth Chair Award Wind Powering America's Wind for Schools Team Honored with Wirth Chair Award May 1, 2012 - 2:46pm Addthis...

  11. Theoretical X-ray Line Profiles from Colliding Wind Binaries

    E-Print Network [OSTI]

    Henley, D B; Pittard, J M

    2003-01-01

    We present theoretical X-ray line profiles from a range of model colliding wind systems. In particular, we investigate the effects of varying the stellar mass-loss rates, the wind speeds, and the viewing orientation. We find that a wide range of theoretical line profile shapes is possible, varying with orbital inclination and phase. At or near conjunction, the lines have approximately Gaussian profiles, with small widths (HWHM ~ 0.1 v_infty) and definite blue- or redshifts (depending on whether the star with the weaker wind is in front or behind). When the system is viewed at quadrature, the lines are generally much broader (HWHM ~ v_infty), flat-topped and unshifted. Local absorption can have a major effect on the observed profiles - in systems with mass-loss rates of a few times 10^{-6} Msol/yr the lower energy lines (E wind of the primary. The orbital variation ...

  12. The modelling of feedback in star formation simulations

    E-Print Network [OSTI]

    Dale, James E

    2015-01-01

    I review the current state of numerical simulations of stellar feedback in the context of star formation at scales ranging from the formation of individual stars to models of galaxy formation including cosmic reionisation. I survey the wealth of algorithms developed recently to solve the radiative transfer problem and to simulate stellar winds, supernovae and protostellar jets. I discuss the results of these simulations with regard to star formation in molecular clouds, the interaction of different feedback mechanisms with each other and with magnetic fields, and in the wider context of galactic-- and cosmological--scale simulations.

  13. Community Wind Handbook/Understand Your Wind Resource and Conduct...

    Open Energy Info (EERE)

    Help Apps Datasets Community Login | Sign Up Search Page Edit History Community Wind HandbookUnderstand Your Wind Resource and Conduct a Preliminary Estimate < Community...

  14. American Wind Energy Association Wind Energy Finance and Investment Seminar

    Office of Energy Efficiency and Renewable Energy (EERE)

    The American Wind Energy Association Wind Energy Finance and Investment Seminar will be attended by representatives in the financial sector, businesses, bankers, government and other nonprofit...

  15. Public Acceptance of Wind: Foundational Study Near US Wind Facilities

    Wind Powering America (EERE)

    Group * Energy Analysis and Environmental Impacts Department Public Acceptance of Wind Power Ben Hoen Lawrence Berkeley National Laboratory WindExchange Webinar June 17, 2015...

  16. 20% Wind Energy by 2030: Increasing Wind Energy's Contribution...

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

    Supply (Executive Summary) 20% Wind Energy by 2030: Increasing Wind Energy's Contribution to U.S. Electricity Supply (Executive Summary) Executive summary of a report on the...

  17. Broken Bow Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin:PontiacInformation ForestBroadStar Wind Systemsand

  18. Brown County Wind | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoop IncIowaWisconsin:PontiacInformation ForestBroadStarBrophy OccurrenceWind Jump

  19. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    al. 2010. Large-scale Offshore Wind for the United States:examined land-based and offshore wind energy in the Easternassistance with the offshore wind energy discussion; Donna

  20. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    with the section on offshore wind; Donna Heimiller and Billythe end of 2011, global offshore wind power capacity stoodEnergy's investments in offshore wind R&D. Interest exists

  1. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    al. 2010. Large-scale Offshore Wind for the United States:assistance with the offshore wind energy discussion; DonnaTechnologies Market Report Offshore Wind Power Project and

  2. Wind Farms in North America

    E-Print Network [OSTI]

    Hoen, Ben

    2014-01-01

    Economic Analysis of a Wind Farm in Nantucket Sound. BeaconP. and Mueller, A. (2010) Wind Farm Announcements and RuralProposed Rail Splitter Wind Farm. Prepared for Hinshaw &

  3. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    Public Service Wind Integration Cost Impact Study. Preparedused to estimate wind integration costs and the ability toColorado 2 GW and 3 GW Wind Integration Cost Study. Denver,

  4. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    from Canada and Mexico; unlike for wind-powered generatingHonduras (16%), Mexico (8%), and Canada (8%). Wind turbineWind belt states include Colorado, Iowa, Kansas, Minnesota, Missouri, Montana, Nebraska, New Mexico,

  5. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    balancing areas, the use of wind forecasts, and intra-hourchallenges and costs. Wind forecasts are most accurate andare the cost of day-ahead wind forecast error; the remaining

  6. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    of wind power capacity in that state) because generatorsgenerators to provide the needed flexibility to integrate wind power.wind power forecasts by system operators can significantly reduce integration challenges and costs. Intra-hour transmission scheduling and generator

  7. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    AWEA). 2010b. AWEA Small Wind Turbine Global Market Survey,html David, A. 2009. Wind Turbines: Industry and Tradewhich new large-scale wind turbines were installed in 2009 (

  8. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    AWEA’s Wind Energy Weekly, DOE/EPRI’s Turbine Verification10% Wind Energy Penetration New large-scale 10 wind turbineswind energy became more challenging, orders for new turbines

  9. Fort Carson Wind Resource Assessment

    SciTech Connect (OSTI)

    Robichaud, R.

    2012-10-01

    This report focuses on the wind resource assessment, the estimated energy production of wind turbines, and economic potential of a wind turbine project on a ridge in the southeastern portion of the Fort Carson Army base.

  10. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    AWEA). 2010b. AWEA Small Wind Turbine Global Market Survey,a brief discussion on Small Wind Turbines is provided on2010a) sometimes also includes small wind turbines. Other

  11. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    Associates. 2010. SPP WITF Wind Integration Study. LittlePool. David, A. 2011. U.S. Wind Turbine Trade in a Changing2011. David, A. 2010. Impact of Wind Energy Installations on

  12. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    ET2/TL-08-1474. May 19, 2010 Wind Technologies Market ReportAssociates. 2010. SPP WITF Wind Integration Study. Little10, 2010. David, A. 2009. Wind Turbines: Industry and Trade

  13. NREL: Wind Research - Offshore Wind Resource Characterization

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of Marine andDrivetrainsNew WindDesign ToolsWind

  14. Diablo Winds Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIX ECoopButtePower VenturesInformation9)ask queries TypeDeveloper|Winds Wind Farm Jump

  15. NREL: Wind Research - Wind Resource Assessment

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home Room NewsInformationJessework usesofPublications The NREL wind research programWebmaster PleaseWind

  16. Wind Program Accomplishments

    SciTech Connect (OSTI)

    Wind Program

    2012-05-24

    This fact sheet describes some of the accomplishments of DOE's Wind Program through its investments in technology development and market barrier reduction, and how those accomplishments are supporting the advancement of renewable energy generated using the United States' abundant wind resources.

  17. Small Wind Information (Postcard)

    SciTech Connect (OSTI)

    Not Available

    2011-08-01

    The U.S. Department of Energy's Wind Powering America initiative maintains a website section devoted to information about small wind turbines for homeowners, ranchers, and small businesses. This postcard is a marketing piece that stakeholders can provide to interested parties; it will guide them to this online resource.

  18. Carbon smackdown: wind warriors

    ScienceCinema (OSTI)

    Glen Dahlbacka of the Accelerator & Fusion Research Division and Ryan Wiser of the Environmental Energy Technologies Division are the speakers.

    2010-09-01

    July 16. 2010 carbon smackdown summer lecture: learn how Berkeley Lab scientists are developing wind turbines to be used in an urban setting, as well as analyzing what it will take to increase the adoption of wind energy in the U.S.

  19. Illinois Wind Workers Group

    SciTech Connect (OSTI)

    David G. Loomis

    2012-05-28

    The Illinois Wind Working Group (IWWG) was founded in 2006 with about 15 members. It has grown to over 200 members today representing all aspects of the wind industry across the State of Illinois. In 2008, the IWWG developed a strategic plan to give direction to the group and its activities. The strategic plan identifies ways to address critical market barriers to the further penetration of wind. The key to addressing these market barriers is public education and outreach. Since Illinois has a restructured electricity market, utilities no longer have a strong control over the addition of new capacity within the state. Instead, market acceptance depends on willing landowners to lease land and willing county officials to site wind farms. Many times these groups are uninformed about the benefits of wind energy and unfamiliar with the process. Therefore, many of the project objectives focus on conferences, forum, databases and research that will allow these stakeholders to make well-educated decisions.

  20. NREL SBV Pilot Wind Technologies

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

    capabilities to develop everything at one location-from small residential wind turbines and components to utility-scale offshore wind technologies. With the NWTC, partners...

  1. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    wind power curtailment and the evolution in turbine design,power and wind resource quality confirms this offsetting effect and shows that turbine design

  2. Maryland Offshore Wind Annual Meeting

    Broader source: Energy.gov [DOE]

    This event will provide updates on regional offshore wind projects and will help attendees understand Maryland's offshore wind project and the team members required. Participants will also learn...

  3. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    Policy Landscape Is Now More Favorable to Wind Energy thanPolicy Landscape Is Now More Favorable to Wind Energy than

  4. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    regulation and frequency response services charge for wind energyRegulation and Frequency Response Service that charges a higher rate for wind energy

  5. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    electricity demand growth; existing state policies that are insufficient to support future wind power capacity additions at the levels 2011 Wind Technologies Market

  6. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    Lab staff. Wind Project Operations and Maintenance CostsWind project operations and maintenance costs come primarilyEnergy Laboratory operations and maintenance publicly owned

  7. Interaction of Infall and Winds in Young Stellar Objects

    E-Print Network [OSTI]

    G. Delamarter; A. Frank; L. Hartmann

    1999-10-14

    The interaction of a stellar or disk wind with a collapsing environment holds promise for explaining a variety of outflow phenomena observed around young stars. In this paper we present the first simulations of these interactions. The focus here is on exploring how ram pressure balance between wind and ambient gas and post-shock cooling affects the shape of the resulting outflows. In our models we explore the role of ram pressure and cooling by holding the wind speed constant and adjusting the ratio of the inflow mass flux to the wind mass flux (Mdot_a/Mdot_w) Assuming non-spherical cloud collapse, we find that relatively strong winds can carve out wide, conical outflow cavities and that relatively weak winds can be strongly collimated into jet-like structures. If the winds become weak enough, they can be cut off entirely by the infalling environment. We identify discrepancies between results from standard snowplow models and those presented here that have important implications for molecular outflows. We also present mass vs. velocity curves for comparison with observations.

  8. The Colliding Winds of WR146: Seeing the Works

    E-Print Network [OSTI]

    E. P. O'Connor; S. M. Dougherty; J. M. Pittard; P. M. Williams

    2005-09-08

    WR146 is a WC6+O8 colliding-wind binary (CWB) system with thermal emission from the stellar winds of the two stars, and bright non-thermal emission from the wind-collision region (WCR) where the winds collide. We present high resolution radio observations from 1.4 to 43 GHz that give one of the best quality radio spectra of any CWB to date. Observations at 22 GHz now span 8 years, and reveal the proper motion of the system, allowing comparison of multi-epoch data. VLBI observations show the location of the WCR relative to the stellar components, from which the wind momentum ratio can be shown to be 0.06+/-0.15. The radio spectrum and the spatial distribution of emission are modelled, and we determine the contribution of both stellar winds and the WCR to the observed emission. We show that our current models fail to account for the high frequency spectrum of WR146, and also produce too much emission far from the stagnation point of the wind collision.

  9. Wind Fins: Novel Lower-Cost Wind Power System

    SciTech Connect (OSTI)

    David C. Morris; Dr. Will D. Swearingen

    2007-10-08

    This project evaluated the technical feasibility of converting energy from the wind with a novel “wind fin” approach. This patent-pending technology has three major components: (1) a mast, (2) a vertical, hinged wind structure or fin, and (3) a power takeoff system. The wing structure responds to the wind with an oscillating motion, generating power. The overall project goal was to determine the basic technical feasibility of the wind fin technology. Specific objectives were the following: (1) to determine the wind energy-conversion performance of the wind fin and the degree to which its performance could be enhanced through basic design improvements; (2) to determine how best to design the wind fin system to survive extreme winds; (3) to determine the cost-effectiveness of the best wind fin designs compared to state-of-the-art wind turbines; and (4) to develop conclusions about the overall technical feasibility of the wind fin system. Project work involved extensive computer modeling, wind-tunnel testing with small models, and testing of bench-scale models in a wind tunnel and outdoors in the wind. This project determined that the wind fin approach is technically feasible and likely to be commercially viable. Project results suggest that this new technology has the potential to harvest wind energy at approximately half the system cost of wind turbines in the 10kW range. Overall, the project demonstrated that the wind fin technology has the potential to increase the economic viability of small wind-power generation. In addition, it has the potential to eliminate lethality to birds and bats, overcome public objections to the aesthetics of wind-power machines, and significantly expand wind-power’s contribution to the national energy supply.

  10. Signature of wide-spread clumping in B supergiant winds

    E-Print Network [OSTI]

    Prinja, Raman

    2010-01-01

    We seek to establish additional observational signatures of the effects of clumping in OB star winds. The action of clumping on strategic wind-formed spectral lines is tested to steer the development of models for clumped winds and thus improve the reliability of mass-loss determinations for massive stars.The SiIV 1400 resonance line doublets of B0 to B5 supergiants are analysed using empirical line-synthesis models. The focus is on decoding information on wind clumping from measurements of ratios of the radial optical depths (tau_(rad)(w)) of the red and blue components of the SiIV doublet. We exploit in particular the fact that the two doublet components are decoupled and formed independently for targets with relatively low wind terminal velocities. Line-synthesis analyses reveal that the mean ratio of tau_(rad)(w) of the blue to red SiIV components are rarely close to the canonical value of ~ 2 (expected from atomic constants), and spread instead over a range of values between ~1 and 2. These results are i...

  11. Gone with the Wind - The Potential Tragedy of the Common Wind

    E-Print Network [OSTI]

    Lifshitz-Goldberg, Yaei

    2010-01-01

    As a result wind turbines can produce energy in winds as lowelectric energy to generate wind, a wind turbine utilizesWind Turbine Projects to Encourage Utilization of Wind Energy

  12. Quantifying Offshore Wind Resources from Satellite Wind Maps

    E-Print Network [OSTI]

    Pryor, Sara C.

    the spatial extent of the wake behind large offshore wind farms. Copyright © 2006 John Wiley & Sons, LtdQuantifying Offshore Wind Resources from Satellite Wind Maps: Study Area the North Sea C. B National Laboratory, Roskilde, Denmark Offshore wind resources are quantified from satellite synthetic

  13. Reference wind farm selection for regional wind power prediction models

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    1 Reference wind farm selection for regional wind power prediction models Nils Siebert George.siebert@ensmp.fr, georges.kariniotakis@ensmp.fr Abstract Short-term wind power forecasting is recognized today as a major requirement for a secure and economic integration of wind generation in power systems. This paper deals

  14. Wind Energy at NREL's National Wind Technology Center

    ScienceCinema (OSTI)

    None

    2013-05-29

    It is a pure, plentiful natural resource. Right now wind is in high demand and it holds the potential to transform the way we power our homes and businesses. NREL is at the forefront of wind energy research and development. NREL's National Wind Technology Center (NWTC) is a world-class facility dedicated to accelerating and deploying wind technology.

  15. Wind Energy at NREL's National Wind Technology Center

    SciTech Connect (OSTI)

    None

    2010-01-01

    It is a pure, plentiful natural resource. Right now wind is in high demand and it holds the potential to transform the way we power our homes and businesses. NREL is at the forefront of wind energy research and development. NREL's National Wind Technology Center (NWTC) is a world-class facility dedicated to accelerating and deploying wind technology.

  16. Small Wind Electric Systems Small Wind Electric Systems

    E-Print Network [OSTI]

    Branoff, Theodore J.

    An Illinois Consumer's Guide Small Wind Electric Systems #12;Small Wind Electric Systems Cover photo: Small wind turbines, like this grid-connected 10-kilowatt Bergey, can provide supplemental power -- Warren Gretz, NREL/PIX09630 #12;Small Wind Electric Systems Contents Introduction

  17. Wind | Department of Energy

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE: Alternative Fuels DataEnergy Webinar: Demonstration of NREL'sWind Wind Wind The United States

  18. WP2 IEA Wind Task 26:The Past and Future Cost of Wind Energy

    E-Print Network [OSTI]

    Lantz, Eric

    2014-01-01

    Carbon Trust. (2008). Offshore Wind Power: Big Challenge,Financial Support for Offshore Wind. The UK Department ofCost Reduction Prospects for Offshore Wind Farms. ” Wind

  19. WP2 IEA Wind Task 26:The Past and Future Cost of Wind Energy

    E-Print Network [OSTI]

    Lantz, Eric

    2014-01-01

    Looking forward, offshore wind costs are generally expectedachieving the U.S. 20% wind cost and performance trajectoryDissecting Wind Turbine Costs. ” WindStats Newsletter (21:

  20. WP2 IEA Wind Task 26:The Past and Future Cost of Wind Energy

    E-Print Network [OSTI]

    Lantz, Eric

    2014-01-01

    Carbon Trust. (2008). Offshore Wind Power: Big Challenge,and Financial Support for Offshore Wind. The UK DepartmentCost Reduction Prospects for Offshore Wind Farms. ” Wind

  1. Wind Program Announces $2 Million to Develop and Field Test Wind...

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

    Wind Program Announces 2 Million to Develop and Field Test Wind Energy Bat Impact Minimization Technologies Wind Program Announces 2 Million to Develop and Field Test Wind Energy...

  2. WP2 IEA Wind Task 26:The Past and Future Cost of Wind Energy

    E-Print Network [OSTI]

    Lantz, Eric

    2014-01-01

    Opportunities in Wind Energy Technology. ” 50th AIAA/ASME/in its European Wind Energy Technology Platform (TP Wind) tothe Chapter on Wind Power in Energy Technology Perspectives

  3. Star-ND (Multi-Dimensional Star-Identification) 

    E-Print Network [OSTI]

    Spratling, Benjamin

    2012-07-16

    of iterations of the run-time algorithm. The associated algorithms, star pattern parameters, and database preparation are collectively referred to as Multi-dimensional Star-Identification (Star-ND). The star pattern parameters developed may also be extended...

  4. Kentish Flats Offshore Wind Farm

    E-Print Network [OSTI]

    Firestone, Jeremy

    Kentish Flats Offshore Wind Farm #12;By August 2005 the offshore wind farm at Kentish Flats plateau just outside the main Thames shipping lanes. The Kentish Flats wind farm will comprise 30 of the wind farm could be up to 90 MW. For the benefit of the environment The British Government has set

  5. wind engineering & natural disaster mitigation

    E-Print Network [OSTI]

    Denham, Graham

    wind engineering & natural disaster mitigation #12;wind engineering & natural disaster mitigation Investment WindEEE Dome at Advanced Manufacturing Park $31million Insurance Research Lab for Better Homes $8million Advanced Facility for Avian Research $9million #12;wind engineering & natural disaster mitigation

  6. Kentish Flats Offshore Wind Farm

    E-Print Network [OSTI]

    Firestone, Jeremy

    Kentish Flats Offshore Wind Farm #12;By August 2005 the offshore wind farm at Kentish Flats and offshore wind energy will contribute sig- nificantly to achieving this target. The Kentish Flats alone plateau just outside the main Thames shipping lanes. The Kentish Flats wind farm will comprise 30

  7. Wind Electrolysis: Hydrogen Cost Optimization

    SciTech Connect (OSTI)

    Saur, G.; Ramsden, T.

    2011-05-01

    This report describes a hydrogen production cost analysis of a collection of optimized central wind based water electrolysis production facilities. The basic modeled wind electrolysis facility includes a number of low temperature electrolyzers and a co-located wind farm encompassing a number of 3MW wind turbines that provide electricity for the electrolyzer units.

  8. 2010 Wind Technologies Market Report

    SciTech Connect (OSTI)

    Wiser, Ryan; Bolinger, Mark

    2011-06-01

    This report provides a comprehensive overview of trends in the U.S. wind power market in 2010. The report analyzes trends in wind power capacity, industry, manufacturing, turbines, installed project costs, project performance, and wind power prices. It also describes trends among wind power developers, project owners, and power purchasers, and discusses financing issues.

  9. Optimization of Wind Turbine Operation

    E-Print Network [OSTI]

    Optimization of Wind Turbine Operation by Use of Spinner Anemometer TF Pedersen, NN Sørensen, L Title: Optimization of Wind Turbine Operation by Use of Spinner Anemometer Department: Wind Energy prototype wind turbine. Statistics of the yaw error showed an average of about 10°. The average flow

  10. Community Wind Benefits (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2012-11-01

    This fact sheet explores the benefits of community wind projects, including citations to published research.

  11. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    wind energy generation within the Electric Reliabilitywind energy generation within the Electric Reliability

  12. The Political Economy of Wind Power in China

    E-Print Network [OSTI]

    Swanson, Ryan Landon

    2011-01-01

    wind manufacturers to produce offshore wind turbines withturbines, including those suitable for offshore wind farms.

  13. DOE Collegiate Wind Competition

    Broader source: Energy.gov [DOE]

    The U.S. Department of Energy (DOE) Collegiate Wind Competition will take place concurrently with the 2014 AWEA WINDPOWER Conference and Exhibition in Las Vegas. Spectators are encouraged to attend...

  14. GSA Wind Supply Opportunity

    Energy Savers [EERE]

    values at the source and sink are added (or subtracted) to the base price. Walnut Ridge Wind Farm Production PJM Grid Energy PJM RECs Transaction Manager National RECs To GSA...

  15. Wind Turbines Benefit Crops

    ScienceCinema (OSTI)

    Takle, Gene

    2013-03-01

    Ames Laboratory associate scientist Gene Takle talks about research into the effect of wind turbines on nearby crops. Preliminary results show the turbines may have a positive effect by cooling and drying the crops and assisting with carbon dioxide uptake.

  16. Wind Turbines Benefit Crops

    SciTech Connect (OSTI)

    Takle, Gene

    2010-01-01

    Ames Laboratory associate scientist Gene Takle talks about research into the effect of wind turbines on nearby crops. Preliminary results show the turbines may have a positive effect by cooling and drying the crops and assisting with carbon dioxide uptake.

  17. County Wind Ordinance Standards

    Broader source: Energy.gov [DOE]

    Assembly Bill 45 of 2009 authorized counties to adopt ordinances to provide for the installation of small wind systems (50 kW or smaller) outside urbanized areas but within the county's...

  18. Wind Tunnel Building - 1 

    E-Print Network [OSTI]

    Unknown

    2005-06-30

    This paper describes a simple graphic tool that enables a building designer to evaluate the potential for wind induced ventilation cooling in several climate zones. Long term weather data were analyzed to determine the conditions for which available...

  19. Airborne Wind Turbine

    SciTech Connect (OSTI)

    2010-09-01

    Broad Funding Opportunity Announcement Project: Makani Power is developing an Airborne Wind Turbine (AWT) that eliminates 90% of the mass of a conventional wind turbine and accesses a stronger, more consistent wind at altitudes of near 1,000 feet. At these altitudes, 85% of the country can offer viable wind resources compared to only 15% accessible with current technology. Additionally, the Makani Power wing can be economically deployed in deep offshore waters, opening up a resource which is 4 times greater than the entire U.S. electrical generation capacity. Makani Power has demonstrated the core technology, including autonomous launch, land, and power generation with an 8 meter wingspan, 20 kW prototype. At commercial scale, Makani Power aims to develop a 600 kW, 28 meter wingspan product capable of delivering energy at an unsubsidized cost competitive with coal, the current benchmark for low-cost power.

  20. Wind Plant Ramping Behavior

    SciTech Connect (OSTI)

    Ela, E.; Kemper, J.

    2009-12-01

    With the increasing wind penetrations, utilities and operators (ISOs) are quickly trying to understand the impacts on system operations and planning. This report focuses on ramping imapcts within the Xcel service region.

  1. FTL Small Wind Tunnel 

    E-Print Network [OSTI]

    Unknown

    2011-08-17

    This research study developed basic dynamic models that can be used to accurately predict the response behavior of a near-shore wind turbine structure with monopile, suction caisson, or gravity-based foundation systems. The marine soil conditions...

  2. NREL: Wind Research - Wind Career Map Shows Wind Industry Career

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of MarineOpportunities, Paths Wind Career

  3. Tornado type wind turbines

    DOE Patents [OSTI]

    Hsu, Cheng-Ting (Ames, IA)

    1984-01-01

    A tornado type wind turbine has a vertically disposed wind collecting tower with spaced apart inner and outer walls and a central bore. The upper end of the tower is open while the lower end of the structure is in communication with a wind intake chamber. An opening in the wind chamber is positioned over a turbine which is in driving communication with an electrical generator. An opening between the inner and outer walls at the lower end of the tower permits radially flowing air to enter the space between the inner and outer walls while a vertically disposed opening in the wind collecting tower permits tangentially flowing air to enter the central bore. A porous portion of the inner wall permits the radially flowing air to interact with the tangentially flowing air so as to create an intensified vortex flow which exits out of the top opening of the tower so as to create a low pressure core and thus draw air through the opening of the wind intake chamber so as to drive the turbine.

  4. Winding for linear pump

    DOE Patents [OSTI]

    Kliman, G.B.; Brynsvold, G.V.; Jahns, T.M.

    1989-08-22

    A winding and method of winding for a submersible linear pump for pumping liquid sodium are disclosed. The pump includes a stator having a central cylindrical duct preferably vertically aligned. The central vertical duct is surrounded by a system of coils in slots. These slots are interleaved with magnetic flux conducting elements, these magnetic flux conducting elements forming a continuous magnetic field conduction path along the stator. The central duct has placed therein a cylindrical magnetic conducting core, this core having a cylindrical diameter less than the diameter of the cylindrical duct. The core once placed to the duct defines a cylindrical interstitial pumping volume of the pump. This cylindrical interstitial pumping volume preferably defines an inlet at the bottom of the pump, and an outlet at the top of the pump. Pump operation occurs by static windings in the outer stator sequentially conveying toroidal fields from the pump inlet at the bottom of the pump to the pump outlet at the top of the pump. The winding apparatus and method of winding disclosed uses multiple slots per pole per phase with parallel winding legs on each phase equal to or less than the number of slots per pole per phase. The slot sequence per pole per phase is chosen to equalize the variations in flux density of the pump sodium as it passes into the pump at the pump inlet with little or no flux and acquires magnetic flux in passage through the pump to the pump outlet. 4 figs.

  5. Independent Signs of Lower Mass-Loss Rates for O-Type Stars

    E-Print Network [OSTI]

    Nathan Smith

    2007-10-18

    I discuss observational evidence -- independent of the direct spectral diagnostics of stellar winds themselves -- suggesting that mass-loss rates for O stars need to be revised downward by roughly a factor of three or more, in line with recent observed mass-loss rates for clumped winds. These independent constraints include the large observed mass-loss rates in LBV eruptions, the large masses of evolved massive stars like LBVs and WNH stars, WR stars in lower metallicity environments, observed rotation rates of massive stars at different metallicity, supernovae that seem to defy expectations of high mass-loss rates in stellar evolution, and other clues. I pay particular attention to the role of feedback that would result from higher mass-loss rates, driving the star to the Eddington limit too particular attention to the role of feedback that would result from higher mass-loss rates, driving the star to the Eddington limit too soon, and therefore making higher rates appear highly implausible. Some of these arguments by themselves may have more than one interpretation, but together they paint a consistent picture that steady line-driven winds of O-type stars have lower mass-loss rates and are significantly clumped.

  6. Small Wind Site Assessment Guidelines

    SciTech Connect (OSTI)

    Olsen, Tim; Preus, Robert

    2015-09-01

    Site assessment for small wind energy systems is one of the key factors in the successful installation, operation, and performance of a small wind turbine. A proper site assessment is a difficult process that includes wind resource assessment and the evaluation of site characteristics. These guidelines address many of the relevant parts of a site assessment with an emphasis on wind resource assessment, using methods other than on-site data collection and creating a small wind site assessment report.

  7. Footprints in the wind of Vela X-1 traced with MAXI

    E-Print Network [OSTI]

    Doroshenko, V; Nakahira, S; Mihara, T; Sugizaki, M; Matsuoka, M; Nakajima, M; Makishima, K

    2013-01-01

    The stellar wind around the compact object in luminous wind-accreting high mass X-ray binaries is expected to be strongly ionized with the X-rays coming from the compact object. The stellar wind of hot stars is mostly driven by light absorption in lines of heavier elements, and X-ray photo-ionization significantly reduces the radiative force within the so-called Stroemgren region leading to wind stagnation around the compact object. In close binaries like Vela X-1 this effect might alter the wind structure throughout the system. Using the spectral data from Monitor of All-sky X-ray Image (MAXI), we study the observed dependence of the photoelectric absorption as function of orbital phase in Vela X-1, and find that it is inconsistent with expectations for a spherically-symmetric smooth wind. Taking into account previous investigations we develop a simple model for wind structure with a stream-like photoionization wake region of slower and denser wind trailing the neutron star responsible for the observed absor...

  8. X-RAY EMISSION FROM MAGNETIC MASSIVE STARS

    SciTech Connect (OSTI)

    Nazé, Yaël; Petit, Véronique; 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.

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

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsourceII JumpQuarterly SmartDB-2, BluePoulsen Hybrid, LLCBiofuelsEthanol LLC Jump

  10. Light curves from supernova shock breakout through an extended wind

    SciTech Connect (OSTI)

    Ginzburg, Sivan; Balberg, Shmuel [Racah Institute of Physics, The Hebrew University, Jerusalem 91904 (Israel)

    2014-01-01

    Recent observations suggest that some supernovae may be the result of an explosion into an optically thick circumstellar material, the product of pre-explosion mass loss (wind) by the progenitor star. This scenario has been studied previously both analytically and numerically. However, many previous studies base their analysis on the diffusion approximation for radiation transfer, which is inappropriate in the optically thin outer layers of the wind. Here we study the deviations from diffusion and calculate light curves more accurately using a Monte Carlo approach to photon transfer. We distinguish between 'compact' winds, for which the diffusion approximation is appropriate, and 'extended' winds, which require a more delicate treatment of the radiation. We show that this effect is more significant than that of the light-travel time difference to a distant observer, which has a secondary influence on the light curves of extended-wind systems. We also comment on the applicability of the widely used flux-limited diffusion approximation in this context: we find that it generally does not reproduce the Monte Carlo results. The flux-limited diffusion approximation leads to results that are not only quantitatively but also qualitatively wrong in the extended-wind regime.

  11. Chemical evolution of galaxies with radiation-driven dust wind

    E-Print Network [OSTI]

    Bekki, Kenji

    2014-01-01

    We discuss how the removal of interstellar dust by radiation pressure of stars influences the chemical evolution of galaxies by using a new one-zone chemical evolution models with dust wind. The removal efficiency of an element (e.g., Fe, Mg, and Ca) through radiation-driven dust wind in a galaxy is assumed to depend both on the dust depletion level of the element in interstellar medium and the total luminosity of the galaxy in the new model. We particularly focus on the time evolution of [alpha/Fe] and its dependence on model parameters for dust wind in this study. The principal results are as follows. The time evolution of [Ca/Fe] is significantly different between models with and without dust wind in the sense that [Ca/Fe] can be systematically lower in the models with dust wind. The time evolution of [Mg/Fe], on the other hand, can not be so different between the models with and without dust wind owing to the lower level of dust depletion for Mg. As a result of this, [Mg/Ca] can be systematically higher i...

  12. Wind energy: Program overview, FY 1992

    SciTech Connect (OSTI)

    Not Available

    1993-06-01

    The DOE Wind Energy Program assists utilities and industry in developing advanced wind turbine technology to be economically competitive as an energy source in the marketplace and in developing new markets and applications for wind systems. This program overview describes the commercial development of wind power, wind turbine development, utility programs, industry programs, wind resources, applied research in wind energy, and the program structure.

  13. Wind Powering America Podcasts, Wind Powering America (WPA)

    SciTech Connect (OSTI)

    Not Available

    2012-04-01

    Wind Powering America and the National Association of Farm Broadcasters produce a series of radio interviews featuring experts discussing wind energy topics. The interviews are aimed at a rural stakeholder audience and are available as podcasts. On the Wind Powering America website, you can access past interviews on topics such as: Keys to Local Wind Energy Development Success, What to Know about Installing a Wind Energy System on Your Farm, and Wind Energy Development Can Revitalize Rural America. This postcard is a marketing piece that stakeholders can provide to interested parties; it will guide them to this online resource for podcast episodes.

  14. The Wind Integration National Dataset (WIND) toolkit (Presentation)

    SciTech Connect (OSTI)

    Caroline Draxl: NREL

    2014-01-01

    Regional wind integration studies require detailed wind power output data at many locations to perform simulations of how the power system will operate under high penetration scenarios. The wind datasets that serve as inputs into the study must realistically reflect the ramping characteristics, spatial and temporal correlations, and capacity factors of the simulated wind plants, as well as being time synchronized with available load profiles.As described in this presentation, the WIND Toolkit fulfills these requirements by providing a state-of-the-art national (US) wind resource, power production and forecast dataset.

  15. PUBLISHED ONLINE: 24 JUNE 2012 | DOI: 10.1038/NGEO1503 Morphology and dynamics of star dunes from

    E-Print Network [OSTI]

    Narteau, Clément

    dunes from numerical modelling Deguo Zhang1 , Clément Narteau1 *, Olivier Rozier1 and Sylvain Courrech du Pont2 * Star dunes are giant, pyramid-shaped dunes composed of interlaced arms. These arms suggest that the star dunes form as a result of complex interactions between a multidirectional wind

  16. Nucleosynthesis in the Ejecta of Neutron Star Mergers

    E-Print Network [OSTI]

    Dirk Martin; Albino Perego; Almudena Arcones; Oleg Korobkin; Friedrich-Karl Thielemann

    2015-09-25

    Heavy elements like gold, platinum or uranium are produced in the r-process, which needs neutron-rich and explosive environments. Neutron star mergers are a promising candidate for an r-process site. They exhibit three different channels for matter ejection fulfilling these conditions: dynamic ejecta due to tidal torques, neutrino-driven winds and evaporating matter from the accretion disk. We present a first study of the integrated nucleosynthesis for a neutrino-driven wind from a neutron star merger with a hyper-massive neutron star. Trajectories from a recent hydrodynamical simulation are divided into four different angle regions and post-processed with a reaction network. We find that the electron fraction varies around $Y_e \\approx 0.1 - 0.4$, but its distribution differs for every angle of ejection. Hence, the wind ejecta do not undergo a robust r-process, but rather possess distinct nucleosynthesis yields depending on the angle range. Compared to the dynamic ejecta, a smaller amount of neutron-rich matter gets unbound, but the production of lighter heavy elements with $A \\lesssim 130$ in the neutrino-driven wind can complement the strong r-process of the dynamic ejecta.

  17. The Biological and Molecular Analysis of a Tick-Encoded Serine Protease Inhibitor (S6) and its Role in the Feeding Cycle of the Lone Star Tick, Amblyomma americanum (L) (Acari: ixodidae) 

    E-Print Network [OSTI]

    Chalaire, Katelyn Cox

    2011-10-21

    silencing of S6 and S6/S17 mRNA was achieved, post-transcriptional gene knockdown had no effect on tick feeding efficiency or fecundity. These findings have been discussed in regards to the development of a vaccine against A. americanum and necessary future...

  18. ANNUAL WIND DATA REPORT Thompson Island

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    ANNUAL WIND DATA REPORT Thompson Island March 1, 2002 ­ February 28, 2003 Prepared.................................................................................................................... 11 Wind Speed Time Series........................................................................................................... 11 Wind Speed Distributions

  19. Wind Turbine Acoustic Noise A white paper

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    Wind Turbine Acoustic Noise A white paper Prepared by the Renewable Energy Research Laboratory...................................................................... 8 Sound from Wind Turbines .............................................................................................. 10 Sources of Wind Turbine Sound

  20. WIND DATA REPORT January -December, 2003

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Vinalhaven January - December, 2003 Prepared for Fox Islands Electric Cooperative...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distributions

  1. WIND DATA REPORT January -March, 2004

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Vinalhaven January - March, 2004 Prepared for Fox Islands Electric Cooperative...................................................................................................................... 9 Wind Speed Time Series............................................................................................................. 9 Wind Speed Distributions

  2. WIND DATA REPORT Deer Island Outfall

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Deer Island Outfall August 18, 2003 ­ December 4, 2003 Prepared for Massachusetts...................................................................................................................... 7 Wind Speed Time Series............................................................................................................. 7 Wind Speed Distributions

  3. WIND DATA REPORT Deer Island Parking Lot

    E-Print Network [OSTI]

    Massachusetts at Amherst, University of

    WIND DATA REPORT Deer Island Parking Lot May 1, 2003 ­ July 15, 2003 Prepared for Massachusetts...................................................................................................................... 7 Wind Speed Time Series............................................................................................................. 7 Wind Speed Distributions

  4. Wind Resource Assessment in Europe Using Emergy

    E-Print Network [OSTI]

    Paudel, Subodh; Santarelli, Massimo; Martin, Viktoria; Lacarriere, Bruno; Le Corre, Olivier

    2014-01-01

    of the Northern Europe offshore wind resource, Journal ofof theoretical offshore wind farm for Jacksonville, Florida,interesting areas for offshore wind farm construction and

  5. Helping Policymakers Evaluate Distributed Wind Options | Department...

    Office of Environmental Management (EM)

    consumers evaluate the effectiveness of policies that promote distributed wind-wind turbines installed at homes, farms, and busi-nesses. Distributed wind allows Americans to...

  6. Wavelet Analysis for Wind Fields Estimation

    E-Print Network [OSTI]

    Leite, Gladeston C.

    2013-01-01

    resource assessment and wind farm development in the UK. Inevaluation of oil spills and wind farms. Keywords: SAR; Winddata to characterize wind farms and their potential energy

  7. Advanced Coal Wind Hybrid: Economic Analysis

    E-Print Network [OSTI]

    Phadke, Amol

    2008-01-01

    Wind Integration Costs ..adequacy costs. Wind generation costs are also significantlyvalue. 3. We add wind integration cost to the levelized cost

  8. Wind Resource Assessment in Europe Using Emergy

    E-Print Network [OSTI]

    Paudel, Subodh; Santarelli, Massimo; Martin, Viktoria; Lacarriere, Bruno; Le Corre, Olivier

    2014-01-01

    of the Northern Europe offshore wind resource, Journal ofof theoretical offshore wind farm for Jacksonville, Florida,the interesting areas for offshore wind farm construction

  9. Advanced Coal Wind Hybrid: Economic Analysis

    E-Print Network [OSTI]

    Phadke, Amol

    2008-01-01

    of Figures Figure ES-1. Advanced Coal Wind Hybrid: Basicviii Figure 1. Advanced-Coal Wind Hybrid: Basic21 Figure 6. Comparison of ACWH and CCGT-Wind

  10. Correlations in thermal comfort and natural wind

    E-Print Network [OSTI]

    Kang, Ki-Nam; Song, Doosam; Schiavon, Stefano

    2013-01-01

    the average wind velocity and power spectrum exponent (?-of natural wind more accurately, power spectral analysisdata of natural wind versus the power spectral analysis

  11. Wind Resource Assessment in Europe Using Emergy

    E-Print Network [OSTI]

    Paudel, Subodh; Santarelli, Massimo; Martin, Viktoria; Lacarriere, Bruno; Le Corre, Olivier

    2014-01-01

    of theoretical offshore wind farm for Jacksonville, Florida,interesting areas for offshore wind farm construction andof theoretical offshore wind farm on Jacksonville, Florida

  12. 2012 Wind Technologies Market Report Presentation

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

    WIND AND WATER POWER PROGRAM 1 2012 Wind Technologies Market Report Ryan Wiser and Mark Bolinger Lawrence Berkeley National Laboratory Report Summary July 2013 WIND AND WATER POWER...

  13. Correlations in thermal comfort and natural wind

    E-Print Network [OSTI]

    Kang, Ki-Nam; Song, Doosam; Schiavon, Stefano

    2013-01-01

    Chaotic ?uctuation in natural wind and its application toof natural and mechanical wind in built environment usingcharacteristics of natural wind. Refrigeration 71 (821),

  14. Strong wind forcing of the ocean

    E-Print Network [OSTI]

    Zedler, Sarah E.

    2007-01-01

    of mesoscale and steady wind driven 1. Introduction 2. Modelparameterization at high wind speeds 1. Introduction 2. DataSupplementary Formulae 1. Wind Stress 2. Rankine Vortex A .

  15. Wind Farm Recommendation Report

    SciTech Connect (OSTI)

    John Reisenauer

    2011-05-01

    On April 21, 2011, an Idaho National Laboratory (INL) Land Use Committee meeting was convened to develop a wind farm recommendation for the Executive Council and a list of proposed actions for proceeding with the recommendation. In terms of land use, the INL Land Use Committee unanimously agrees that Site 6 is the preferred location of the alternatives presented for an INL wind farm. However, further studies and resolution to questions raised (stated in this report) by the INL Land Use Committee are needed for the preferred location. Studies include, but are not limited to, wind viability (6 months), bats (2 years), and the visual impact of the wind farm. In addition, cultural resource surveys and consultation (1 month) and the National Environmental Policy Act process (9 to 12 months) need to be completed. Furthermore, there is no documented evidence of developers expressing interest in constructing a small wind farm on INL, nor a specific list of expectations or concessions for which a developer might expect INL to cover the cost. To date, INL assumes the National Environmental Policy Act activities will be paid for by the Department of Energy and INL (the environmental assessment has only received partial funding). However, other concessions also may be expected by developers such as roads, fencing, power line installation, tie-ins to substations, annual maintenance, snow removal, access control, down-time, and remediation. These types of concessions have not been documented, as a request, from a developer and INL has not identified the short and long-term cost liabilities for such concessions should a developer expect INL to cover these costs. INL has not identified a go-no-go funding level or the priority this Wind Farm Project might have with respect to other nuclear-related projects, should the wind farm remain an unfunded mandate. The Land Use Committee recommends Legal be consulted to determine what, if any, liabilities exist with the Wind Farm Project and INL’s rights and responsibilities in regards to access to the wind farm once constructed. An expression of interest is expected to go out soon to developers. However, with the potential of 2 years of study remaining for Site 6, the expectation of obtaining meaningful interest from developers should be questioned.

  16. High-Speed Optical Spectroscopy of a Cataclysmic Variable Wind: BZ Camelopardalis

    E-Print Network [OSTI]

    F. A. Ringwald; T. Naylor

    1997-10-02

    BZ Cam is the first cataclysmic variable star with an accretion disk wind evident in its optical spectrum. The wind was found by Thorstensen, who discovered intermittent P Cygni profiles occurring simultaneously in He I 5876 Angstroms and H alpha. We have since obtained spectra with 0.4-Angstroms/pixel dispersion and 60-s time resolution. We find a wind much faster and more rapidly variable than the radiatively accelerated winds of OB stars, Wolf-Rayet stars, or luminous blue variables. Instead of showing blob ejection, the whole wind of BZ Cam appears to turn on and off. We use this to measure the acceleration law of a CV wind for the first time. The velocity increases linearly with time, attaining blue edge velocities near -3000 km/s, and absorption velocities near -1700 km/s, in 6 to 8 min after starting near rest. We also find a subsequent linear deceleration to nearly rest in 30 to 40 min, perhaps an effect of dilution as the wind expands. No periodicity from rotational outflow is obvious. This wind is erratic and incessantly variable, and perhaps bipolar and face-on, but not highly collimated. The P Cygni absorption events trace out sawtooth waves, occurring within 30 to 40 white dwarf radii from the disk. This is the approximate size of the disk, as well as the disk/wind transition region recently postulated by Knigge and Drew. We estimate a distance of 830 +/- 160 pc, and an orbital inclination i such that 12 < i(degrees) < 40.

  17. NREL: Wind Research - Offshore Wind Research

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of Marine andDrivetrainsNew WindDesign Tools

  18. NREL: Wind Research - Site Wind Resource Characteristics

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of Marine andDrivetrainsNewSite Wind Resource

  19. NREL: Wind Research - Small Wind Turbine Development

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of Marine andDrivetrainsNewSite Wind

  20. NREL: Wind Research - Wind Energy Videos

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass map shines lightGeospatialDevelopment of MarineOpportunities, Paths Wind

  1. Previous Wind Power Announcements (generation/wind)

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power Administration wouldMass mapSpeedingProgram Guidelines ThisHENPDepartment'sPrestonPreviousMembers | HomeWind

  2. High Winds Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsource History View NewGuam: Energyarea, CaliforniaHess RetailResolution ImagingWinds

  3. Prairie Winds Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on QA:QA J-E-1 SECTION J APPENDIXsourceII JumpQuarterly SmartDB-2, BluePoulsen Hybrid, LLCBiofuelsEthanol LLC Jump8)Wind

  4. Wyoming Wind Power Project (generation/wind)

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantityBonneville Power AdministrationRobust,Field-effectWorkingLos Alamos verifies largest single goldWind Power > Generation Hydro

  5. Accretion-Powered Stellar Winds III: Spin Equilibrium Solutions

    E-Print Network [OSTI]

    Sean Matt; Ralph E. Pudritz

    2008-02-12

    We compare the stellar wind torque calculated in a previous work (Paper II) to the spin-up and spin-down torques expected to arise from the magnetic interaction between a slowly rotating ($\\sim 10$% of breakup) pre-main-sequence star and its accretion disk. This analysis demonstrates that stellar winds can carry off orders of magnitude more angular momentum than can be transferred to the disk, provided that the mass outflow rates are greater than the solar wind. Thus, the equilibrium spin state is simply characterized by a balance between the angular momentum deposited by accretion and that extracted by a stellar wind. We derive a semi-analytic formula for predicting the equilibrium spin rate as a function only of the ratio of $\\dot M_{\\rm w} / \\dot M_{\\rm a}$ and a dimensionless magnetization parameter, $\\Psi \\equiv B_*^2 R_*^2 (\\dot M_{\\rm a} v_{\\rm esc})^{-1}$, where $\\dot M_{\\rm w}$ is the stellar wind mass outflow rate, $\\dot M_{\\rm a}$ the accretion rate, $B_*$ the stellar surface magnetic field strength, $R_*$ the stellar radius, and $v_{\\rm esc}$ the surface escape speed. For parameters typical of accreting pre-main-sequence stars, this explains spin rates of $\\sim 10$% of breakup speed for $\\dot M_{\\rm w} / \\dot M_{\\rm a} \\sim 0.1$. Finally, the assumption that the stellar wind is driven by a fraction of the accretion power leads to an upper limit to the mass flow ratio of $\\dot M_{\\rm w} / \\dot M_{\\rm a} \\la 0.6$.

  6. Advancements in Wind Integration Study Data Modeling: The Wind Integration National Dataset (WIND) Toolkit; Preprint

    SciTech Connect (OSTI)

    Draxl, C.; Hodge, B. M.; Orwig, K.; Jones, W.; Searight, K.; Getman, D.; Harrold, S.; McCaa, J.; Cline, J.; Clark, C.

    2013-10-01

    Regional wind integration studies in the United States require detailed wind power output data at many locations to perform simulations of how the power system will operate under high-penetration scenarios. The wind data sets that serve as inputs into the study must realistically reflect the ramping characteristics, spatial and temporal correlations, and capacity factors of the simulated wind plants, as well as be time synchronized with available load profiles. The Wind Integration National Dataset (WIND) Toolkit described in this paper fulfills these requirements. A wind resource dataset, wind power production time series, and simulated forecasts from a numerical weather prediction model run on a nationwide 2-km grid at 5-min resolution will be made publicly available for more than 110,000 onshore and offshore wind power production sites.

  7. Wind for Schools: A Wind Powering America Project (Alaska) (Brochure)

    SciTech Connect (OSTI)

    Not Available

    2010-02-01

    This brochure provides an overview of Wind Powering America's Wind for Schools Project, including a description of the project, the participants, funding sources, the basic configurations, and how interested parties can become involved.

  8. Wind for Schools: A Wind Powering America Project (Brochure)

    SciTech Connect (OSTI)

    Baring-Gould, I.

    2009-08-01

    This brochure provides an overview of Wind Powering America's Wind for Schools Project, including a description of the project, the participants, funding sources, the basic configurations, and how interested parties can become involved.

  9. Wind Vision: A New Era for Wind Power

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

    a period of volatility in natural gas fuel prices launched the modern era of U.S. wind power. Electric system operators and utilities now routinely consider wind power as part...

  10. EA-1726: Kahuku Wind Power, LLC Wind Power Generation Facility...

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

    Us Offices May 3, 2010 EA-1726: Final Environmental Assessment Loan Guarantee to Kahuku Wind Power, LLC for Construction of the Kahuku Wind Power Facility in Kahuku, O'ahu,...

  11. Chaninik Wind Group Wind Heat Smart Grids Final Report

    SciTech Connect (OSTI)

    Meiners, Dennis

    2013-06-29

    Final report summarizes technology used, system design and outcomes for US DoE Tribal Energy Program award to deploy Wind Heat Smart Grids in the Chaninik Wind Group communities in southwest Alaska.

  12. Wind Energy Status and Future Wind Engineering Challenges: Preprint

    SciTech Connect (OSTI)

    Thresher, R.; Schreck, S.; Robinson, M.; Veers, P.

    2008-08-01

    This paper describes the current status of wind energy technology, the potential for future wind energy development and the science and engineering challenges that must be overcome for the technology to meet its potential.

  13. Responses of floating wind turbines to wind and wave excitation

    E-Print Network [OSTI]

    Lee, Kwang Hyun

    2005-01-01

    The use of wind power has recently emerged as a promising alternative to conventional electricity generation. However, space requirements and public pressure to place unsightly wind turbines out of visual range make it ...

  14. Wind Powering America Webinar Series (Postcard), Wind Powering America (WPA)

    SciTech Connect (OSTI)

    Not Available

    2012-02-01

    Wind Powering America offers a free monthly webinar series that provides expert information on today?s key wind energy topics. This postcard is an outreach tool that provides a brief description of the webinars as well as the URL.

  15. Sandia Energy - Wind Vision 2015: A New Era for Wind Power in...

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

    Wind Vision 2015: A New Era for Wind Power in the United States Home Stationary Power Energy Conversion Efficiency Wind Energy Special Programs Wind Vision 2015: A New Era for Wind...

  16. Midsize Wind Turbines for the U.S. Community Wind Market | Department...

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

    Midsize Wind Turbines for the U.S. Community Wind Market Midsize Wind Turbines for the U.S. Community Wind Market A presentation on the midsize wind markets, including town-owned,...

  17. Gone with the Wind - The Potential Tragedy of the Common Wind

    E-Print Network [OSTI]

    Lifshitz-Goldberg, Yaei

    2010-01-01

    Regulatory Process for Offshore Wind Energy Development, 31Offshore and Larger Wind Farm Developments, BRrrIS WIND ENERGYfor Offshore Wind in Europe, TilE EUROPIEAN WIND ENERGY

  18. Wind Technology Advancements and Impacts on Western Wind Resources (Presentation)

    SciTech Connect (OSTI)

    Robichaud, R.

    2014-09-01

    Robi Robichaud made this presentation at the Bureau of Land Management West-wide Wind Opportunities and Constraints Mapping (WWOCM) Project public meeting in Denver, Colorado in September 2014. This presentation outlines recent wind technology advancements, evolving turbine technologies, and industry challenges. The presentation includes maps of mean wind speeds at 50-m, 80-m, and 100-m hub heights on BLM lands. Robichaud also presented on the difference in mean wind speeds from 80m to 100m in Wyoming.

  19. Modelling the observed properties of carbon-enhanced metal-poor stars using binary population synthesis

    E-Print Network [OSTI]

    Abate, C; Stancliffe, R J; Izzard, R G; Karakas, A I; Beers, T C; Lee, Y S

    2015-01-01

    The stellar population in the Galactic halo is characterised by a large fraction of CEMP stars. Most CEMP stars are enriched in $s$-elements (CEMP-$s$ stars), and some of these are also enriched in $r$-elements (CEMP-$s/r$ stars). One formation scenario proposed for CEMP stars invokes wind mass transfer in the past from a TP-AGB primary star to a less massive companion star which is presently observed. We generate low-metallicity populations of binary stars to reproduce the observed CEMP-star fraction. In addition, we aim to constrain our wind mass-transfer model and investigate under which conditions our synthetic populations reproduce observed abundance distributions. We compare the CEMP fractions and the abundance distributions determined from our synthetic populations with observations. Several physical parameters of the binary stellar population of the halo are uncertain, e.g. the initial mass function, the mass-ratio and orbital-period distributions, and the binary fraction. We vary the assumptions in o...

  20. Classical T Tauri stars: magnetic fields, coronae, and star-disc interactions

    E-Print Network [OSTI]

    Johnstone, C P; Gregory, S G; Donati, J -F; Hussain, G

    2013-01-01

    The magnetic fields of young stars set their coronal properties and control their spin evolution via the star-disc interaction and outflows. Using 14 magnetic maps of 10 classical T Tauri stars (CTTSs) we investigate their closed X-ray emitting coronae, their open wind-bearing magnetic fields, and the geometry of magnetospheric accretion flows. The magnetic fields of all the CTTSs are multipolar. Stars with simpler (more dipolar) large-scale magnetic fields have stronger fields, are slower rotators, and have larger X-ray emitting coronae compared to stars with more complex large-scale magnetic fields. The field complexity controls the distribution of open and closed field regions across the stellar surface, and strongly influences the location and shapes of accretion hot spots. However, the higher order field components are of secondary importance in determining the total unsigned open magnetic flux, which depends mainly on the strength of the dipole component and the stellar surface area. Likewise, the dipol...

  1. Optimum propeller wind turbines

    SciTech Connect (OSTI)

    Sanderson, R.J.; Archer, R.D.

    1983-11-01

    The Prandtl-Betz-Theodorsen theory of heavily loaded airscrews has been adapted to the design of propeller windmills which are to be optimized for maximum power coefficient. It is shown that the simpler, light-loading, constant-area wake assumption can generate significantly different ''optimum'' performance and geometry, and that it is therefore not appropriate to the design of propeller wind turbines when operating in their normal range of high-tip-speed-to-wind-speed ratio. Design curves for optimum power coefficient are presented and an example of the design of a typical two-blade optimum rotor is given.

  2. Wind Program News

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity of NaturalDukeWakefield Municipal Gas &SCE-Sessions |discussed how saving energy could betoldwind/wind-program-news en Wind

  3. WINDExchange: Wind Energy Ordinances

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Homesum_a_epg0_fpd_mmcf_m.xls" ,"Available from WebQuantity ofkandz-cm11 Outreach Home RoomPreservationBio-Inspired SolarAbout /Two0 -UsingHeatInformationDevelopment Resources andWindWind

  4. Wind Success Stories

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

    AFDC Printable Version Share this resource Send a link to EERE: Alternative Fuels Data Center Home Page to someone by E-mail Share EERE: Alternative Fuels Data Center Home Page on Facebook Tweet about EERE: Alternative Fuels Data Center Home Page on Twitter Bookmark EERE: Alternative Fuels Data Center Home Page on Google Bookmark EERE: Alternative Fuels Data Center Home Page on Delicious Rank EERE: Alternative FuelsofProgram: Report1538-1950DepartmentWaveWind Program R&DResearch and6 Wind

  5. A Census of the Carina Nebula. I: Cumulative Energy Input from Massive Stars

    E-Print Network [OSTI]

    Nathan Smith

    2006-01-04

    (abridged) The Carina Nebula (NGC 3372) is our richest nearby laboratory in which to study feedback through UV radiation and stellar winds from very massive stars during the formation of an OB association before supernova explosions have influenced the environment. This paper takes inventory of the combined effect from all the known massive stars that power the Carina Nebula. The present-day total ionizing photon luminosity produced by the 65 O stars and 3 WNL stars in Carina is about 1e51/s, the total bolometric luminosity of all stars earlier than B2 is 2.5e7 Lsun, and the total mechanical luminosity of stellar winds is about 1e5 Lsun. The total ionizing flux was about 25 per cent higher when eta Car was on the main sequence, before it and its companion were surrounded by its obscuring dust shell, and when the 3 WNL stars were on the main sequence. For the first 3 Myr, the net ionizing flux of the 70 O-type stars in Carina was about 150 times greater than in the Orion Nebula. About 400-500 Msun has been contributed to the region by stellar wind mass loss during the past 3 Myr. The net ionizing flux and mechanical luminosity are also given for the individual clusters Tr14, 15, and 16, and Bo10 and 11, which are relevant on smaller spatial scales.

  6. WIND ENERGY Wind Energ. 2013; 16:7790

    E-Print Network [OSTI]

    Papalambros, Panos

    increase the total power production using the same grid and foundation. Copyright © 2012 John Wiley & SonsWIND ENERGY Wind Energ. 2013; 16:77­90 Published online 19 March 2012 in Wiley Online Library Mieras2 1 Faculty of Aerospace Engineering, Department of Aerodynamics and Wind Energy, Delft University

  7. LIDAR Wind Speed Measurements of Evolving Wind Fields

    SciTech Connect (OSTI)

    Simley, E.; Pao, L. Y.

    2012-07-01

    Light Detection and Ranging (LIDAR) systems are able to measure the speed of incoming wind before it interacts with a wind turbine rotor. These preview wind measurements can be used in feedforward control systems designed to reduce turbine loads. However, the degree to which such preview-based control techniques can reduce loads by reacting to turbulence depends on how accurately the incoming wind field can be measured. Past studies have assumed Taylor's frozen turbulence hypothesis, which implies that turbulence remains unchanged as it advects downwind at the mean wind speed. With Taylor's hypothesis applied, the only source of wind speed measurement error is distortion caused by the LIDAR. This study introduces wind evolution, characterized by the longitudinal coherence of the wind, to LIDAR measurement simulations to create a more realistic measurement model. A simple model of wind evolution is applied to a frozen wind field used in previous studies to investigate the effects of varying the intensity of wind evolution. LIDAR measurements are also evaluated with a large eddy simulation of a stable boundary layer provided by the National Center for Atmospheric Research. Simulation results show the combined effects of LIDAR errors and wind evolution for realistic turbine-mounted LIDAR measurement scenarios.

  8. Metal-Poor Stars

    E-Print Network [OSTI]

    Anna Frebel

    2008-02-13

    The abundance patterns of metal-poor stars provide us a wealth of chemical information about various stages of the chemical evolution of the Galaxy. In particular, these stars allow us to study the formation and evolution of the elements and the involved nucleosynthesis processes. This knowledge is invaluable for our understanding of the cosmic chemical evolution and the onset of star- and galaxy formation. Metal-poor stars are the local equivalent of the high-redshift Universe, and offer crucial observational constraints on the nature of the first stars. This review presents the history of the first discoveries of metal-poor stars that laid the foundation to this field. Observed abundance trends at the lowest metallicities are described, as well as particular classes of metal-poor stars such as r-process and C-rich stars. Scenarios on the origins of the abundances of metal-poor stars and the application of large samples of metal-poor stars to cosmological questions are discussed.

  9. 2012 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2014-01-01

    prototype floating offshore wind turbine was deployed. AlsoWind Technologies Market Report No Commercial Offshore Turbineswind turbine nacelle assembly capacity; Charlie Bloch, Terese Decker, and Bruce Hamilton (Navigant Consulting) for assistance with the section on offshore

  10. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    a Changing Environment. WINDPOWER 2011. Poster Presentation.sources and others, e.g. , Windpower Monthly, the GlobalTurboWinds (1.6 MW), Nordic Windpower (2 MW), Emergya Wind

  11. AWEA Wind Project Siting Seminar

    Office of Energy Efficiency and Renewable Energy (EERE)

    The AWEA Wind Project Siting Seminar takes an in-depth look at the latest siting challenges and identify opportunities to reduce risks associated with the siting and operation of wind farms to...

  12. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    Monthly. Bloomberg New Energy Finance. 2010a. Q1 Wind MarketOutlook. February 2010. Bloomberg New Energy Finance.Bloomberg New Energy Finance. 2010b. Q2 Wind Market Outlook.

  13. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    Inc. 2009 Wind Technologies Market Report Mexico (7%). It isMexico Cowlitz Public Utility District WPPI Energy Alliant Energy Puget Sound Energy Northwestern Energy * Based on a projection of wind

  14. Value of Wind Power Forecasting

    SciTech Connect (OSTI)

    Lew, D.; Milligan, M.; Jordan, G.; Piwko, R.

    2011-04-01

    This study, building on the extensive models developed for the Western Wind and Solar Integration Study (WWSIS), uses these WECC models to evaluate the operating cost impacts of improved day-ahead wind forecasts.

  15. 2010 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2012-01-01

    and Transmission Study. NREL/SR-550-47078. Golden, Colorado:Wind Integration Study. NREL/ SR-550-47519. Golden,Wind and Solar Integration Study. NREL/SR-550-47434. Golden,

  16. 20% Wind Energy by 2030

    SciTech Connect (OSTI)

    Not Available

    2008-07-01

    This analysis explores one clearly defined scenario for providing 20% of our nations electricity demand with wind energy by 2030 and contrasts it to a scenario of no new wind power capacity.

  17. San Diego County- Wind Regulations

    Office of Energy Efficiency and Renewable Energy (EERE)

    The County of San Diego has established zoning guidelines for wind turbine systems of varying sizes in the unincorporated areas of San Diego County. Wind turbine systems can be classified as small,...

  18. Variables Affecting Economic Development of Wind Energy

    SciTech Connect (OSTI)

    Lantz, E.; Tegen, S.

    2008-07-01

    NREL's JEDI Wind model performed an analysis of wind-power-related economic development drivers. Economic development benefits for wind and coal were estimated using NREL's JEDI Wind and JEDI Coal models.

  19. Cost of Offshore Wind Energy Charlene Nalubega

    E-Print Network [OSTI]

    Mountziaris, T. J.

    water as well as on land based wind farms. The specific offshore wind energy case under consideration, most of the offshore wind farms are in Europe, which started being developed in the early 1990's Cost of Offshore Wind Energy

  20. Wind Power Overview Windpoweristhefastestgrowingformofrenewableenergy,withpoten-

    E-Print Network [OSTI]

    Wind Power Overview · Windpoweristhefastestgrowingformofrenewableenergy Offshore Wind Power for Florida? · AveragehouseholdelectricitycostsforFloridaare expectedtoincreaseby4Pensacola. · SiemensWindPowerNorthAmerica isbasedinOrlando. · Sugarland Wind is planning onshorewindfarmadjacentto

  1. Spittal Hill Wind Farm | Open Energy Information

    Open Energy Info (EERE)

    Spittal Hill Wind Farm Jump to: navigation, search Name: Spittal Hill Wind Farm Place: United Kingdom Sector: Wind energy Product: Set up to manage wind projects in the Scotland....

  2. Class Generation for Numerical Wind Atlases

    E-Print Network [OSTI]

    Class Generation for Numerical Wind Atlases Risø National Laboratory Wind Energy Department Constructing a Numerical Wind Atlas 5 2.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . 13 2.4 The existing procedure at Risø . . . . . . . . . . . . . . . . . . . 13 3 Representing a Wind

  3. Wind Technologies and Evolving Opportunities (Presentation)

    SciTech Connect (OSTI)

    Robi Robichaud

    2014-03-01

    This presentation provides an overview of wind energy research being conducted at the National Wind Technology Center, market and technology trends in wind energy, and opportunities for wind technology.

  4. DWEA SMART Wind Composites Subgroup

    Broader source: Energy.gov [DOE]

    Monday, February 16, 6:00 PMOpen to all SMART Wind participants: “Dutch Treat” group dinner, RSVP required | Location: TBD

  5. 2012 Wind Technologies Market Report

    SciTech Connect (OSTI)

    Wiser, Ryan; Bolinger, Mark

    2013-08-01

    An annual report on the wind energy industry including key statistics, economic data, installation, capacity, and generation statistics, and more.

  6. 2011 Wind Technologies Market Report

    SciTech Connect (OSTI)

    Wiser, Ryan; Bolinger, Mark

    2012-08-01

    An annual report on the wind energy industry including key statistics, economic data, installation, capacity, and generation statistics, and more.

  7. 2008 WIND TECHNOLOGIES MARKET REPORT

    E-Print Network [OSTI]

    Bolinger, Mark

    2010-01-01

    wind Source: EIA, Ventyx, AWEA, IREC, Berkeley Lab Figure 2.Renewable Energy Council (IREC) and Berkeley Lab. Data on

  8. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    wind energy generation within the Electric ReliabilityEnergy Regulatory Commission General Electric Corporation gigawatt generation and

  9. 2009 Wind Technologies Market Report

    E-Print Network [OSTI]

    Wiser, Ryan

    2010-01-01

    and Germany’s 25,813 MW. Several countries are beginning to achieve relatively high levels of wind energy

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

    SciTech Connect (OSTI)

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

    2010-05-10

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

  11. Advanced Coal Wind Hybrid: Economic Analysis

    E-Print Network [OSTI]

    Phadke, Amol

    2008-01-01

    When the wind generators are producing power, the powerWhen the wind generators are not producing power, the power

  12. Low-Maintenance Wind Power System

    E-Print Network [OSTI]

    Rasson, Joseph E

    2010-01-01

    Improved Vertical Axis Wind Turbine and Aerodynamic ControlDarrieus Vertical Axis Wind Turbines and Aerodynamic Control

  13. Wind Tunnel Building - 4 

    E-Print Network [OSTI]

    Unknown

    2005-06-30

    of the Sargassum loop system sheds light on the seasonal migration patterns of the macro-algae. Through use of NASA’s Landsat satellite imagery the presence and abundance of Sargassum has been analyzed. Based on several factors, such as ocean currents, wind...

  14. Coastal Ohio Wind Project

    SciTech Connect (OSTI)

    Gorsevski, Peter; Afjeh, Abdollah; Jamali, Mohsin; Bingman, Verner

    2014-04-04

    The Coastal Ohio Wind Project intends to address problems that impede deployment of wind turbines in the coastal and offshore regions of Northern Ohio. The project evaluates different wind turbine designs and the potential impact of offshore turbines on migratory and resident birds by developing multidisciplinary research, which involves wildlife biology, electrical and mechanical engineering, and geospatial science. Firstly, the project conducts cost and performance studies of two- and three-blade wind turbines using a turbine design suited for the Great Lakes. The numerical studies comprised an analysis and evaluation of the annual energy production of two- and three-blade wind turbines to determine the levelized cost of energy. This task also involved wind tunnel studies of model wind turbines to quantify the wake flow field of upwind and downwind wind turbine-tower arrangements. The experimental work included a study of a scaled model of an offshore wind turbine platform in a water tunnel. The levelized cost of energy work consisted of the development and application of a cost model to predict the cost of energy produced by a wind turbine system placed offshore. The analysis found that a floating two-blade wind turbine presents the most cost effective alternative for the Great Lakes. The load effects studies showed that the two-blade wind turbine model experiences less torque under all IEC Standard design load cases considered. Other load effects did not show this trend and depending on the design load cases, the two-bladed wind turbine showed higher or lower load effects. The experimental studies of the wake were conducted using smoke flow visualization and hot wire anemometry. Flow visualization studies showed that in the downwind turbine configuration the wake flow was insensitive to the presence of the blade and was very similar to that of the tower alone. On the other hand, in the upwind turbine configuration, increasing the rotor blade angle of attack reduced the wake size and enhanced the vortices in the flow downstream of the turbine-tower compared with the tower alone case. Mean and rms velocity distributions from hot wire anemometer data confirmed that in a downwind configuration, the wake of the tower dominates the flow, thus the flow fields of a tower alone and tower-turbine combinations are nearly the same. For the upwind configuration, the mean velocity shows a narrowing of the wake compared with the tower alone case. The downwind configuration wake persisted longer than that of an upwind configuration; however, it was not possible to quantify this difference because of the size limitation of the wind tunnel downstream of the test section. The water tunnel studies demonstrated that the scale model studies could be used to adequately produce accurate motions to model the motions of a wind turbine platform subject to large waves. It was found that the important factors that affect the platform is whether the platform is submerged or surface piercing. In the former, the loads on the platform will be relatively reduced whereas in the latter case, the structure pierces the wave free surface and gains stiffness and stability. The other important element that affects the movement of the platform is depth of the sea in which the wind turbine will be installed. Furthermore, the wildlife biology component evaluated migratory patterns by different monitoring systems consisting of marine radar, thermal IR camera and acoustic recorders. The types of radar used in the project are weather surveillance radar and marine radar. The weather surveillance radar (1988 Doppler), also known as Next Generation Radar (NEXRAD), provides a network of weather stations in the US. Data generated from this network were used to understand general migratory patterns, migratory stopover habitats, and other patterns caused by the effects of weather conditions. At a local scale our marine radar was used to complement the datasets from NEXRAD and to collect additional monitoring parameters such as passage rates, flight paths, flight directi

  15. Contracting for wind generation

    E-Print Network [OSTI]

    Newbery, David

    on the discount offered to small wind farms, but it might even be as high as 15-20%. These figures may also reflect risk surrounding ROC prices, which although apparently stable, are subject to political and credibility risk. EPRG No 1120 14 ahead of time...

  16. SPRING 2014 wind energy's impact

    E-Print Network [OSTI]

    Balasubramanian, Ravi

    , operators of offshore wind farms will have an increasing interest in technology that can reduce incidents Interactions with Offshore Wind Energy Facilities," involves the design, deployment and testing species, and about 150 other birds on two wind farms in Wyoming. This was the first enforcement of federal

  17. WIND ENERGY AND NEGATIVE PRICING

    E-Print Network [OSTI]

    McCalley, James D.

    at negative prices #12;Wind power and negative prices · Wind power production is related to electricity power integration · Negative prices are "market distortions" that need to be addressed · "PTC aggravatesWIND ENERGY AND NEGATIVE PRICING Is Production Tax Credit to Blame? Yu Wang Iowa State University

  18. 2011 Wind Technologies Market Report

    E-Print Network [OSTI]

    Bolinger, Mark

    2013-01-01

    of Energy (DOE) Wind & Water Power Program team, and inwere funded by the Wind & Water Power Program, Office ofWater and Power’s proposed Barren Ridge Renewable Transmission Project is expected to provide 1,100 MW of transmission capacity to transport wind and

  19. Model Predictive Control Wind Turbines

    E-Print Network [OSTI]

    Model Predictive Control of Wind Turbines Martin Klauco Kongens Lyngby 2012 IMM-MSc-2012-65 #12;Summary Wind turbines are the biggest part of the green energy industry. Increasing interest control strategies. Control strategy has a significant impact on the wind turbine operation on many levels

  20. Wind Energy Information Guide 2004

    SciTech Connect (OSTI)

    anon.

    2004-01-01

    The guide provides a list of contact information and Web site addresses for resources that provide a range of general and technical information about wind energy, including general information, wind and renewable energy, university programs and research institutes, international wind energy associations and others.

  1. Wind Turbine Blockset General Overview

    E-Print Network [OSTI]

    Wind Turbine Blockset in Saber General Overview and Description of the Models Florin Iov, Adrian Turbine Blockset in Saber Abstract. This report presents a new developed Saber Toolbox for wind turbine, optimize and design wind turbines". The report provides a quick overview of the Saber and then explains

  2. 2012 Wind Technologies Market Report

    Office of Energy Efficiency and Renewable Energy (EERE)

    The 2012 Wind Technologies Market Report is a comprehensive analyses of the U.S. distributed wind energy market ever published, this report provides a detailed overview of developments and trends in the U.S. wind power market, focusing on 2012.

  3. Bird orientation: compensation for wind

    E-Print Network [OSTI]

    Thorup, Kasper

    Bird orientation: compensation for wind drift in migrating raptors is age dependent Kasper Thorup1 14.04.03 Despite the potentially strong effect of wind on bird orientation, our understanding of how wind drift affects migrating birds is still very limited. Using data from satellite-based radio

  4. Energy 101: Wind Turbines - 2014 Update

    ScienceCinema (OSTI)

    None

    2014-06-05

    See how wind turbines generate clean electricity from the power of wind. The video highlights the basic principles at work in wind turbines, and illustrates how the various components work to capture and convert wind energy to electricity. This updated version also includes information on the Energy Department's efforts to advance offshore wind power. Offshore wind energy footage courtesy of Vestas.

  5. Version:April 2014 Wind Energy EFA

    E-Print Network [OSTI]

    Kusiak, Andrew

    Version:April 2014 Wind Energy EFA Wind energy has become a major source of clean energy. Wind backgrounds and knowledge of wind energy fundamentals are needed to fill these jobs. The Wind Energy EFA prepares students for a career in wind energy, and allows for completing all requirements

  6. The Future of Offshore Wind Energy

    E-Print Network [OSTI]

    Firestone, Jeremy

    1 The Future of Offshore Wind Energy #12;2 #12;3 Offshore Wind Works · Offshore wind parks: 28 in 10 countries · Operational since 1991 · Current installed capacity: 1,250 MW · Offshore wind parks in the waters around Europe #12;4 US Offshore Wind Projects Proposed Atlantic Ocean Gulf of Mexico Cape Wind

  7. Energy 101: Wind Turbines - 2014 Update

    SciTech Connect (OSTI)

    2014-05-06

    See how wind turbines generate clean electricity from the power of wind. The video highlights the basic principles at work in wind turbines, and illustrates how the various components work to capture and convert wind energy to electricity. This updated version also includes information on the Energy Department's efforts to advance offshore wind power. Offshore wind energy footage courtesy of Vestas.

  8. Star-Crossed 

    E-Print Network [OSTI]

    Tyellas

    2002-01-01

    - tion effects could be simulated. The 1. 5 m x 1. 5 m wind tunnel is located at Texas ASM Agricultural Engineering Research shops. The blower (Westinghouse Model 429A) and the electric motor (Baldor 40 h. p. ) system of the wind tunnel is capable...

  9. Applied wind energy research at the National Wind Technology Center

    SciTech Connect (OSTI)

    Robinson, M C; Tu, P

    1996-06-01

    Applied research activities at the National Wind Technology Center are divided into several technical disciplines. Not surprisingly, these engineering and science disciplines highlight the technology similarities between aircraft and wind turbine design requirements. More often than not, wind turbines are assumed to be a subset of the much larger and more comprehensive list of well understood aerospace engineering accomplishments and it is difficult for the general public to understand the poor performance history of wind turbines in sustained operation. Often overlooked are the severe environmental conditions and operational demands placed on turbine designs which define unique requirements beyond typical aerospace applications. It is the role of the National Wind Technology Center to investigate and quantify the underlying physical phenomena which make the wind turbine design problem unique and to provide the technology advancements necessary to overcome current operational limitations. This paper provides a brief overview of research areas involved with the design of wind turbines.

  10. Assessment Of The Wind Farm Impact On The Radar

    E-Print Network [OSTI]

    Norman, Evgeny D

    2010-01-01

    This study shows the means to evaluate the wind farm impact on the radar. It proposes the set of tools, which can be used to realise this objective. The big part of report covers the study of complex pattern propagation factor as the critical issue of the Advanced Propagation Model (APM). Finally, the reader can find here the implementation of this algorithm - the real scenario in Inverness airport (the United Kingdom), where the ATC radar STAR 2000, developed by Thales Air Systems, operates in the presence of several wind farms. Basically, the project is based on terms of the department "Strategy Technology & Innovation", where it has been done. Also you can find here how the radar industry can act with the problem engendered by wind farms. The current strategies in this area are presented, such as a wind turbine production, improvements of air traffic handling procedures and the collaboration between developers of radars and wind turbines. The possible strategy for Thales as a main pioneer was given as ...

  11. Wind/Hybrid Electricity Applications

    SciTech Connect (OSTI)

    McDaniel, Lori

    2001-03-31

    Wind energy is widely recognized as the most efficient and cost effective form of new renewable energy available in the Midwest. New utility-scale wind farms (arrays of large turbines in high wind areas producing sufficient energy to serve thousands of homes) rival the cost of building new conventional forms of combustion energy plants, gas, diesel and coal power plants. Wind energy is not subject to the inflationary cost of fossil fuels. Wind energy can also be very attractive to residential and commercial electric customers in high wind areas who would like to be more self-sufficient for their energy needs. And wind energy is friendly to the environment at a time when there is increasing concern about pollution and climate change. However, wind energy is an intermittent source of power. Most wind turbines start producing small amounts of electricity at about 8-10 mph (4 meters per second) of wind speed. The turbine does not reach its rated output until the wind reaches about 26-28 mph (12 m/s). So what do you do for power when the output of the wind turbine is not sufficient to meet the demand for energy? This paper will discuss wind hybrid technology options that mix wind with other power sources and storage devices to help solve this problem. This will be done on a variety of scales on the impact of wind energy on the utility system as a whole, and on the commercial and small-scale residential applications. The average cost and cost-benefit of each application along with references to manufacturers will be given. Emerging technologies that promise to shape the future of renewable energy will be explored as well.

  12. How plausible are the proposed formation scenarios of CEMP-r/s stars?

    E-Print Network [OSTI]

    Abate, Carlo; Liu, Zheng-Wei

    2016-01-01

    CEMP-$r/s$ stars are metal-poor stars with enhanced abundances of carbon and heavy elements associated with the slow ($s$-) and rapid ($r$-) neutron-capture process. It is believed that carbon and $s$-elements were accreted from the wind of an AGB primary star, a scenario that is generally accepted to explain the formation of CEMP stars that are only enhanced in $s$-elements (CEMP-$s$ stars). The origin of $r$-element-enrichment in CEMP-$r/s$ stars is debated and many formation scenarios have been put forward. We aim to determine the likelihood of the scenarios proposed to explain the formation of CEMP-$r/s$ stars. We calculate the frequency of CEMP-$r/s$ stars among CEMP-$s$ stars for a variety of scenarios, and we compare it with that determined from an observed sample of CEMP-$r/s$ stars collected from the literature. The theoretical frequency of CEMP-$r/s$ stars predicted in most scenarios underestimates the observed ratio by at least a factor of 5. If the enrichments in $s$- and $r$-elements are independ...

  13. Relics of metal-free low mass stars exploding as thermonuclear supernovae

    E-Print Network [OSTI]

    Takuji Tsujimoto; Toshikazu Shigeyama

    2006-01-16

    Renewed interest in the first stars that were formed in the universe has led to the discovery of extremely iron-poor stars. Since several competing scenarios exist, our understanding of the mass range that determines the observed elemental abundances remains unclear. In this study, we consider three well-studied metal-poor stars in terms of the theoretical supernovae (SNe) model. Our results suggest that the observed abundance patterns in the metal-poor star BD +80 245 and the pair of stars HD 134439/40 agree strongly with the theoretical possibility that these stars inherited their heavy element abundance patterns from SNe initiated by thermonuclear runaways in the degenerate carbon-oxygen cores of primordial asymptotic giant branch stars with \\~3.5-5 solar masses. Recent theoretical calculations have predicted that such SNe could be originated from metal-free stars in the intermediate mass range. On the other hand, intermediate mass stars containing some metals would end their lives as white dwarfs after expelling their envelopes in the wind due to intense momentum transport from outgoing photons to heavy elements. This new pathway for the formation of SNe requires that stars are formed from the primordial gas. Thus, we suggest that stars of a few solar masses were formed from the primordial gas and that some of them caused thermonuclear explosions when the mass of their degenerate carbon-oxygen cores increased to the Chandrasekhar limit without experiencing efficient mass loss.

  14. Lower Sioux Wind Feasibility & Development

    SciTech Connect (OSTI)

    Minkel, Darin

    2012-04-01

    This report describes the process and findings of a Wind Energy Feasibility Study (Study) conducted by the Lower Sioux Indian Community (Community). The Community is evaluating the development of a wind energy project located on tribal land. The project scope was to analyze the critical issues in determining advantages and disadvantages of wind development within the Community. This analysis addresses both of the Community's wind energy development objectives: the single turbine project and the Commerical-scale multiple turbine project. The main tasks of the feasibility study are: land use and contraint analysis; wind resource evaluation; utility interconnection analysis; and project structure and economics.

  15. 2013 Wind Technologies Market Report

    SciTech Connect (OSTI)

    Wiser, R.; Bolinger, M.; Barbose, G.; Darghouth, N.; Hoen, B.; Mills, A.; Weaver, S.; Porter, K.; Buckley, M.; Oteri, F.; Tegen, S.

    2014-08-01

    This annual report provides a detailed overview of developments and trends in the U.S. wind power market, with a particular focus on 2013. This 2013 edition updates data presented in previous editions while highlighting key trends and important new developments. The report includes an overview of key installation-related trends; trends in wind power capacity growth; how that growth compares to other countries and generation sources; the amount and percentage of wind energy in individual states; the status of offshore wind power development and the quantity of proposed wind power capacity in various interconnection queues in the United States.

  16. The Optical Wind Line Variability of $\\eta$ Carinae During the 2009.0 Event

    E-Print Network [OSTI]

    Richardson, Noel D; Gull, Theodore R; Moffat, Anthony F J; St-Jean, Lucas

    2015-01-01

    We report on high-resolution spectroscopy of the 2009.0 spectroscopic event of $\\eta$ Carinae collected via SMARTS observations using the CTIO 1.5 m telescope and echelle spectrograph. Our observations were made almost every night over a two-month interval around the photometric minimum of $\\eta$ Car associated with the periastron passage of a hot companion. The photoionizing flux of the companion and heating related to colliding winds causes large changes in the wind properties of the massive primary star. Here we present an analysis of temporal variations in a sample of spectral lines that are clearly formed in the wind of the primary star. These lines are affected by a changing illumination of the flux of the secondary star during the periastron passage. We document the sudden onset of blue-shifted absorption that occurred in most of the lines near or slightly after periastron, and we argue that these absorption components are seen when we view the relatively undisturbed wind of the foreground primary star...

  17. Offshore Wind Research (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2011-10-01

    This 2-page fact sheet describes NREL's offshore wind research and development efforts and capabilities. The National Renewable Energy Laboratory is internationally recognized for offshore wind energy research and development (R&D). Its experience and capabilities cover a wide spectrum of wind energy disciplines. NREL's offshore wind R&D efforts focus on critical areas that address the long-term needs of the offshore wind energy industry and the Department of Energy (DOE). R&D efforts include: (1) Developing offshore design tools and methods; (2) Collaborating with international partners; (3) Testing offshore systems and developing standards; (4) Conducting economic analyses; (5) Characterizing offshore wind resources; and (6) Identifying and mitigating offshore wind grid integration challenges and barriers. NREL has developed and maintains a robust, open-source, modular computer-aided engineering (CAE) tool, known as FAST. FAST's state-of-the-art capabilities provide full dynamic system simulation for a range of offshore wind systems. It models the coupled aerodynamic, hydrodynamic, control system, and structural response of offshore wind systems to support the development of innovative wind technologies that are reliable and cost effective. FAST also provides dynamic models of wind turbines on offshore fixed-bottom systems for shallow and transitional depths and floating-platform systems in deep water, thus enabling design innovation and risk reduction and facilitating higher performance designs that will meet DOE's cost of energy, reliability, and deployment objectives.

  18. Hot galactic winds constrained by the X-ray luminosities of galaxies

    SciTech Connect (OSTI)

    Zhang, Dong; Thompson, Todd A. [Department of Astronomy, The Ohio State University, 140 W. 18th Avenue, Columbus, OH 43210 (United States); Murray, Norman [Canadian Institute for Theoretical Astrophysics, 60 St. George Street, University of Toronto, Toronto, ON M5S 3H8 (Canada); Quataert, Eliot, E-mail: dzhang@astronomy.ohio-state.edu, E-mail: thompson@astronomy.ohio-state.edu [Astronomy Department and Theoretical Astrophysics Center, 601 Campbell Hall, University of California, Berkeley, CA 94720 (United States)

    2014-04-01

    Galactic superwinds may be driven by very hot outflows generated by overlapping supernovae within the host galaxy. We use the Chevalier and Clegg (CC85) wind model and the observed correlation between X-ray luminosities of galaxies and their star formation rates (SFRs) to constrain the mass-loss rates ( M-dot {sub hot}) across a wide range of SFRs, from dwarf starbursts to ultraluminous infrared galaxies. We show that for fixed thermalization and mass-loading efficiencies, the X-ray luminosity of the hot wind scales as L{sub X} ?SFR{sup 2}, significantly steeper than is observed for star-forming galaxies: L{sub X} ?SFR. Using this difference, we constrain the mass-loading and thermalization efficiency of hot galactic winds. For reasonable values of the thermalization efficiency (? 1) and for SFR ? 10 M {sub ?} yr{sup –1} we find that M-dot {sub hot}/SFR? 1, which is significantly lower than required by integrated constraints on the efficiency of stellar feedback in galaxies and potentially too low to explain observations of winds from rapidly star-forming galaxies. In addition, we highlight the fact that heavily mass-loaded winds cannot be described by the adiabatic CC85 model because they become strongly radiative.

  19. Reduced vibration motor winding arrangement

    DOE Patents [OSTI]

    Slavik, C.J.; Rhudy, R.G.; Bushman, R.E.

    1997-11-11

    An individual phase winding arrangement having a sixty electrical degree phase belt width for use with a three phase motor armature includes a delta connected phase winding portion and a wye connected phase winding portion. Both the delta and wye connected phase winding portions have a thirty electrical degree phase belt width. The delta and wye connected phase winding portions are each formed from a preselected number of individual coils each formed, in turn, from an unequal number of electrical conductor turns in the approximate ratio of {radical}3. The individual coils of the delta and wye connected phase winding portions may either be connected in series or parallel. This arrangement provides an armature winding for a three phase motor which retains the benefits of the widely known and utilized thirty degree phase belt concept, including improved mmf waveform and fundamental distribution factor, with consequent reduced vibrations and improved efficiency. 4 figs.

  20. Reduced vibration motor winding arrangement

    DOE Patents [OSTI]

    Slavik, Charles J. (Rexford, NY); Rhudy, Ralph G. (Scotia, NY); Bushman, Ralph E. (Lathem, NY)

    1997-01-01

    An individual phase winding arrangement having a sixty electrical degree phase belt width for use with a three phase motor armature includes a delta connected phase winding portion and a wye connected phase winding portion. Both the delta and wye connected phase winding portions have a thirty electrical degree phase belt width. The delta and wye connected phase winding portions are each formed from a preselected number of individual coils each formed, in turn, from an unequal number of electrical conductor turns in the approximate ratio of .sqroot.3. The individual coils of the delta and wye connected phase winding portions may either be connected in series or parallel. This arrangement provides an armature winding for a three phase motor which retains the benefits of the widely known and utilized thirty degree phase belt concept, including improved mmf waveform and fundamental distribution factor, with consequent reduced vibrations and improved efficiency.