National Library of Energy BETA

Sample records for gateway solar wind

  1. Towards an Industry Data Gateway: An Integrated Platform for the Analysis of Wind Turbine Data

    E-Print Network [OSTI]

    Towards an Industry Data Gateway: An Integrated Platform for the Analysis of Wind Turbine Data monitoring of sensor information from wind turbines, and how a data gateway can help to increase in the context of wind turbines. It goes on to describe the innovative approach used in VAVID to meet

  2. Petrovay: Solar physics Solar wind and heliosphere THE SOLAR WIND AND THE HELIOSPHERE

    E-Print Network [OSTI]

    Petrovay, Kristóf

    Petrovay: Solar physics Solar wind and heliosphere THE SOLAR WIND AND THE HELIOSPHERE 1951: First proposal of solar corpuscular radiation by Biermann, to explain slight deviation of comets' ion tails from radial (aberration effect). 1958: Parker's supersonic wind model 1962: Mariner-2 detects solar wind. v

  3. Supercomputers Capture Turbulence in the Solar Wind

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

    Capture Turbulence in the Solar Wind Supercomputers Capture Turbulence in the Solar Wind Berkeley Lab visualizations could help scientists forecast destructive space weather...

  4. SciTech Connect: "solar plasma wind"

    Office of Scientific and Technical Information (OSTI)

    solar plasma wind" Find + Advanced Search Term Search Semantic Search Advanced Search All Fields: "solar plasma wind" Semantic Semantic Term Title: Full Text: Bibliographic...

  5. Forecasting Solar Wind Speeds

    E-Print Network [OSTI]

    Takeru K. Suzuki

    2006-02-03

    By explicitly taking into account effects of Alfven waves, I derive from a simple energetics argument a fundamental relation which predicts solar wind (SW) speeds in the vicinity of the earth from physical properties on the sun. Kojima et al. recently found from their observations that a ratio of surface magnetic field strength to an expansion factor of open magnetic flux tubes is a good indicator of the SW speed. I show by using the derived relation that this nice correlation is an evidence of the Alfven wave which accelerates SW in expanding flux tubes. The observations further require that fluctuation amplitudes of magnetic field lines at the surface should be almost universal in different coronal holes, which needs to be tested by future observations.

  6. Wind and Solar Curtailment: Preprint

    SciTech Connect (OSTI)

    Lew, D.; Bird, L.; Milligan, M.; Speer, B.; Wang, X.; Carlini, E. M.; Estanqueiro, A.; Flynn, D.; Gomez-Lazaro, E.; Menemenlis, N.; Orths, A.; Pineda, I.; Smith, J. C.; Soder, L.; Sorensen, P.; Altiparmakis, A.; Yoh, Y.

    2013-09-01

    High penetrations of wind and solar generation on power systems are resulting in increasing curtailment. Wind and solar integration studies predict increased curtailment as penetration levels grow. This paper examines experiences with curtailment on bulk power systems internationally. It discusses how much curtailment is occurring, how it is occurring, why it is occurring, and what is being done to reduce curtailment. This summary is produced as part of the International Energy Agency Wind Task 25 on Design and Operation of Power Systems with Large Amounts of Wind Power.

  7. RELATED LINKS Photos: Solar & Wind

    E-Print Network [OSTI]

    RELATED LINKS Photos: Solar & Wind Power for the Home Photos: Energy Efficiency for the Home Photos of Architects (AIA) Home Design Trends Survey for the second quarter of 2009 that focused on emerging home

  8. STATIONARITY IN SOLAR WIND FLOWS

    SciTech Connect (OSTI)

    Perri, S.; Balogh, A. E-mail: a.balogh@imperial.ac.u

    2010-05-01

    By using single-point measurements in space physics it is possible to study a phenomenon only as a function of time. This means that we cannot have direct access to information about spatial variations of a measured quantity. However, the investigation of the properties of turbulence and of related phenomena in the solar wind widely makes use of an approximation frequently adopted in hydrodynamics under certain conditions, the so-called Taylor hypothesis; indeed, the solar wind flow has a bulk velocity along the radial direction which is much higher than the velocity of a single turbulent eddy embedded in the main flow. This implies that the time of evolution of the turbulent features is longer than the transit time of the flow through the spacecraft position, so that the turbulent field can be considered frozen into the solar wind flow. This assumption allows one to easily associate time variations with spatial variations and stationarity to homogeneity. We have investigated, applying criteria for weak stationarity to Ulysses magnetic field data in different solar wind regimes, at which timescale and under which conditions the hypothesis of stationarity, and then of homogeneity, of turbulence in the solar wind is well justified. We extend the conclusions of previous studies by Matthaeus and Goldstein to different parameter ranges in the solar wind. We conclude that the stationarity assumption in the inertial range of turbulence on timescales of 10 minutes to 1 day is reasonably satisfied in fast and uniform solar wind flows, but that in mixed, interacting fast, and slow solar wind streams the assumption is frequently only marginally valid.

  9. Solar and Wind Rights

    Broader source: Energy.gov [DOE]

    The law stipulates that associations must adopt an energy policy statement specifying details such as location, design, and architectural requirements of the solar energy systems within 120 days...

  10. ASYMMETRIC SOLAR WIND ELECTRON DISTRIBUTIONS

    SciTech Connect (OSTI)

    Yoon, Peter H.; Kim, Sunjung; Lee, Junggi; Lee, Junhyun; Park, Jongsun; Park, Kyungsun; Seough, Jungjoon [School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 446-701 (Korea, Republic of); Hong, Jinhy [Department of Physics, Korea Advanced Institute of Science and Technology, Daejeon 305-701 (Korea, Republic of)

    2012-08-20

    The present paper provides a possible explanation for the solar wind electron velocity distribution functions possessing asymmetric energetic tails. By numerically solving the electrostatic weak turbulence equations that involve nonlinear interactions among electrons, Langmuir waves, and ion-sound waves, it is shown that different ratios of ion-to-electron temperatures lead to the generation of varying degrees of asymmetric tails. The present finding may be applicable to observations in the solar wind near 1 AU and in other regions of the heliosphere and interplanetary space.

  11. Western Wind and Solar Integration Study

    SciTech Connect (OSTI)

    GE Energy

    2010-05-01

    This report provides a full description of the Western Wind and Solar Integration Study (WWSIS) and its findings.

  12. Turbulence of the Solar Wind Studies of the Solar Wind Using the ACE and Helios Spacecraft

    E-Print Network [OSTI]

    provide enough energy to account for the heating of the solar wind relative to an adiabatic expansion Composition Explorer to compute the cascade rate of the turbulence in the solar wind. We nd the energy cascadeTurbulence of the Solar Wind Studies of the Solar Wind Using the ACE and Helios Spacecraft Bejamin

  13. Solar wind electron density and temperature over solar cycle 23: Thermal noise measurements on Wind

    E-Print Network [OSTI]

    California at Berkeley, University of

    Solar wind electron density and temperature over solar cycle 23: Thermal noise measurements on Wind; received in revised form 6 April 2005; accepted 25 April 2005 Abstract We present the solar wind plasma parameters obtained from the Wind spacecraft during more than nine years, encompassing almost the whole solar

  14. 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

  15. Maximizing Network Lifetime Via 3G Gateway Assignment in Dual-Radio Sensor Networks

    E-Print Network [OSTI]

    Liang, Weifa

    - ments, such as temperature, humidity, wind, solar radiation, etc. [3]. Sensor nodes are typically as well as in the idling cost [5]. If all sensors are gateways, they will run out of energy within a shortMaximizing Network Lifetime Via 3G Gateway Assignment in Dual-Radio Sensor Networks Xu Xu, Weifa

  16. The Structure of the Solar Wind in the Inner Heliosphere

    E-Print Network [OSTI]

    Lee, Christina On-Yee

    2010-01-01

    Improvement in the prediction of solar wind condi- tions2007, Metric for solar wind prediction models: Comparison oflong- term predictions of the episodic solar disturbances,

  17. The Solar Wind Helium Abundance: Variation with Wind Speed and the Solar Cycle

    E-Print Network [OSTI]

    Richardson, John

    The Solar Wind Helium Abundance: Variation with Wind Speed and the Solar Cycle Matthias R. Aellig Alamos National Lab., Los Alamos, NM 87545 Abstract We investigate the helium abundance in the solar wind of 1994 and early 2000 are analyzed. In agreement with similar work for previous solar cycles, we find

  18. The Heating & Acceleration of the Solar Wind

    E-Print Network [OSTI]

    Wurtele, Jonathan

    The Heating & Acceleration of the Solar Wind Eliot Quataert (UC Berkeley) Collaborators: Steve & Slow Winds · The Puzzle of the High Frequency Cascade (or the lack thereof ....) · Possible Solutions #12;Background · Heating required to accelerate the solar wind · Early models invoked e- conduction

  19. Photovoltaic Performance and Reliability Database: A Gateway to Experimental Data Monitoring Projects for PV at the Florida Solar Energy Center

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

    This site is the gateway to experimental data monitoring projects for photovoltaic (PV) at the Florida Solar Energy Center. The website and the database were designed to facilitate and standardize the processes for archiving, analyzing and accessing data collected from dozens of operational PV systems and test facilities monitored by FSEC's Photovoltaics and Distributed Generation Division. [copied from http://www.fsec.ucf.edu/en/research/photovoltaics/data_monitoring/index.htm

  20. Solar wind plasma correlations between IMP 8, INTERBALL-1 and WIND

    E-Print Network [OSTI]

    Richardson, John

    an important task. Clearly even if the impact on Earth's magnetosphere of a change in solar wind plasma1 21 Solar wind plasma correlations between IMP 8, INTERBALL-1 and WIND K. I. Paularena Center Short title: SOLAR WIND CORRELATIONS: IMP 8, INTERBALL, AND WIND #12;2 Abstract. Solar wind plasma ux

  1. IDENTIFYING CURRENT-SHEET–LIKE STRUCTURES IN THE SOLAR WIND

    E-Print Network [OSTI]

    Li, Gang

    2008-01-01

    Barish, F. D. 1974, in Solar Wind Three, ed. C. T. Russell (in AIP Conf. Proc. 471, Solar Wind Nine, ed. S. R. Habbal (SHEET–LIKE STRUCTURES IN THE SOLAR WIND G. Li Space Science

  2. The Structure of the Solar Wind in the Inner Heliosphere

    E-Print Network [OSTI]

    Lee, Christina On-Yee

    2010-01-01

    and allows solar wind forecasts at the ?rst Lagrange point (reliably model and forecast the global solar wind and theto some extent forecast, the solar wind structure for quiet

  3. IDENTIFYING CURRENT-SHEET–LIKE STRUCTURES IN THE SOLAR WIND

    E-Print Network [OSTI]

    Li, Gang

    2008-01-01

    Barish, F. D. 1974, in Solar Wind Three, ed. C. T. Russell (AIP Conf. Proc. 471, Solar Wind Nine, ed. S. R. Habbal (NewSTRUCTURES IN THE SOLAR WIND G. Li Space Science Laboratory,

  4. Large-scale structure of the fast solar wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; Habbal, S. Rifai; Jones, R. A.

    2007-01-01

    measurements of Solar Wind velocity, in press, Journal of1992), The Ulysses solar wind plasma experiment, AstronomyA. Hewish (1967), The solar wind outside the plane of the

  5. Expansion effects on solar wind hybrid simulations

    SciTech Connect (OSTI)

    Parashar, Tulasi N.; Velli, Marco; Goldstein, Bruce E. [NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 (United States)

    2013-06-13

    Ion kinetic simulations of the solar wind using hybrid codes can model local wave input, heating and instabilities, but generally do not include long term evolution effects in the expanding solar wind. We further develop the expanding box model used in earlier studies to include the mirror force effects and study their role in the evolution of the proton distribution functions in the outer corona and inner heliosphere. The mirror force, significant in the acceleration region of the solar wind, is required for consistency with the conservation of magnetic moment of particles in the expanding wind. We present preliminary results from the modified 1D expanding box hybrid (EBHM) simulations.

  6. NERSC Science Gateways

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

    Users Science Gateways Science Gateways About Science Gateways A science gateway is a web based interface to access HPC computers and storage systems. Gateways allow science...

  7. Solar and Wind Energy Resource Assessment Programme's Renewable...

    Open Energy Info (EERE)

    Solar and Wind Energy Resource Assessment Programme's Renewable Energy Resource Explorer Jump to: navigation, search Tool Summary LAUNCH TOOL Name: Solar and Wind Energy Resource...

  8. Solar energy system with wind vane

    DOE Patents [OSTI]

    Grip, Robert E

    2015-11-03

    A solar energy system including a pedestal defining a longitudinal axis, a frame that is supported by the pedestal and that is rotateable relative to the pedestal about the longitudinal axis, the frame including at least one solar device, and a wind vane operatively connected to the frame to urge the frame relative to the pedestal about the longitudinal axis in response to wind acting on the wind vane.

  9. How do Wind and Solar Power Affect Grid Operations: The Western Wind and Solar Integration Study; Preprint

    SciTech Connect (OSTI)

    Lew, D.; Milligan, M.; Jordan, G.; Freeman, L.; Miller, N.; Clark, K.; Piwko, R.

    2009-09-01

    This paper reviews the scope of the Western Wind and Solar Integration Study, the development of wind and solar datasets, and the results to date on three scenarios.

  10. Small Solar Wind Transients and Their Connection to the Large-Scale Coronal Structure

    E-Print Network [OSTI]

    2009-01-01

    AT SOLAR MINIMUM Small Solar Wind Transients and Theirinclude closed loops, Small Solar Wind Transients and Theirthe transient on Small Solar Wind Transients and Their

  11. The Solar Wind and Its Interaction with the Interstellar Medium

    E-Print Network [OSTI]

    Richardson, John

    The Solar Wind and Its Interaction with the Interstellar Medium John D. Richardson Abstract The solar wind is a magnetized plasma of ions and electrons which flows outward from the Sun. This chapter begins with a brief history of the discovery of the solar wind. Solar wind properties at 1 AU

  12. The solar wind in the outer heliosphere

    E-Print Network [OSTI]

    Richardson, John D.

    The solar wind evolves as it moves outward due to interactions with both itself and with the circum-heliospheric interstellar medium. The speed is, on average, constant out to 30 AU, then starts a slow decrease due to the ...

  13. Wind and Solar Energy Curtailment Practices (Presentation)

    SciTech Connect (OSTI)

    Bird, L.; Cochran, J.; Wang, X.

    2014-10-01

    This presentation to the fall 2014 technical meeting of the Utility Variable-Generation Integration Group summarizes experience with curtailment of wind and solar in the U.S.

  14. Large-scale structure of the fast solar wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; Habbal, S. Rifai; Jones, R. A.

    2007-01-01

    to detect small variations in the fast solar wind struc-small-scale (?100 km) density variations in the solar wind.small step in density seen in the Ulysses data indicated the presence of two modes of fast wind,

  15. Empirical Solar Wind Forecasting from the Chromosphere

    E-Print Network [OSTI]

    Robert J. Leamon; Scott W. McIntosh

    2007-01-12

    Recently, we correlated the inferred structure of the solar chromospheric plasma topography with solar wind velocity and composition data measured at 1AU. We now offer a physical justification of these relationships and present initial results of a empirical prediction model based on them. While still limited by the fundamentally complex physics behind the origins of the solar wind and how its structure develops in the magnetic photosphere and expands into the heliosphere, our model provides a near continuous range of solar wind speeds and composition quantities that are simply estimated from the inferred structure of the chromosphere. We suggest that the derived quantities may provide input to other, more sophisticated, prediction tools or models such as those to study Coronal Mass Ejections (CME) propagation and Solar Energetic Particle (SEP) generation.

  16. Large-scale structure of the fast solar wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; Habbal, S. Rifai; Jones, R. A.

    2007-01-01

    Scintillation measurements of Solar Wind velocity, in press,K. Sakurai (1992), The Ulysses solar wind plasma experiment,Telescope for the SOHO Mission, Solar Physics, 162, 291–312.

  17. Solar Wind Forecasting with Coronal Holes

    E-Print Network [OSTI]

    S. Robbins; C. J. Henney; J. W. Harvey

    2007-01-09

    An empirical model for forecasting solar wind speed related geomagnetic events is presented here. The model is based on the estimated location and size of solar coronal holes. This method differs from models that are based on photospheric magnetograms (e.g., Wang-Sheeley model) to estimate the open field line configuration. Rather than requiring the use of a full magnetic synoptic map, the method presented here can be used to forecast solar wind velocities and magnetic polarity from a single coronal hole image, along with a single magnetic full-disk image. The coronal hole parameters used in this study are estimated with Kitt Peak Vacuum Telescope He I 1083 nm spectrograms and photospheric magnetograms. Solar wind and coronal hole data for the period between May 1992 and September 2003 are investigated. The new model is found to be accurate to within 10% of observed solar wind measurements for its best one-month periods, and it has a linear correlation coefficient of ~0.38 for the full 11 years studied. Using a single estimated coronal hole map, the model can forecast the Earth directed solar wind velocity up to 8.5 days in advance. In addition, this method can be used with any source of coronal hole area and location data.

  18. Turbulent density fluctuations in the solar wind

    E-Print Network [OSTI]

    Ingale, Madhusudan

    2015-01-01

    Treatments of the radio scattering due to density turbulence in the solar wind typically employ asymptotic approximations to the phase structure function. We use a general structure function (GSF) that straddles the asymptotic limits and quantify the relative error introduced by the approximations. We show that the regimes where GSF predictions are accurate than those of its asymptotic approximations is not only of practical relevance, but are where inner scale effects influence the estimate of the scatter-broadening. Thus we propose that GSF should henceforth be used for scatter broadening calculations and estimates of quantities characterizing density turbulence in the solar corona and solar wind. In the next part of this thesis we use measurements of density turbulence in the solar wind from previously publish observations of radio wave scattering and interplanetary scintillations. Density fluctuations are inferred using the GSF for radio scattering data and existing analysis methods for IPS. Assuming that...

  19. 15/06/2005 Solar Wind 11/SOHO 16 1 Radial Dependence of Solar

    E-Print Network [OSTI]

    Kallenrode, May-Britt

    small solar events Invariant spectra Hucke et al., 1992, Solar Phys. 142, 143 #12;15/06/2005 Solar Wind15/06/2005 Solar Wind 11/SOHO 16 1 Radial Dependence of Solar Energetic Particle Events M.-B. Kallenrode #12;15/06/2005 Solar Wind 11/SOHO 16 2 Outline No discussion about composition and charge states

  20. Energy Transfer via Solar Wind Driven Ultra Low Frequency Waves in the Earth's Magnetosphere

    E-Print Network [OSTI]

    Hartinger, Michael David

    2012-01-01

    Modeling energy transfer via solar wind driven ULFthrough which solar wind energy can drive wave activity. Inthrough which solar wind energy can drive wave activity. In

  1. Laboratory Facility for Simulating Solar Wind Sails

    SciTech Connect (OSTI)

    Funaki, Ikkoh [Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, 229-8510 (Japan); JST/CREST, Kawaguchi, Saitama, 332-0012 (Japan); Ueno, Kazuma; Oshio, Yuya [Graduate University for Advanced Studies, Sagamihara, Kanagawa, 229-8510 (Japan); Ayabe, Tomohiro; Horisawa, Hideyuki [Tokai University, Hiratsuka, Kanagawa, 259-1292 (Japan); Yamakawa, Hiroshi [Kyoto University, Uji, Kyoto, 611-0011 (Japan); JST/CREST, Kawaguchi, Saitama, 332-0012 (Japan)

    2008-12-31

    Magnetic sail (MagSail) is a deep space propulsion system, in which an artificial magnetic cavity captures the energy of the solar wind to propel a spacecraft in the direction leaving the sun. For a scale-model experiment of the plasma flow of MagSail, we employed a magnetoplasmadynamic arcjet as a solar wind simulator. It is observed that a plasma flow from the solar wind simulator reaches a quasi-steady state of about 0.8 ms duration after a transient phase when initiating the discharge. During this initial phase of the discharge, a blast-wave was observed to develop radially in a vacuum chamber. When a solenoidal coil (MagSail scale model) is immersed into the quasi-steady flow where the velocity is 45 km/s, and the number density is 10{sup 19} m-3, a bow shock as well as a magnetic cavity were formed in front of the coil. As a result of the interaction between the plasma flow and the magnetic cavity, the momentum of the simulated solar wind is decreased, and it is found from the thrust measurement that the solar wind momentum is transferred to the coil simulating MagSail.

  2. Wind Issues in Solar Thermal Performance Ratings: Preprint

    SciTech Connect (OSTI)

    Burch, J.; Casey, R.

    2009-04-01

    We suggest that wind bias against unglazed solar water heaters be mitigated by using a calibrated collector model to derive a wind correction to the measured efficiency curve.

  3. Energy dissipation processes in solar wind turbulence

    E-Print Network [OSTI]

    Wang, Y; Feng, X S; Xu, X J; Zhang, J; Sun, T R; Zuo, P B

    2015-01-01

    Turbulence is a chaotic flow regime filled by irregular flows. The dissipation of turbulence is a fundamental problem in the realm of physics. Theoretically, dissipation cannot be ultimately achieved without collisions, and so how turbulent kinetic energy is dissipated in the nearly collisionless solar wind is a challenging problem. Wave particle interactions and magnetic reconnection are two possible dissipation mechanisms, but which mechanism dominates is still a controversial topic. Here we analyze the dissipation region scaling around a solar wind magnetic reconnection region. We find that the magnetic reconnection region shows a unique multifractal scaling in the dissipation range, while the ambient solar wind turbulence reveals a monofractal dissipation process for most of the time. These results provide the first observational evidences for the intermittent multifractal dissipation region scaling around a magnetic reconnection site, and they also have significant implications for the fundamental energy...

  4. Solar and Wind Technologies for Hydrogen Production Report to Congress

    Fuel Cell Technologies Publication and Product Library (EERE)

    DOE's Solar and Wind Technologies for Hydrogen Production Report to Congress summarizes the technology roadmaps for solar- and wind-based hydrogen production. Published in December 2005, it fulfills t

  5. Solar and Wind Contractor Licensing

    Broader source: Energy.gov [DOE]

    In June of 2014, SB 447 mandated that the Louisiana State Licencsing Board for Contractors develop new rules for solar contractors no later than January 1, 2015. Licensed contractors must be in c...

  6. Identifying Wind and Solar Ramping Events: Preprint

    SciTech Connect (OSTI)

    Florita, A.; Hodge, B. M.; Orwig, K.

    2013-01-01

    Wind and solar power are playing an increasing role in the electrical grid, but their inherent power variability can augment uncertainties in power system operations. One solution to help mitigate the impacts and provide more flexibility is enhanced wind and solar power forecasting; however, its relative utility is also uncertain. Within the variability of solar and wind power, repercussions from large ramping events are of primary concern. At the same time, there is no clear definition of what constitutes a ramping event, with various criteria used in different operational areas. Here the Swinging Door Algorithm, originally used for data compression in trend logging, is applied to identify variable generation ramping events from historic operational data. The identification of ramps in a simple and automated fashion is a critical task that feeds into a larger work of 1) defining novel metrics for wind and solar power forecasting that attempt to capture the true impact of forecast errors on system operations and economics, and 2) informing various power system models in a data-driven manner for superior exploratory simulation research. Both allow inference on sensitivities and meaningful correlations, as well as the ability to quantify the value of probabilistic approaches for future use in practice.

  7. SUBMITTED TO GRL 1 Thermal Anisotropies in the Solar Wind

    E-Print Network [OSTI]

    Richardson, John

    SUBMITTED TO GRL 1 E Thermal Anisotropies in the Solar Wind: vidence of Heating by Interstellar cyclotron instabilit s generated by newly created pickup ions and heats the thermal solar wind protons TO GRL 2 T Introduction he thermal anisotropy of the solar wind is the ratio between the temperatures p

  8. Solar and wind power advancing

    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 RoomPreservation ofAlbuquerque|Sensitive Species3performedValley |Solar PowerofThermalSolar and

  9. The Genesis Mission: Solar Wind Conditions, and Implications for the FIP Fractionation of the Solar Wind.

    SciTech Connect (OSTI)

    Reisenfeld, D. B.; Wiens, R. C.; Barraclough, B. L.; Steinberg, J. T; Dekoning, C. A.; Zurbuchen, T. H.; Burnett, D. S.

    2005-01-01

    The NASA Genesis mission collected solar wind on ultrapure materials between November 30, 2001 and April 1, 2004. The samples were returned to Earth September 8, 2004. Despite the hard landing that resulted from a failure of the avionics to deploy the parachute, many samples were returned in a condition that will permit analyses. Sample analyses of these samples should give a far better understanding of the solar elemental and isotopic composition (Burnett et al. 2003). Further, the photospheric composition is thought to be representative of the solar nebula, so that the Genesis mission will provide a new baseline for the average solar nebula composition with which to compare present-day compositions of planets, meteorites, and asteroids. Sample analysis is currently underway. The Genesis samples must be placed in the context of the solar and solar wind conditions under which they were collected. Solar wind is fractionated from the photosphere by the forces that accelerate the ions off of the Sun. This fractionation appears to be ordered by the first ionization potential (FIP) of the elements, with the tendency for low-FIP elements to be over-abundant in the solar wind relative to the photosphere, and high-FIP elements to be under-abundant (e.g. Geiss, 1982; von Steiger et al., 2000). In addition, the extent of elemental fractionation differs across different solarwind regimes. Therefore, Genesis collected solar wind samples sorted into three regimes: 'fast wind' or 'coronal hole' (CH), 'slow wind' or 'interstream' (IS), and 'coronal mass ejection' (CME). To carry this out, plasma ion and electron spectrometers (Barraclough et al., 2003) continuously monitored the solar wind proton density, velocity, temperature, the alpha/proton ratio, and angular distribution of suprathermal electrons, and those parameters were in turn used in a rule-based algorithm that assigned the most probable solar wind regime (Neugebauer et al., 2003). At any given time, only one of three regime-specific collectors (CH, IS, or CME) was exposed to the solar wind. Here we report on the regime-specific solar wind conditions from in-situ instruments over the course of the collection period. Further, we use composition data from the SWICS (Solar Wind Ion Composition Spectrometer) instrument on ACE (McComas et al., 1998) to examine the FIP fractionation between solar wind regimes, and make a preliminary comparison of these to the FIP analysis of Ulysses/SWICS composition data (von Steiger et al. 2000). Our elemental fractionation study includes a reevaluation of the Ulysses FIP analysis in light of newly reported photospheric abundance data (Asplund, Grevesse & Sauval, 2005). The new abundance data indicate a metallicity (Z/X) for the Sun almost a factor of two lower than that reported in the widely used compilation of Anders & Grevesse (1989). The new photospheric abundances suggest a lower degree of solar wind fractionation than previously reported by von Steiger et al. (2000) for the first Ulysses polar orbit (1991-1998).

  10. IDENTIFYING CURRENT-SHEET–LIKE STRUCTURES IN THE SOLAR WIND

    E-Print Network [OSTI]

    Li, Gang

    2008-01-01

    Ulysses for two periods, one in solar maximum and the otherstructures in solar wind turbulence are one-dimensionalone can infer the existence of current sheets in the solar

  11. Solar 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 E LIST OFAMERICA'SHeavyAgencyTendo New Energy Equipment Co LtdSimranSkykonAllianceWind

  12. Lognormal distributions and spectra of solar wind plasma fluctuations: Wind 19951998

    E-Print Network [OSTI]

    Richardson, John

    Lognormal distributions and spectra of solar wind plasma fluctuations: Wind 1995­1998 L. F. Burlaga, and T were double-peaked; nevertheless, the number of observations associated with the fast wind distribution with large tails. There remains a need for dynamical models of the solar wind that incorporate and describe

  13. Wind/SWE observations of firehose constraint on solar wind proton temperature anisotropy

    E-Print Network [OSTI]

    Richardson, John

    Wind/SWE observations of firehose constraint on solar wind proton temperature anisotropy Justin C the Wind spacecraft are reported here. These measurements show for the first time with a comprehensive plasma and magnetic field data set that this constraint is statistically satisfied in the solar wind near

  14. Denver Solar and 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 ECoopButtePower VenturesInformation9) WindGridDeepiSolar and Wind Jump to:

  15. The Solar Wind in the Outer Heliosphere at Solar John D. Richardson and Chi Wang

    E-Print Network [OSTI]

    Richardson, John

    The Solar Wind in the Outer Heliosphere at Solar Maximum John D. Richardson and Chi Wang Center solar wind observations in the outer heliosphere, concentrating on the recent data near solar maximum. The speed and temperature tend to be lower at solar maximum, due to the lack of coronal holes. The near

  16. ELECTRON PROPERTIES AND COULOMB COLLISIONS IN THE SOLAR WIND AT 1 AU: WIND OBSERVATIONS

    E-Print Network [OSTI]

    California at Berkeley, University of

    headings: methods: data analysis -- plasmas -- solar wind 1. INTRODUCTION One of the major issues of solar, the electrons play an important role in the solar wind expansion and the associated energy transport since of the energy sources that drives the expansion of the solar corona (Hundhausen 1972; Feldman et al. 1975

  17. Western Wind and Solar Integration Study (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2012-09-01

    Initiated in 2007 to examine the operational impact of up to 35% penetration of wind, photovoltaic (PV), and concentrating solar power (CSP) energy on the electric power system, the Western Wind and Solar Integration Study (WWSIS) is one of the largest regional wind and solar integration studies to date. The goal is to understand the effects of variability and uncertainty of wind, PV, and CSP on the grid. In the Western Wind and Solar Integration Study Phase 1, solar penetration was limited to 5%. Utility-scale PV was not included because of limited capability to model sub-hourly, utility-scale PV output . New techniques allow the Western Wind and Solar Integration Study Phase 2 to include high penetrations of solar - not only CSP and rooftop PV but also utility-scale PV plants.

  18. The Solar Wind, CMEs and the Origins of Heliospheric Activity

    E-Print Network [OSTI]

    release o Coronal holes o Source of high-speed solar wind #12;peter.gallagher@tcd.ie #12;#12;peter Parker => Parker Spiral: r - r0 = -(v/ )( - 0) o Winding angle: o Inclined at ~45º at 1 AU and ~90º by 10The Solar Wind, CMEs and the Origins of Heliospheric Activity Peter T. Gallagher School of Physics

  19. Turbulent heating of the corona and solar wind: the heliospheric

    E-Print Network [OSTI]

    Turbulent heating of the corona and solar wind: the heliospheric dark energy problem Stuart D. Bale that the gas is highly ionized, i.e. a magnetized collisionless plasma ( wind model A `solar wind' is accelerated from the corona - Hydrostatic solution (similar to Bondi accretion

  20. Oxygen Loss from Venus and the Influence of Extreme Solar Wind Conditions

    E-Print Network [OSTI]

    McEnulty, Tess

    2012-01-01

    W. C. Feldman (1978), Solar wind stream interfaces, Journal2008a), Evolution of solar wind structures from 0.72 to 123/24 with Historical Solar Wind Records at 1 AU, Solar

  1. Organization of Energetic Particles by the Solar Wind Structure During the Declining to Minimum Phase of Solar Cycle 23

    E-Print Network [OSTI]

    2010-01-01

    Feldman, W.C. : 1978, Solar wind stream interfaces. J.of large-scale solar wind structures. Ph.D. dissertation,R.M. : 2008, Weaker solar wind from the polar coronal holes

  2. ISOTOPIC MASS FRACTIONATION OF SOLAR WIND: EVIDENCE FROM FAST AND SLOW SOLAR WIND COLLECTED BY THE GENESIS MISSION

    SciTech Connect (OSTI)

    Heber, Veronika S.; Baur, Heinrich; Wieler, Rainer; Bochsler, Peter; McKeegan, Kevin D.; Neugebauer, Marcia; Reisenfeld, Daniel B.; Wiens, Roger C.

    2012-11-10

    NASA's Genesis space mission returned samples of solar wind collected over {approx}2.3 years. We present elemental and isotopic compositions of He, Ne, and Ar analyzed in diamond-like carbon targets from the slow and fast solar wind collectors to investigate isotopic fractionation processes during solar wind formation. The solar wind provides information on the isotopic composition for most volatile elements for the solar atmosphere, the bulk Sun and hence, on the solar nebula from which it formed 4.6 Ga ago. Our data reveal a heavy isotope depletion in the slow solar wind compared to the fast wind composition by 63.1 {+-} 2.1 per mille for He, 4.2 {+-} 0.5 per mille amu{sup -1} for Ne and 2.6 {+-} 0.5 per mille amu{sup -1} for Ar. The three Ne isotopes suggest that isotopic fractionation processes between fast and slow solar wind are mass dependent. The He/H ratios of the collected slow and fast solar wind samples are 0.0344 and 0.0406, respectively. The inefficient Coulomb drag model reproduces the measured isotopic fractionation between fast and slow wind. Therefore, we apply this model to infer the photospheric isotopic composition of He, Ne, and Ar from our solar wind data. We also compare the isotopic composition of oxygen and nitrogen measured in the solar wind with values of early solar system condensates, probably representing solar nebula composition. We interpret the differences between these samples as being due to isotopic fractionation during solar wind formation. For both elements, the magnitude and sign of the observed differences are in good agreement with the values predicted by the inefficient Coulomb drag model.

  3. Solar wind electron temperature and density measurements on the Solar Orbiter with thermal noise spectroscopy

    E-Print Network [OSTI]

    California at Berkeley, University of

    for the Solar Orbiter mission. One can already figure out what could be the Te gra- dients in this radial rangeSolar wind electron temperature and density measurements on the Solar Orbiter with thermal noise Abstract The measurement of the solar wind electron temperature in the unexplored region between 1 and 45

  4. Development of Multidimensional MHD Model for the Solar Corona and Solar Wind

    E-Print Network [OSTI]

    California at Berkeley, University of

    self-consistent 2D MHD model of the solar corona and solar wind that explicitly solves the energy models assume polytropic energy equations, or an ad-hoc heating function. Chen & Hu (2001) includedDevelopment of Multidimensional MHD Model for the Solar Corona and Solar Wind E. C. Sittler Jr.1

  5. Clark County- Solar and Wind Building Permit Guides

    Broader source: Energy.gov [DOE]

    Clark County, Nevada has established guides for obtaining building permits for wind and solar photovoltaic (PV) systems for both residential and commercial purposes. The guides outline applicable...

  6. Large-Distributed Solar and Wind Grant Program

    Broader source: Energy.gov [DOE]

    The Illinois Department of Commerce and Economic Opportunity (DCEO) is offering grants for community-scale solar and wind projects located in Illinois.

  7. On the response of polar cap dynamics to its solar wind and magnetotail drivers at high levels of geomagnetic activity

    E-Print Network [OSTI]

    Gao, Ye

    2012-01-01

    nearly universal solar wind-magnetosphere coupling functionits controlling factors in solar wind and magnetotail, J.on its controlling factors in solar wind and magnetotail, J.

  8. On the response of polar cap dynamics to its solar wind and magnetotail drivers at high levels of geomagnetic activity

    E-Print Network [OSTI]

    Gao, Ye

    2012-01-01

    of polar cap potential by intense solar wind electricelectric potential as a function of solar wind parameters bypolar cap potential increases linearly with the solar wind

  9. Atlantic Wind Solar Inc | 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 JEnvironmental Jump to:EAandAmminex A SOpenAshley, Ohio:Atchison-HoltAtlantaBiomassEnergyWind Solar

  10. Solar Wind: Manifestations of Solar Activity E N CYC LO PE D IA O F AS T R O N O MY AN D AS T R O PHYS I C S Solar Wind: Manifestations of Solar

    E-Print Network [OSTI]

    Webb, David F.

    Solar Wind: Manifestations of Solar Activity E N CYC LO PE D IA O F AS T R O N O MY AN D AS T R O PHYS I C S Solar Wind: Manifestations of Solar Activity The Sun's outer atmosphere, the corona, is continually heated and expands to create the solar wind. Solar activity waxes and wanes with the 11 yr cycle

  11. ELECTRON TRANSPORT IN THE FAST SOLAR WIND

    SciTech Connect (OSTI)

    Smith, H. M.; Marsch, E. [Max-Planck-Institut fuer Sonnensystemforschung, Max-Planck-Strasse 2, 37191 Katlenburg-Lindau (Germany); Helander, P., E-mail: hakan.smith@ipp.mpg.de [Max-Planck-Institut fuer Plasmaphysik, Wendelsteinstrasse 1, 17491 Greifswald (Germany)

    2012-07-01

    The electron velocity distribution function is studied in the extended solar corona above coronal holes (i.e., the inner part of the fast solar wind) from the highly collisional corona close to the Sun to the weakly collisional regions farther out. The electron kinetic equation is solved with a finite-element method in velocity space using a linearized Fokker-Planck collision operator. The ion density and temperature profiles are assumed to be known and the electric field and electron temperature are determined self-consistently. The results show quantitatively how much lower the electron heat flux and the thermal force are than predicted by high-collisionality theory. The sensitivity of the particle and heat fluxes to the assumed ion temperature profile and the applied boundary condition at the boundary far from the Sun is also studied.

  12. Solar and Wind Easements & Rights Laws & Local Option Solar Rights...

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

    Schools State Government Federal Government Agricultural Institutional Savings Category Solar - Passive Solar Water Heat Solar Space Heat Solar Thermal Electric Solar Thermal...

  13. ON THE ORIGIN OF MID-LATITUDE FAST WIND: CHALLENGING THE TWO-STATE SOLAR WIND PARADIGM

    E-Print Network [OSTI]

    Stakhiv, Mark

    The bimodal paradigm of solar wind describes a slow solar wind situated near the heliospheric current sheet while a fast wind overexpands from the poles to fill in the remainder of the heliosphere. In this paper, we challenge ...

  14. Small Solar Wind Transients and Their Connection to the Large-Scale Coronal Structure

    E-Print Network [OSTI]

    2009-01-01

    I.G. : 2006, In situ solar wind and magnetic ?eld signaturesE. : 2008, The IMPACT Solar Wind Electron Analyzer (SWEA).Heliospheric images of the solar wind at Earth. Astrophys.

  15. Interplanetary Scintillation Observations of Stream Interaction Regions in the Solar Wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; O’Neill, I. J.

    2010-01-01

    Measurements of the solar wind velocity with EISCAT. Astron.measurements of the solar wind. Ann. Geophys. 14, 1235.regions in the solar wind. Adv. Space Res. Breen, A.R. ,

  16. Comment on "Air Emissions Due to Wind and Solar Power" and Supporting Information

    E-Print Network [OSTI]

    Mills, Andrew D.

    2011-01-01

    due to wind and solar power. Environ. Sci. Technol. (2)Emissions Due to Wind and Solar Power” Andrew Mills, ? , †due to wind and solar power. Environ. Sci. Technol. (2)

  17. Solar wind-magnetosphere coupling leading to relativistic electron energization during high-speed streams

    E-Print Network [OSTI]

    Lyons, Larry

    Solar wind-magnetosphere coupling leading to relativistic electron energization during high. Smith (2005), Solar wind-magnetosphere coupling leading to relativistic electron energization during. Using observations during a period of persistent high-speed, corotating, solar wind streams, we

  18. Solar wind driving of magnetospheric ULF waves: Field line resonances driven by dynamic pressure fluctuations

    E-Print Network [OSTI]

    Solar wind driving of magnetospheric ULF waves: Field line resonances driven by dynamic pressure observational studies suggest that solar wind dynamic pressure fluctuations can drive magnetosphericFedderMobarry (LFM) global, threedimensional magnetohydrodynamic (MHD) simulations of the solar wind

  19. A Multispacecraft Analysis of a Small-Scale Transient Entrained by Solar Wind Streams

    E-Print Network [OSTI]

    2009-01-01

    panels show IMPACT observations of solar wind proton speed (Entrained by Solar Wind Streams Figure 8 PLASTIC and IMPACTIMPACT package, are used in the present study. Near-Earth solar wind

  20. Dust Detection by the Wave Instrument on STEREO: Nanoparticles Picked up by the Solar Wind?

    E-Print Network [OSTI]

    2009-01-01

    the solar wind at 1 AU were produced by impacts of micron-solar wind during the Jupiter ?y-by, which are consistent with impactsimpacts and thus shows the ubiquitous plasma quasi-thermal noise in the solar wind,

  1. Dust Detection by the Wave Instrument on STEREO: Nanoparticles Picked up by the Solar Wind?

    E-Print Network [OSTI]

    2009-01-01

    2007, Basics of the Solar Wind, Cambridge University Press,Picked up by the Solar Wind? N. Meyer-Vernet · M. Maksimovicof magnitude of the solar wind speed. Nanoparticles, which

  2. Energetic neutral atom response to solar wind dynamic pressure enhancements

    E-Print Network [OSTI]

    Lyons, Larry

    Energetic neutral atom response to solar wind dynamic pressure enhancements D.-Y. Lee,1 S. Ohtani,2; published 11 September 2007. [1] We have investigated the response of the ring current to solar wind dynamic adiabatically energized by the compression. The increased ENA emission rate drops as Pdyn decreases, implying

  3. Solar and Wind Technologies for Hydrogen Production Report to Congress

    SciTech Connect (OSTI)

    None, None

    2005-12-01

    DOE's Solar and Wind Technologies for Hydrogen Production Report to Congress summarizes the technology roadmaps for solar- and wind-based hydrogen production. Published in December 2005, it fulfills the requirement under section 812 of the Energy Policy Act of 2005.

  4. Mirror Mode Structures in the Solar Wind: STEREO Observations

    E-Print Network [OSTI]

    California at Berkeley, University of

    Mirror Mode Structures in the Solar Wind: STEREO Observations O. Enríquez-Rivera1 , X. Blanco-Cano1 Autónoma de México, Coyoacán, D.F., 04510, MEXICO 2. Institute of Geophysics and Planetary Physics of California, Berkeley, CA 94720, USA Abstract. Mirror mode structures occur in the solar wind either

  5. Western Wind and Solar Integration Study Phase 3: Technical Overview

    SciTech Connect (OSTI)

    2015-11-01

    Technical fact sheet outlining the key findings of Phase 3 of the Western Wind and Solar Integration Study (WWSIS-3). NREL and GE find that with good system planning, sound engineering practices, and commercially available technologies, the Western grid can maintain reliability and stability during the crucial first minute after grid disturbances with high penetrations of wind and solar power.

  6. The Western Wind and Solar Integration Study Phase 2

    SciTech Connect (OSTI)

    Lew, Debra; Brinkman, Greg; Ibanez, E.; Florita, A.; Heaney, M.; Hodge, B. -M.; Hummon, M.; Stark, G.; King, J.; Lefton, S. A.; Kumar, N.; Agan, D.; Jordan, G.; Venkataraman, S.

    2013-09-01

    The electric grid is a highly complex, interconnected machine, and changing one part of the grid can have consequences elsewhere. Adding wind and solar affects the operation of the other power plants and adding high penetrations can induce cycling of fossil-fueled generators. Cycling leads to wear-and-tear costs and changes in emissions. Phase 2 of the Western Wind and Solar Integration Study (WWSIS-2) evaluated these costs and emissions and simulated grid operations for a year to investigate the detailed impact of wind and solar on the fossil-fueled fleet. This built on Phase 1, one of the largest wind and solar integration studies ever conducted, which examined operational impacts of high wind and solar penetrations in the West(GE Energy 2010).

  7. The Western Wind and Solar Integration Study Phase 2

    SciTech Connect (OSTI)

    Lew, D.; Brinkman, G.; Ibanez, E.; Hodge, B. M.; Hummon, M.; Florita, A.; Heaney, M.

    2013-09-01

    The electric grid is a highly complex, interconnected machine, and changing one part of the grid can have consequences elsewhere. Adding wind and solar affects the operation of the other power plants and adding high penetrations can induce cycling of fossil-fueled generators. Cycling leads to wear-and-tear costs and changes in emissions. Phase 2 of the Western Wind and Solar Integration Study (WWSIS-2) evaluated these costs and emissions and simulated grid operations for a year to investigate the detailed impact of wind and solar on the fossil-fueled fleet. This built on Phase 1, one of the largest wind and solar integration studies ever conducted, which examined operational impacts of high wind and solar penetrations in the West.

  8. OBSERVATION OF FLUX-TUBE CROSSINGS IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Arnold, L.; Li, G.; Li, X.; Yan, Y.

    2013-03-20

    Current sheets are ubiquitous in the solar wind. They are a major source of the solar wind MHD turbulence intermittency. They may result from nonlinear interactions of the solar wind MHD turbulence or are the boundaries of flux tubes that originate from the solar surface. Some current sheets appear in pairs and are the boundaries of transient structures such as magnetic holes and reconnection exhausts or the edges of pulsed Alfven waves. For an individual current sheet, discerning whether it is a flux-tube boundary or due to nonlinear interactions or the boundary of a transient structure is difficult. In this work, using data from the Wind spacecraft, we identify two three-current-sheet events. Detailed examination of these two events suggests that they are best explained by the flux-tube-crossing scenario. Our study provides convincing evidence supporting the scenario that the solar wind consists of flux tubes where distinct plasmas reside.

  9. Solar energetic particle events in different types of solar wind

    SciTech Connect (OSTI)

    Kahler, S. W.; Vourlidas, A.

    2014-08-10

    We examine statistically some properties of 96 20 MeV gradual solar energetic proton (SEP) events as a function of three different types of solar wind (SW) as classified by Richardson and Cane. Gradual SEP (E > 10 MeV) events are produced in shocks driven by fast (V ? 900 km s{sup –1}) and wide (W > 60°) coronal mass ejections (CMEs). We find no differences among the transient, fast, and slow SW streams for SEP 20 MeV proton event timescales. It has recently been found that the peak intensities Ip of these SEP events scale with the ?2 MeV proton background intensities, which may be a proxy for the near-Sun shock seed particles. Both the intensities Ip and their 2 MeV backgrounds are significantly enhanced in transient SW compared to those of fast and slow SW streams, and the values of Ip normalized to the 2 MeV backgrounds only weakly correlate with CME V for all SW types. This result implies that forecasts of SEP events could be improved by monitoring both the Sun and the local SW stream properties and that the well known power-law size distributions of Ip may differ between transient and long-lived SW streams. We interpret an observed correlation between CME V and the 2 MeV background for SEP events in transient SW as a manifestation of enhanced solar activity.

  10. Comment on "Air Emissions Due to Wind and Solar Power" and Supporting Information

    E-Print Network [OSTI]

    Mills, Andrew D.

    2011-01-01

    and Renewable Energy (Wind & Hy- dropower Technologiesand Renewable Energy (Wind & Hy- dropower Technologies7) GE Energy Consulting, Western Wind & Solar Integration

  11. ASYMMETRIC ELECTRON DISTRIBUTIONS IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Rha, Kicheol; Ryu, Chang-Mo [Department of Physics, Pohang University of Science and Technology, Pohang 790-784 (Korea, Republic of)] [Department of Physics, Pohang University of Science and Technology, Pohang 790-784 (Korea, Republic of); Yoon, Peter H. [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742 (United States)] [Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742 (United States)

    2013-09-20

    A plausible mechanism responsible for producing asymmetric electron velocity distribution functions in the solar wind is investigated by means of one-dimensional electrostatic particle-in-cell (PIC) simulation. A recent paper suggests that the variation in the ion-to-electron temperature ratio influences the nonlinear wave-particle dynamics such that it results in the formation of asymmetric distributions. The present PIC code simulation largely confirms this finding, but quantitative differences between the weak turbulence formalism and the present PIC simulation are also found, suggesting the limitation of the analytical method. The inter-relationship between the asymmetric electron distribution and the ion-to-electron temperature ratio may be a new useful concept for the observation.

  12. RELAXATION PROCESSES IN SOLAR WIND TURBULENCE

    SciTech Connect (OSTI)

    Servidio, S.; Carbone, V.; Gurgiolo, C.; Goldstein, M. L.

    2014-07-10

    Based on global conservation principles, magnetohydrodynamic (MHD) relaxation theory predicts the existence of several equilibria, such as the Taylor state or global dynamic alignment. These states are generally viewed as very long-time and large-scale equilibria, which emerge only after the termination of the turbulent cascade. As suggested by hydrodynamics and by recent MHD numerical simulations, relaxation processes can occur during the turbulent cascade that will manifest themselves as local patches of equilibrium-like configurations. Using multi-spacecraft analysis techniques in conjunction with Cluster data, we compute the current density and flow vorticity and for the first time demonstrate that these localized relaxation events are observed in the solar wind. Such events have important consequences for the statistics of plasma turbulence.

  13. Innovations in Wind and Solar PV Financing

    SciTech Connect (OSTI)

    Cory, K.; Coughlin, J.; Jenkin, T.; Pater, J.; Swezey, B.

    2008-02-01

    There is growing national interest in renewable energy development based on the economic, environmental, and security benefits that these resources provide. Historically, greater development of our domestic renewable energy resources has faced a number of hurdles, primarily related to cost, regulation, and financing. With the recent sustained increase in the costs and associated volatility of fossil fuels, the economics of renewable energy technologies have become increasingly attractive to investors, both large and small. As a result, new entrants are investing in renewable energy and new business models are emerging. This study surveys some of the current issues related to wind and solar photovoltaic (PV) energy project financing in the electric power industry, and identifies both barriers to and opportunities for increased investment.

  14. COMPOSITION OF THE SOLAR CORONA, SOLAR WIND, AND SOLAR ENERGETIC PARTICLES

    SciTech Connect (OSTI)

    Schmelz, J. T.; Reames, D. V.; Von Steiger, R.; Basu, S.

    2012-08-10

    Along with temperature and density, the elemental abundance is a basic parameter required by astronomers to understand and model any physical system. The abundances of the solar corona are known to differ from those of the solar photosphere via a mechanism related to the first ionization potential of the element, but the normalization of these values with respect to hydrogen is challenging. Here, we show that the values used by solar physicists for over a decade and currently referred to as the 'coronal abundances' do not agree with the data themselves. As a result, recent analysis and interpretation of solar data involving coronal abundances may need to be revised. We use observations from coronal spectroscopy, the solar wind, and solar energetic particles as well as the latest abundances of the solar photosphere to establish a new set of abundances that reflect our current understanding of the coronal plasma.

  15. Residual Energy Spectrum of Solar Wind Turbulence

    E-Print Network [OSTI]

    Chen, C H K; Salem, C S; Maruca, B A

    2013-01-01

    It has long been known that the energy in velocity and magnetic field fluctuations in the solar wind is not in equipartition. In this paper, we present an analysis of 5 years of Wind data at 1 AU to investigate the reason for this. The residual energy (difference between energy in velocity and magnetic field fluctuations) was calculated using both the standard magnetohydrodynamic (MHD) normalization for the magnetic field and a kinetic version, which includes temperature anisotropies and drifts between particle species. It was found that with the kinetic normalization, the fluctuations are closer to equipartition, with a mean normalized residual energy of sigma_r = -0.19 and mean Alfven ratio of r_A = 0.71. The spectrum of residual energy, in the kinetic normalization, was found to be steeper than both the velocity and magnetic field spectra, consistent with some recent MHD turbulence predictions and numerical simulations, having a spectral index close to -1.9. The local properties of residual energy and cros...

  16. Gateway Design for Data Gathering Sensor Raluca Musaloiu-E.

    E-Print Network [OSTI]

    Amir, Yair

    such a gateway requires special energy sources, such as rechargeable batteries coupled with solar panels@cs.jhu.edu Abstract--Innovation in gateways for data gathering sensor networks has lagged compared to advances in mote investigate mechanisms to minimize energy consumption at the gateway including completely powering it off

  17. Science Gateways

    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 RoomPreservation ofAlbuquerque| Stanford SynchrotronVideo-Contest December 17, 2015Gateways

  18. Impact of increased penetration of wind and PV solar resources on the

    E-Print Network [OSTI]

    Stoltz, Brian M.

    Impact of increased penetration of wind and PV solar resources on the bulk power system Vijay;Wind and PV solar grid interface · Modern wind turbine generators are typically rated between 1.5 MW through a power electronic converter 3 #12;Wind and PV solar grid interface 4 Schematic of Type 3 wind

  19. Solar Wind Turbulence A Study of Corotating Interaction Regions at 1 AU

    E-Print Network [OSTI]

    Solar Wind Turbulence A Study of Corotating Interaction Regions at 1 AU Je rey A. Tessein Department of Physics University of New Hampshire Durham, NH 03824 May 15, 2009 #12;Abstract The solar wind's rotation and the variability in the source of the solar wind, fast moving wind can crash into slow wind

  20. Solar Wind Sources in the Late Declining Phase of Cycle 23: Effects of the Weak Solar Polar Field on High Speed Streams

    E-Print Network [OSTI]

    2009-01-01

    Isenberg, P.A. (eds. ) Solar Wind Nine, AIP Conf. Proc. 471,AT SOLAR MINIMUM Solar Wind Sources in the Late Decliningfor their high speed solar wind streams that dominate the

  1. Altered solar wind -magnetosphere interaction at low Mach numbers: coronal mass ejections

    E-Print Network [OSTI]

    Boyer, Edmond

    1 Altered solar wind - magnetosphere interaction at low Mach numbers: coronal mass ejections Benoit fundamental alterations of the solar wind ­ magnetosphere interaction that occur during low Mach number solar wind. We first show that low Mach number solar wind conditions are often characteristic of coronal mass

  2. Narrow coronal holes in Yohkoh soft X-ray images and the slow solar wind

    E-Print Network [OSTI]

    California at Berkeley, University of

    Narrow coronal holes in Yohkoh soft X-ray images and the slow solar wind C.N. Arge , K.L. Harvey of this phenomenon, and have found several candidates. From observations of the associated solar wind, and from modeling, we find these regions to be sources of slow solar wind. INTRODUCTION The solar wind arguably

  3. 10 Questions for a Wind & Solar Integration Analyst: Kirsten Orwig

    Broader source: Energy.gov [DOE]

    Kirsten Orwig shares how her experiences in storm chasing led her to this position at National Renewable Energy Laboratory (NREL) and why understanding meteorology is important for advancing reliable solar and wind energy.

  4. Wind and Solar Energy Curtailment: Experience and Practices in...

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

    Wind and Solar Energy Curtailment: Experience and Practices in the United States Lori Bird, Jaquelin Cochran, and Xi Wang Technical Report NRELTP-6A20-60983 March 2014 NREL is a...

  5. Western Wind and Solar Integration Study Phase 2 (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2013-09-01

    This is one-page, two-sided fact sheet presents high-level summary results of the Western Wind and Solar Integration Study Phase 2, which examined operational impacts of high penetrations of variable renewable generation in the West.

  6. Understanding of solar wind structure might be wrong

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

    of solar wind structure might be wrong The plasma particles flowing from the Sun and blasting past the Earth might be configured more as a network of tubes than a...

  7. Western Wind and Solar Integration Study: Phase 2 (Presentation)

    SciTech Connect (OSTI)

    Lew, D.; Brinkman, G.; Ibanez, E.; Lefton, S.; Kumar, N.; Venkataraman, S.; Jordan, G.

    2013-09-01

    This presentation summarizes the scope and results of the Western Wind and Solar Integration Study Phase 2, which examined operational impacts of high penetrations of variable renewable generation in the West.

  8. The Western Wind and Solar Integration Study Phase 2

    Office of Energy Efficiency and Renewable Energy (EERE)

    Greg Brinkman will present the results of the Western Wind and Solar Integration Study (WWSIS), Phase 2. This study, which follows the first phase of WWSIS, focuses on potential emissions and wear...

  9. Potential for Development of Solar and Wind Resource in Bhutan

    SciTech Connect (OSTI)

    Gilman, P.; Cowlin, S.; Heimiller, D.

    2009-09-01

    With support from the U.S. Agency for International Development (USAID), the U.S. Department of Energy's National Renewable Energy Laboratory (NREL) produced maps and data of the wind and solar resources in Bhutan. The solar resource data show that Bhutan has an adequate resource for flat-plate collectors, with annual average values of global horizontal solar radiation ranging from 4.0 to 5.5 kWh/m2-day (4.0 to 5.5 peak sun hours per day). The information provided in this report may be of use to energy planners in Bhutan involved in developing energy policy or planning wind and solar projects, and to energy analysts around the world interested in gaining an understanding of Bhutan's wind and solar energy potential.

  10. The dynamic character of the polar solar wind

    SciTech Connect (OSTI)

    Jackson, B. V.; Yu, H.-S.; Buffington, A.; Hick, P. P. E-mail: hsyu@ucsd.edu E-mail: pphick@ucsd.edu

    2014-09-20

    The Solar and Heliospheric Observatory (SOHO) Large Angle and Spectrometric Coronagraph C2 and Solar Terrestrial Relations Observatory (STEREO) COR2A coronagraph images, when analyzed using correlation tracking techniques, show a surprising result in places ordinarily thought of as 'quiet' solar wind above the poles in coronal hole regions. Instead of the static well-ordered flow and gradual acceleration normally expected, coronagraph images show outflow in polar coronal holes consisting of a mixture of intermittent slow and fast patches of material. We compare measurements of this highly variable solar wind from C2 and COR2A images and show that both coronagraphs measure essentially the same structures. Measurements of the mean velocity as a function of height of these structures are compared with mass flux determinations of the solar wind outflow in the large polar coronal hole regions and give similar results.

  11. Western Wind and Solar Integration Study Phase 2: Preprint

    SciTech Connect (OSTI)

    Lew, D.; Brinkman, G.; Ibanez, E.; Hodge, B.-M.; King, J.

    2012-09-01

    The Western Wind and Solar Integration Study (WWSIS) investigates the impacts of high penetrations of wind and solar power into the Western Interconnection of the United States. WWSIS2 builds on the Phase 1 study but with far greater refinement in the level of data inputs and production simulation. It considers the differences between wind and solar power on systems operations. It considers mitigation options to accommodate wind and solar when full costs of wear-and-tear and full impacts of emissions rates are taken into account. It determines wear-and-tear costs and emissions impacts. New data sets were created for WWSIS2, and WWSIS1 data sets were refined to improve realism of plant output and forecasts. Four scenarios were defined for WWSIS2 that examine the differences between wind and solar and penetration level. Transmission was built out to bring resources to load. Statistical analysis was conducted to investigate wind and solar impacts at timescales ranging from seasonal down to 5 minutes.

  12. Interplanetary Scintillation Observations of Stream Interaction Regions in the Solar Wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; O’Neill, I. J.

    2010-01-01

    1985, Measurements of the solar wind velocity with EISCAT.scintillation. J. Atmos. Solar Terr. Phys. 58, 507. Breen,Eiscat measurements of the solar wind. Ann. Geophys. 14,

  13. Interplanetary Field Enhancements: The Interaction between Solar Wind and Interplanetary Dusty Plasma Released by Interplanetary Collisions

    E-Print Network [OSTI]

    Lai, Hairong

    2014-01-01

    R.A. , 1976. Depletion of solar wind plasma near a planetaryLayers………………………. ………. ………………1 1.1.2. Solar MagneticField and Solar Wind……………………………. …………. …2 1.2. Small

  14. Radiation belt electrons respond to multiple solar wind inputs

    E-Print Network [OSTI]

    Radiation belt electrons respond to multiple solar wind inputs E. J. Rigler,1 M. Wiltberger,1 and D is clearly valuable from a practical standpoint, but the latter helps build confidence in any physical on the fractional or percent variance of radiation belt electron flux that can be attributed to each different solar

  15. Modeling Jets in the Corona and Solar Wind

    E-Print Network [OSTI]

    Torok, T; Titov, V S; Leake, J E; Mikic, Z; Linker, J A; Linton, M G

    2015-01-01

    Coronal jets are transient, collimated eruptions that occur in regions of predominantly open magnetic field in the solar corona. Our understanding of these events has greatly evolved in recent years but several open questions, such as the contribution of coronal jets to the solar wind, remain. Here we present an overview of the observations and numerical modeling of coronal jets, followed by a brief description of "next-generation" simulations that include an advanced description of the energy transfer in the corona ("thermodynamic MHD"), large spherical computational domains, and the solar wind. These new models will allow us to address some of the open questions.

  16. Relationship Between Solar Wind Speed and Coronal Magnetic Field Properties

    E-Print Network [OSTI]

    Fujiki, Ken'ichi; Iju, Tomoya; Hakamada, Kazuyuki; Kojima, Masayoshi

    2015-01-01

    We have studied the relationship between the solar-wind speed $[V]$ and the coronal magnetic-field properties (a flux expansion factor [$f$] and photospheric magnetic-field strength [$B_{\\mathrm{S}}$]) at all latitudes using data of interplanetary scintillation and solar magnetic field obtained for 24 years from 1986 to 2009. Using a cross-correlation analyses, we verified that $V$ is inversely proportional to $f$ and found that $V$ tends to increase with $B_{\\mathrm{S}}$ if $f$ is the same. As a consequence, we find that $V$ has extremely good linear correlation with $B_{\\mathrm{S}}/f$. However, this linear relation of $V$ and $B_{\\mathrm{S}}/f$ cannot be used for predicting the solar-wind velocity without information on the solar-wind mass flux. We discuss why the inverse relation between $V$ and $f$ has been successfully used for solar-wind velocity prediction, even though it does not explicitly include the mass flux and magnetic-field strength, which are important physical parameters for solar-wind accele...

  17. Solar, Wind, Hydropower: Home Renewable Energy Installations...

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

    to find out about financial incentives in your area. Addthis Related Articles Use solar power to heat water and more Today's solar power is highly efficient. You can buy...

  18. Name _____________________ Lab 10. Solar and Wind Power

    E-Print Network [OSTI]

    Perfect, Ed

    be "daisy-chained" by connecting them together to create a solar panel to produce more electricity. For example solar panels can be put on the roofs of buildings or they can be arranged in larger arrays in open that we can produce using solar panels obviously depends on the amount of sunlight that strikes the panels

  19. Role of Concentrating Solar Power in Integrating Solar and Wind Energy: Preprint

    SciTech Connect (OSTI)

    Denholm, P.; Mehos, M.

    2015-06-03

    As wind and solar photovoltaics (PV) increase in penetration it is increasingly important to examine enabling technologies that can help integrate these resources at large scale. Concentrating solar power (CSP) when deployed with thermal energy storage (TES) can provide multiple services that can help integrate variable generation (VG) resources such as wind and PV. CSP with TES can provide firm, highly flexible capacity, reducing minimum generation constraints which limit penetration and results in curtailment. By acting as an enabling technology, CSP can complement PV and wind, substantially increasing their penetration in locations with adequate solar resource.

  20. "Complexity" Induced Plasma Turbulence in Coronal Holes and the Solar Wind

    E-Print Network [OSTI]

    that are generally detected in the solar wind [10]. We also address the concept of resonant energization of solar"Complexity" Induced Plasma Turbulence in Coronal Holes and the Solar Wind Tom Chang Center that plasma turbulence emanating from coronal holes may efficiently accelerate the solar wind to observed

  1. Evidence that solar wind fluctuations substantially affect global convection and substorm occurrence

    E-Print Network [OSTI]

    California at Berkeley, University of

    that this implies that solar wind ULF power may be an important contributor to the strength of coupling of solar for the connection between iono- spheric convection and solar wind ULF power. The high correlations between ULF powerEvidence that solar wind fluctuations substantially affect global convection and substorm

  2. The characteristics of sharp (small-scale) boundaries of solar wind plasma and magnetic field structures

    E-Print Network [OSTI]

    Richardson, John

    The characteristics of sharp (small-scale) boundaries of solar wind plasma and magnetic field are the boundaries of small-scale and mid- dle-scale solar wind structures. We describe the behavior of the solar boundaries of small and medium scale solar wind plasma structures which we identify by looking for sharp

  3. CHANDRA OBSERVATIONS OF THE ``DARK'' MOON AND GEOCORONAL SOLAR WIND CHARGE TRANSFER

    E-Print Network [OSTI]

    Wargelin, Bradford J.

    CHANDRA OBSERVATIONS OF THE ``DARK'' MOON AND GEOCORONAL SOLAR WIND CHARGE TRANSFER B. J. Wargelin, which were tentatively ascribed to continuum emission from energetic solar wind electrons impacting with contemporaneous measurements of solar wind parameters, strongly favor charge transfer between highly charged solar

  4. Long-term-average, solar cycle, and seasonal response of magnetospheric energetic electrons to the solar wind speed

    E-Print Network [OSTI]

    Vassiliadis, Dimitrios

    is parameterized by the time delay (t), measured from the time of solar wind impact, and the L shell (L). We to the solar wind speed D. Vassiliadis,1 A. J. Klimas,2 S. G. Kanekal,3 D. N. Baker,3 and R. S. Weigel4. [1] Among the interplanetary activity parameters the solar wind speed is the one best correlated

  5. Magnetic field gradients in solar wind plasma and geophysics periods

    E-Print Network [OSTI]

    A. Bershadskii

    2006-11-16

    Using recent data obtained by Advanced Composition Explorer (ACE) the pumping scale of the magnetic field gradients of the solar wind plasma has been calculated. This pumping scale is found to be equal to 24h $\\pm$ 2h. The ACE spacecraft orbits at the L1 libration point which is a point of Earth-Sun gravitational equilibrium about 1.5 million km from Earth. Since the Earth's magnetosphere extends into the vacuum of space from approximately 80 to 60,000 kilometers on the side toward the Sun the pumping scale cannot be a consequence of the 24h-period of the Earth's rotation. Vise versa, a speculation is suggested that for the very long time of the coexistence of Earth and of the solar wind the weak interaction between the solar wind and Earth could lead to stochastic synchronization between the Earth's rotation and the pumping scale of the solar wind magnetic field gradients. This synchronization could transform an original period of the Earth's rotation to the period close to the pumping scale of the solar wind magnetic field gradients.

  6. THE TURBULENT CASCADE AND PROTON HEATING IN THE SOLAR WIND DURING SOLAR MINIMUM

    SciTech Connect (OSTI)

    Coburn, Jesse T.; Smith, Charles W.; Vasquez, Bernard J.; Stawarz, Joshua E.; Forman, Miriam A. E-mail: Charles.Smith@unh.edu E-mail: Joshua.Stawarz@Colorado.edu

    2012-08-01

    The recently protracted solar minimum provided years of interplanetary data that were largely absent in any association with observed large-scale transient behavior on the Sun. With large-scale shear at 1 AU generally isolated to corotating interaction regions, it is reasonable to ask whether the solar wind is significantly turbulent at this time. We perform a series of third-moment analyses using data from the Advanced Composition Explorer. We show that the solar wind at 1 AU is just as turbulent as at any other time in the solar cycle. Specifically, the turbulent cascade of energy scales in the same manner proportional to the product of wind speed and temperature. Energy cascade rates during solar minimum average a factor of 2-4 higher than during solar maximum, but we contend that this is likely the result of having a different admixture of high-latitude sources.

  7. Weakest solar wind of the space age and the current 'MINI' solar maximum

    SciTech Connect (OSTI)

    McComas, D. J.; Angold, N.; Elliott, H. A.; Livadiotis, G.; Schwadron, N. A.; Smith, C. W.; Skoug, R. M.

    2013-12-10

    The last solar minimum, which extended into 2009, was especially deep and prolonged. Since then, sunspot activity has gone through a very small peak while the heliospheric current sheet achieved large tilt angles similar to prior solar maxima. The solar wind fluid properties and interplanetary magnetic field (IMF) have declined through the prolonged solar minimum and continued to be low through the current mini solar maximum. Compared to values typically observed from the mid-1970s through the mid-1990s, the following proton parameters are lower on average from 2009 through day 79 of 2013: solar wind speed and beta (?11%), temperature (?40%), thermal pressure (?55%), mass flux (?34%), momentum flux or dynamic pressure (?41%), energy flux (?48%), IMF magnitude (?31%), and radial component of the IMF (?38%). These results have important implications for the solar wind's interaction with planetary magnetospheres and the heliosphere's interaction with the local interstellar medium, with the proton dynamic pressure remaining near the lowest values observed in the space age: ?1.4 nPa, compared to ?2.4 nPa typically observed from the mid-1970s through the mid-1990s. The combination of lower magnetic flux emergence from the Sun (carried out in the solar wind as the IMF) and associated low power in the solar wind points to the causal relationship between them. Our results indicate that the low solar wind output is driven by an internal trend in the Sun that is longer than the ?11 yr solar cycle, and they suggest that this current weak solar maximum is driven by the same trend.

  8. Solar Wind Sources in the Late Declining Phase of Cycle 23: Effects of the Weak Solar Polar Field on High Speed Streams

    E-Print Network [OSTI]

    2009-01-01

    B spacecraft for L1 solar wind prediction purposes (e.g.solar wind model currently running at the NOAA Space Weather Prediction

  9. Agua Caliente Wind/Solar Project at Whitewater Ranch

    SciTech Connect (OSTI)

    Hooks, Todd; Stewart, Royce

    2014-12-16

    Agua Caliente Band of Cahuilla Indians (ACBCI) was awarded a grant by the Department of Energy (DOE) to study the feasibility of a wind and/or solar renewable energy project at the Whitewater Ranch (WWR) property of ACBCI. Red Mountain Energy Partners (RMEP) was engaged to conduct the study. The ACBCI tribal lands in the Coachella Valley have very rich renewable energy resources. The tribe has undertaken several studies to more fully understand the options available to them if they were to move forward with one or more renewable energy projects. With respect to the resources, the WWR property clearly has excellent wind and solar resources. The DOE National Renewable Energy Laboratory (NREL) has continued to upgrade and refine their library of resource maps. The newer, more precise maps quantify the resources as among the best in the world. The wind and solar technology available for deployment is also being improved. Both are reducing their costs to the point of being at or below the costs of fossil fuels. Technologies for energy storage and microgrids are also improving quickly and present additional ways to increase the wind and/or solar energy retained for later use with the network management flexibility to provide power to the appropriate locations when needed. As a result, renewable resources continue to gain more market share. The transitioning to renewables as the major resources for power will take some time as the conversion is complex and can have negative impacts if not managed well. While the economics for wind and solar systems continue to improve, the robustness of the WWR site was validated by the repeated queries of developers to place wind and/or solar there. The robust resources and improving technologies portends toward WWR land as a renewable energy site. The business case, however, is not so clear, especially when the potential investment portfolio for ACBCI has several very beneficial and profitable alternatives.

  10. The turbulent cascade and proton heating in the solar wind during solar minimum

    SciTech Connect (OSTI)

    Coburn, Jesse T.; Smith, Charles W.; Vasquez, Bernard J.; Stawarz, Joshua E.; Forman, Miriam A.

    2013-06-13

    Solar wind measurements at 1 AU during the recent solar minimum and previous studies of solar maximum provide an opportunity to study the effects of the changing solar cycle on in situ heating. Our interest is to compare the levels of activity associated with turbulence and proton heating. Large-scale shears in the flow caused by transient activity are a source that drives turbulence that heats the solar wind, but as the solar cycle progresses the dynamics that drive the turbulence and heat the medium are likely to change. The application of third-moment theory to Advanced Composition Explorer (ACE) data gives the turbulent energy cascade rate which is not seen to vary with the solar cycle. Likewise, an empirical heating rate shows no significan changes in proton heating over the cycle.

  11. CORE ELECTRON HEATING IN SOLAR WIND RECONNECTION EXHAUSTS

    SciTech Connect (OSTI)

    Pulupa, M. P.; Salem, C.; Phan, T. D.; Bale, S. D.; Gosling, J. T.

    2014-08-10

    We present observational evidence of core electron heating in solar wind reconnection exhausts. We show two example events, one which shows clear heating of the core electrons within the exhaust, and one which demonstrates no heating. The event with heating occurred during a period of high inflow Alfvén speed (V {sub AL}), while the event with no heating had a low V {sub AL}. This agrees with the results of a recent study of magnetopause exhausts, and suggests that similar core electron heating can occur in both symmetric (solar wind) and asymmetric (magnetopause) exhausts.

  12. CHARACTERIZATION OF TRANSITIONS IN THE SOLAR WIND PARAMETERS

    SciTech Connect (OSTI)

    Perri, S.; Balogh, A. E-mail: a.balogh@imperial.ac.u

    2010-02-20

    The distinction between fast and slow solar wind streams and the dynamically evolved interaction regions is reflected in the characteristic fluctuations of both the solar wind and the embedded magnetic field. High-resolution magnetic field data from the Ulysses spacecraft have been analyzed. The observations show rapid variations in the magnetic field components and in the magnetic field strength, suggesting a structured nature of the solar wind at small scales. The typical sizes of fluctuations cover a broad range. If translated to the solar surface, the scales span from the size of granules ({approx}10{sup 3} km) and supergranules ({approx}10{sup 4} km) on the Sun down to {approx}10{sup 2} km and less. The properties of the short time structures change in the different types of solar wind. While fluctuations in fast streams are more homogeneous, slow streams present a bursty behavior in the magnetic field variances, and the regions of transition are characterized by high levels of power in narrow structures around the transitions. The probability density functions of the magnetic field increments at several scales reveal a higher level of intermittency in the mixed streams, which is related to the presence of well localized features. It is concluded that, apart from the differences in the nature of fluctuations in flows of different coronal origin, there is a small-scale structuring that depends on the origin of streams themselves but it is also related to a bursty generation of the fluctuations.

  13. Wind and Solar on the Power Grid: Myths and Misperceptions, Greening...

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

    SOLAR ON THE POWER GRID: MYTHS AND MISPERCEPTIONS GREENING THE GRID Wind and solar are inherently more variable and uncertain than the traditional dispatchable thermal and hydro...

  14. U.S. Virgin Islands- Solar and Wind Easements & Rights Laws

    Broader source: Energy.gov [DOE]

    In the U.S. Virgin Islands, the owner of a solar or wind-energy system is permitted to negotiate for assurance of continued access to the system’s energy source. "Solar or wind-energy system" is...

  15. Western Wind and Solar Integration Study: Executive Summary, (WWSIS) May 2010

    SciTech Connect (OSTI)

    R. Piwko; K. Clark; L. Freeman; G. Jordan; N. Miller

    2010-05-01

    This report provides a summary of background, approach, and findings of the Western Wind and Solar Integration Study (WWSIS).

  16. Grand Traverse Band Renewable Energy Feasibility Study in Wind, Biomass and Solar

    SciTech Connect (OSTI)

    Suzanne McSawby, Project Director Steve Smiley, Principle Investigator Grand Traverse Resort, Cost Sharing Partner

    2008-12-31

    Renewable Energy Feasibility Study for wind, biomass, solar on the Grand Traverse Band tribal lands from 2005 - 2008

  17. Solar wind drivers of large geomagnetically induced currents during the solar cycle 23

    E-Print Network [OSTI]

    Bergen, Universitetet i

    amplitudes. The best correlation with the GIC amplitudes was found with the solar wind electric field geomagnetically induced currents during the solar cycle 23, Space Weather, 6, S10002, doi:10.1029/2007SW000374. 1) in tech- nological conductor systems such as power grids or pipelines [e.g., Boteler, 2003; Pirjola, 2000

  18. IMPLICATIONS OF THE RECENT LOW SOLAR MINIMUM FOR THE SOLAR WIND DURING THE MAUNDER MINIMUM

    SciTech Connect (OSTI)

    Lockwood, M.; Owens, M. J., E-mail: m.lockwood@reading.ac.uk [Department of Meteorology, University of Reading, Earley Gate, RG6 6BB (United Kingdom)

    2014-01-20

    The behavior of the Sun and near-Earth space during grand solar minima is not understood; however, the recent long and low minimum of the decadal-scale solar cycle gives some important clues, with implications for understanding the solar dynamo and predicting space weather conditions. The speed of the near-Earth solar wind and the strength of the interplanetary magnetic field (IMF) embedded within it can be reliably reconstructed for before the advent of spacecraft monitoring using observations of geomagnetic activity that extend back to the mid-19th century. We show that during the solar cycle minima around 1879 and 1901 the average solar wind speed was exceptionally low, implying the Earth remained within the streamer belt of slow solar wind flow for extended periods. This is consistent with a broader streamer belt, which was also a feature of the recent low minimum (2009), and yields a prediction that the low near-Earth IMF during the Maunder minimum (1640-1700), as derived from models and deduced from cosmogenic isotopes, was accompanied by a persistent and relatively constant solar wind of speed roughly half the average for the modern era.

  19. The genesis solar-wind sample return mission

    SciTech Connect (OSTI)

    Wiens, Roger C

    2009-01-01

    The compositions of the Earth's crust and mantle, and those of the Moon and Mars, are relatively well known both isotopically and elementally. The same is true of our knowledge of the asteroid belt composition, based on meteorite analyses. Remote measurements of Venus, the Jovian atmosphere, and the outer planet moons, have provided some estimates of their compositions. The Sun constitutes a large majority, > 99%, of all the matter in the solar system. The elemental composition of the photosphere, the visible 'surface' of the Sun, is constrained by absorption lines produced by particles above the surface. Abundances for many elements are reported to the {+-}10 or 20% accuracy level. However, the abundances of other important elements, such as neon, cannot be determined in this way due to a relative lack of atomic states at low excitation energies. Additionally and most importantly, the isotopic composition of the Sun cannot be determined astronomically except for a few species which form molecules above sunspots, and estimates derived from these sources lack the accuracy desired for comparison with meteoritic and planetary surface samples measured on the Earth. The solar wind spreads a sample of solar particles throughout the heliosphere, though the sample is very rarified: collecting a nanogram of oxygen, the third most abundant element, in a square centimeter cross section at the Earth's distance from the Sun takes five years. Nevertheless, foil collectors exposed to the solar wind for periods of hours on the surface of the Moon during the Apollo missions were used to determine the helium and neon solar-wind compositions sufficiently to show that the Earth's atmospheric neon was significantly evolved relative to the Sun. Spacecraft instruments developed subsequently have provided many insights into the composition of the solar wind, mostly in terms of elemental composition. These instruments have the advantage of observing a number of parameters simultaneously, including charge state distributions, velocities, and densities, all of which have been instrumental in characterizing the nature of the solar wind. However, these instruments have lacked the ability to make large dynamic range measurements of adjacent isotopes (i.e., {sup 17}O/{sup 16}O {approx} 2500) or provide the permil (tenths of percent) accuracy desirable for comparison with geochemical isotopic measurements. An accurate knowledge of the solar and solar-wind compositions helps to answer important questions across a number of disciplines. It aids in understanding the acceleration mechanisms of the solar wind, gives an improved picture of the charged particle environment near the photosphere, it constrains processes within the Sun over its history, and it provides a database by which to compare differences among planetary systems with the solar system's starting composition, providing key information on planetary evolution. For example, precise knowledge of solar isotopic and elemental compositions of volatile species in the Sun provides a baseline for models of atmospheric evolution over time for Earth, Venus, and Mars. Additionally, volatile and chemically active elements such as C, H, O, N, and S can tell us about processes active during the evolution of the solar nebula. A classic example of this is the oxygen isotope system. In the 1970s it was determined that the oxygen isotopic ratio in refractory inclusions in primitive meteorites was enriched {approx}4% in {sup 16}O relative to the average terrestrial, lunar, and thermally processed meteorite materials. In addition, all processed solar-system materials appeared to each have a unique oxygen isotopic composition (except the Moon and Earth, which are thought to be formed from the same materials), though differences are in the fraction of a percent range, much smaller than the refractory material {sup 16}O enrichment. Several theories were developed over the years to account for the oxygen isotope heterogeneity, each theory predicting a different solar isotopic composition and each invoking a differ

  20. Proton corebeam system in the expanding solar wind: Hybrid simulations

    E-Print Network [OSTI]

    California at Berkeley, University of

    Proton corebeam system in the expanding solar wind: Hybrid simulations Petr Hellinger1,2 and Pavel 9 November 2011. [1] Results of a twodimensional hybrid expanding box simulation of a proton to a decrease of the ratio between the proton perpendicular and parallel temperatures as well as to an increase

  1. Western Wind and Solar Integration Study: Executive Summary

    Broader source: Energy.gov [DOE]

    This study investigates the operational impact of up to 35% energy penetration of wind, photovoltaics (PVs), and concentrating solar power (CSP) on the power system operated by the WestConnect group of utilities in Arizona, Colorado, Nevada, New Mexico, and Wyoming.

  2. Ring current formation influenced by solar wind substorm conditions

    E-Print Network [OSTI]

    Winglee, Robert M.

    Click Here for Full Article Ring current formation influenced by solar wind substorm conditions M outflows during an internally driven substorm. We show that the energization of the ions is not correlated with the time that the ions leave the ionosphere; instead energization is correlated with the formation

  3. Hydro, Solar, Wind The Future of Renewable Energy

    E-Print Network [OSTI]

    Lavaei, Javad

    Hydro, Solar, Wind The Future of Renewable Energy Joseph Flocco David Lath Department of Electrical the turbine speed constant. The available hydro power is calculated using the height difference between source has become popular and has many immediate benefits to communities that opt to build a hydro

  4. Enhanced solar wind geoeffectiveness after a sudden increase in dynamic pressure during southward IMF orientation

    E-Print Network [OSTI]

    Lummerzheim, Dirk

    a pressure front impact lead to enhanced coupling between the solar wind and the terrestrial magnetosphereEnhanced solar wind geoeffectiveness after a sudden increase in dynamic pressure during southward increase in solar wind pressure results in poleward expansion of the auroral oval and closing of the polar

  5. THEMIS observations of a hot flow anomaly: Solar wind, magnetosheath, and ground-based measurements

    E-Print Network [OSTI]

    Mende, Stephen B.

    solar wind, and it has been suggested that they have a significant impact on the mag- netosphere [eTHEMIS observations of a hot flow anomaly: Solar wind, magnetosheath, and ground-based measurements and the subsequent downstream response. THEMIS-A, in the solar wind, observed classic HFA signatures. Isotropic

  6. Nightside flow enhancement associated with solar wind dynamic pressure driven reconnection

    E-Print Network [OSTI]

    Lummerzheim, Dirk

    the impact of a solar wind dynamic pressure front. Their results show a significant increase in iono- sphericNightside flow enhancement associated with solar wind dynamic pressure driven reconnection A years the prominent role of solar wind dynamic pressure in enhancing dayside and nightside reconnection

  7. Title: Feasibility Study for 20 MW Hybrid Solar and Wind Park in Colombia

    E-Print Network [OSTI]

    Johnson, Eric E.

    1 of 2 Title: Feasibility Study for 20 MW Hybrid Solar and Wind Park in Colombia Principal to assess the Colombian solar and wind resources, looking at different technology options, anticipated performance, and evaluating the economics of solar and wind power technologies. The NMSU team also evaluates

  8. Effect of solar wind pressure pulses on the size and strength of the auroral oval

    E-Print Network [OSTI]

    Lummerzheim, Dirk

    Effect of solar wind pressure pulses on the size and strength of the auroral oval A. Boudouridis, E. [1] It has recently been found that solar wind dynamic pressure changes can dramatically affect solar wind dynamic pressure increases on the location, size, and intensity of the auroral oval using

  9. Predicting the arrival of high-speed solar wind streams at Earth using the STEREO

    E-Print Network [OSTI]

    Lockwood, Mike

    Predicting the arrival of high-speed solar wind streams at Earth using the STEREO Heliospheric of solar wind speed to predict the arrival of such streams at Earth, assuming they corotated with the Sun November 2011; accepted 11 December 2011; published 16 February 2012. [1] High-speed solar wind streams

  10. Prediction of the AL index using solar wind Xinlin Li,1,2,5

    E-Print Network [OSTI]

    Li, Xinlin

    Prediction of the AL index using solar wind parameters Xinlin Li,1,2,5 Kap Soo Oh,1,3 and M are based on solar wind and magnetometer data from the year 1995. The simple model predicts the 10-min averaged AL index for 1995 using only solar wind measurements with a prediction efficiency of 0

  11. Interplanetary scintillation observations of the solar wind disappearance event of May 1999

    E-Print Network [OSTI]

    Padmanabhan, Janardhan

    of the solar wind. They are derived from the power spectrum of the observed intensity fluctuations of compactInterplanetary scintillation observations of the solar wind disappearance event of May 1999 V scintillation (IPS) observations of the solar wind during the period centered around 11 May 1999, when the Earth

  12. Energy analysis of substorms based on remote sensing techniques, solar wind measurements, and geomagnetic indices

    E-Print Network [OSTI]

    Ã?stgaard, Nikolai

    Energy analysis of substorms based on remote sensing techniques, solar wind measurements to balance the energy budget. We find that a viscous interaction that transfers 0.17% of the solar wind, is sufficient to balance the total energy dissipation UT. INDEX TERMS: 2784 Magnetospheric Physics: Solar wind

  13. Global and multi-scale features of solar wind-magnetosphere coupling: From modeling to forecasting

    E-Print Network [OSTI]

    Sitnov, Mikhail I.

    Global and multi-scale features of solar wind-magnetosphere coupling: From modeling to forecasting issue. This paper presents a data-derived model of the solar wind-magnetosphere coupling that combines of solar wind-magnetosphere coupling: From modeling to forecasting, Geophys. Res. Lett., 31, L08802, doi:10

  14. The Solar Wind: Probing the Heliosphere with Multiple Spacecraft John D. Richardson

    E-Print Network [OSTI]

    Richardson, John

    1 The Solar Wind: Probing the Heliosphere with Multiple Spacecraft John D. Richardson Center of the Voyager spacecraft in the outer heliosphere, Ulysses at high latitudes, and multiple solar wind monitors near Earth provides a unique opportunity to study the global structure and evolution of the solar wind

  15. Solar Wind and Interplanetary Magnetic Field: A Tutorial C. T. Russell

    E-Print Network [OSTI]

    Russell, Christopher T.

    Solar Wind and Interplanetary Magnetic Field: A Tutorial C. T. Russell Institute of Geophysics at the center of the sun to its radiation into space by the photosphere, but most importantly for the solar wind controls the properties of the solar wind. In this tutorial review we examine the properties of the fields

  16. THE SOLAR WIND INTERACTION WITH UNMAGNETIZED PLANETS: A TUTORIAL J. G. Luhmann

    E-Print Network [OSTI]

    California at Berkeley, University of

    THE SOLAR WIND INTERACTION WITH UNMAGNETIZED PLANETS: A TUTORIAL J. G. Luhmann Institute of solar wind origin is transported through the ionopause and distributed within the ionosphere theorists and observationalists. The relative strength of the solar wind and ionospheric pressures at Mars

  17. Effect of solar wind variation on low-energy O+ populations in the magnetosphere during

    E-Print Network [OSTI]

    Carlson, Charles W.

    Effect of solar wind variation on low-energy O+ populations in the magnetosphere during geomagneticFadden, E. J. Lund, and C. W. Carlson (2008), Effect of solar wind variation on low-energy O+ populations 2008. [1] The relationship between solar wind conditions and variations in low-energy (

  18. Are energetic electrons in the solar wind the source of the outer radiation belt?

    E-Print Network [OSTI]

    Li, Xinlin

    . Mewaldt6 Abstract. Using data from WIND, SAMPEX (Solar, Anomalous, and Magnetospheric Particle Explorer the outer radiation belt electrons. Al- though lower energy electrons in the solar wind could be a seedAre energetic electrons in the solar wind the source of the outer radiation belt? Xinlin Li,1 D. N

  19. Hybrid energy cell for simultaneously harvesting wind, solar, and chemical energies

    E-Print Network [OSTI]

    Wang, Zhong L.

    Hybrid energy cell for simultaneously harvesting wind, solar, and chemical energies Yingchun Wu1 KEYWORDS hybrid energy cell, wind energy, solar energy, triboelectric nanogenerators, electrochemical cells ABSTRACT We report a hybrid energy cell that can simultaneously or individually harvest wind, solar

  20. Discrepancies in the Prediction of Solar Wind using Potential Field Source Surface Model: An

    E-Print Network [OSTI]

    Zhao, Xuepu

    Discrepancies in the Prediction of Solar Wind using Potential Field Source Surface Model. This inverse relation has been made use of in the prediction of solar wind speed at 1 AU using a potential between the magnetic flux tube expansion factor (FTE) at the source surface and the solar wind speed

  1. Solar wind turbulence at 0.72 AU and solar minimum

    E-Print Network [OSTI]

    Teodorescu, Eliza; Munteanu, Costel; Zhang, Tielong; Bruno, Roberto; Kovacs, Peter

    2015-01-01

    We investigate Venus Express (VEX) observations of magnetic field fluctuations performed systematically in the solar wind at 0.72 Astronomical Units (AU), between 2007 and 2009, during the deep minimum of the solar cycle 24. The Power Spectral Densities (PSD) of the magnetic field components have been computed for the time intervals that satisfy data integrity criteria and have been grouped according to the type of wind, fast and slow defined for speeds larger and respectively smaller than 450 km/s. The PSDs show higher levels of power for the fast than for the slow wind. The spectral slopes estimated for all PSDs in the frequency range 0.005-0.1 Hz exhibit a normal distribution. The average value of the trace of the spectral matrix is -1.60 for fast solar wind and -1.65 for slow wind. Compared to the corresponding average slopes at 1 AU, the PSDs are shallower at 0.72 AU for slow wind conditions suggesting a steepening of the solar wind spectra between Venus and Earth. No significant time variation trend is ...

  2. Large Scale Wind and Solar Integration in Germany

    SciTech Connect (OSTI)

    Ernst, Bernhard; Schreirer, Uwe; Berster, Frank; Pease, John; Scholz, Cristian; Erbring, Hans-Peter; Schlunke, Stephan; Makarov, Yuri V.

    2010-02-28

    This report provides key information concerning the German experience with integrating of 25 gigawatts of wind and 7 gigawatts of solar power capacity and mitigating its impacts on the electric power system. The report has been prepared based on information provided by the Amprion GmbH and 50Hertz Transmission GmbH managers and engineers to the Bonneville Power Administration (BPA) and Pacific Northwest National Laboratory representatives during their visit to Germany in October 2009. The trip and this report have been sponsored by the BPA Technology Innovation office. Learning from the German experience could help the Bonneville Power Administration engineers to compare and evaluate potential new solutions for managing higher penetrations of wind energy resources in their control area. A broader dissemination of this experience will benefit wind and solar resource integration efforts in the United States.

  3. 20th Century Reanalysis Project Ensemble Gateway: 56 Estimates of World Temperature, Pressure, Humidity, and Wind, 1871-2010

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

    This site provides data from the 20th Century Reanalysis Project, offering temperature, pressure, humidity, and wind predictions in 200 km sections all around the earth from 1871 to 2010, every 6 hours, based on historical data. The ensemble mean and standard deviation for each value were calculated over a set of 56 simulations. Data for each of the 56 ensemble members are included here. The dataset consists of files in netCDF 4 format that are available for download from the National Energy Research. The goal of the 20th Century Reanalysis Project is to use a Kalman filter-based technique to produce a global trophospheric circulation dataset at four-times-daily resolution back to 1871. The only dataset available for the early 20th century consists of error-ridden hand-drawn analyses of the mean sea level pressure field over the Northern Hemisphere. Modern data assimilation systems have the potential to improve upon these maps, but prior to 1948, few digitized upper-air sounding observations are available for such a reanalysis. The global tropospheric circulation dataset will provide an important validation check on the climate models used to make 21st century climate projections....[copied from http://portal.nersc.gov/project/20C_Reanalysis/

  4. Improved Method for Specifying Solar Wind Speed Near the Sun Charles N. Arge*

    E-Print Network [OSTI]

    California at Berkeley, University of

    much better than one derived previously, which is a function of fs only. We focus here on the solarImproved Method for Specifying Solar Wind Speed Near the Sun Charles N. Arge* , Dusan Odstrcil solar wind flow speed near the Sun (~0.1 AU) us- ing a set of three simple inter-linked coronal/solar

  5. Long-term-average, solar cycle, and seasonal response of magnetospheric energetic electrons to the solar wind speed

    E-Print Network [OSTI]

    . [1] Among the interplanetary activity parameters the solar wind speed is the one best correlatedLong-term-average, solar cycle, and seasonal response of magnetospheric energetic electrons to the solar wind speed D. Vassiliadis,1 A. J. Klimas,2 S. G. Kanekal,3 D. N. Baker,3 and R. S. Weigel4

  6. Solar wind samples give insight into birth of solar system

    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 RoomPreservation ofAlbuquerque|Sensitive Species3performedValley |Solar PowerofThermalSolar

  7. Western Wind and Solar Integration Study: Hydropower Analysis

    SciTech Connect (OSTI)

    Acker, T.; Pete, C.

    2012-03-01

    The U.S. Department of Energy's (DOE) study of 20% Wind Energy by 2030 was conducted to consider the benefits, challenges, and costs associated with sourcing 20% of U.S. energy consumption from wind power by 2030. This study found that with proactive measures, no insurmountable barriers were identified to meet the 20% goal. Following this study, DOE and the National Renewable Energy Laboratory (NREL) conducted two more studies: the Eastern Wind Integration and Transmission Study (EWITS) covering the eastern portion of the U.S., and the Western Wind and Solar Integration Study (WWSIS) covering the western portion of the United States. The WWSIS was conducted by NREL and research partner General Electric (GE) in order to provide insight into the costs, technical or physical barriers, and operational impacts caused by the variability and uncertainty of wind, photovoltaic, and concentrated solar power when employed to serve up to 35% of the load energy in the WestConnect region (Arizona, Colorado, Nevada, New Mexico, and Wyoming). WestConnect is composed of several utility companies working collaboratively to assess stakeholder and market needs to and develop cost-effective improvements to the western wholesale electricity market. Participants include the Arizona Public Service, El Paso Electric Company, NV Energy, Public Service of New Mexico, Salt River Project, Tri-State Generation and Transmission Cooperative, Tucson Electric Power, Xcel Energy and the Western Area Power Administration.

  8. CME propagation: Where does the solar wind drag take over?

    E-Print Network [OSTI]

    Sachdeva, Nishtha; Colaninno, Robin; Vourlidas, Angelos

    2015-01-01

    We investigate the Sun-Earth dynamics of a set of eight well observed solar coronal mass ejections (CMEs) using data from the STEREO spacecraft. We seek to quantify the extent to which momentum coupling between these CMEs and the ambient solar wind (i.e., the aerodynamic drag) influences their dynamics. To this end, we use results from a 3D flux rope model fit to the CME data. We find that solar wind aerodynamic drag adequately accounts for the dynamics of the fastest CME in our sample. For the relatively slower CMEs, we find that drag-based models initiated below heliocentric distances ranging from 15 to 50 $R_{\\odot}$ cannot account for the observed CME trajectories. This is at variance with the general perception that the dynamics of slow CMEs are influenced primarily by solar wind drag from a few $R_{\\odot}$ onwards. Several slow CMEs propagate at roughly constant speeds above 15--50 $R_{\\odot}$. Drag-based models initiated above these heights therefore require negligible aerodynamic drag to explain their...

  9. Small solar wind transients: Stereo-A observations in 2009

    SciTech Connect (OSTI)

    Yu, W.; Farrugia, C. J.; Galvin, A. B.; Simunac, K. D. C.; Popecki, M. A.; Lugaz, N.; Kilpua, E. K. J.; Moestl, C.; Luhmann, J. G.; Opitz, A.; Sauvaud, J.-A.

    2013-06-13

    Year 2009 was the last year of a long and pronounced solar activity minimum. In this year the solar wind in the inner heliosphere was for 90% of the time slow (< 450 km s{sup -1}) and with a weaker magnetic field strength compared to the previous solar minimum 1995-1996. We choose this year to present the results of a systematic search for small solar wind transients (STs) observed by the STEREO-Ahead (ST-A) probe. The data are from the PLASTIC and IMPACT instrument suites. By 'small' we mean a duration from {approx}1 to 12 hours. The parameters we search for to identify STs are (i) the total field strength, (ii) the rotation of the magnetic field vector, (iii) its smoothness, (iv) proton temperature, (v) proton beta, and (vi) Alfven Mach number. We find 45 examples. The STs have an average duration of {approx}4 hours. Ensemble averages of key quantities are: (i) maximum B = 7.01 nT; (ii) proton {beta}= 0.18; (iii) proton thermal speed = 20.8 km s{sup -1}; and (iv) Alfven Mach number = 6.13. No distinctive feature is found in the pitch angle distributions of suprathermal electrons. Our statistical results are compared with those of STs observed near Earth by Wind during 2009.

  10. Solar and Wind Easements | Department of Energy

    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 Natural GasAdjustmentsShirleyEnergyTher iSlide 1 More Documents &1000radiation, often6 SolarLoan to InvestWebsite

  11. Solar and Wind Rights | Department of Energy

    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 Natural GasAdjustmentsShirleyEnergyTher iSlide 1 More Documents &1000radiation, often6 SolarLoanSavings<- Passive

  12. Nebraska Wind and Solar | 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:QAsource History ViewMayo, Maryland:NPI Ventures Ltd Jump to:InformationNdunga Geothermal PowerSolar Jump to:

  13. Supercomputers Capture Turbulence in the Solar 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 WebQuantity ofkandz-cm11 Outreach Home RoomPreservationBio-Inspired Solar Fuel Production 1: Total systemsSuccess NSECCapture

  14. VENUS EXPRESS STUDIES PERTAINING TO THE LOSS OF THE VENUS ATMOSPHERE BY ITS INTERACTION WITH THE SOLAR WIND

    E-Print Network [OSTI]

    California at Berkeley, University of

    WITH THE SOLAR WIND C. T. Russell, T. L. Zhang, M. Delva, S. Barabash, J. G. Luhmann, and H. Y. Wei The solar wind can be a source and a sink for planetary atmospheres. This is especially true for unmagnetized effectively excludes the solar wind from the planetary atmosphere but that the solar wind can still erode

  15. Extended Coronal Heating and Solar Wind Acceleration Over the Solar Cycle

    E-Print Network [OSTI]

    Cranmer, Steven R; Miralles, Mari Paz; van Ballegooijen, Adriaan A

    2010-01-01

    This paper reviews our growing understanding of the physics behind coronal heating (in open-field regions) and the acceleration of the solar wind. Many new insights have come from the last solar cycle's worth of observations and theoretical work. Measurements of the plasma properties in the extended corona, where the primary solar wind acceleration occurs, have been key to discriminating between competing theories. We describe how UVCS/SOHO measurements of coronal holes and streamers over the last 14 years have provided clues about the detailed kinetic processes that energize both fast and slow wind regions. We also present a brief survey of current ideas involving the coronal source regions of fast and slow wind streams, and how these change over the solar cycle. These source regions are discussed in the context of recent theoretical models (based on Alfven waves and MHD turbulence) that have begun to successfully predict both the heating and acceleration in fast and slow wind regions with essentially no fre...

  16. Predicted Impacts of Proton Temperature Anisotropy on Solar Wind Turbulence

    E-Print Network [OSTI]

    Klein, Kristopher G

    2015-01-01

    Particle velocity distributions measured in the weakly collisional solar wind are frequently found to be non-Maxwellian, but how these non-Maxwellian distributions impact the physics of plasma turbulence in the solar wind remains unanswered. Using numerical solutions of the linear dispersion relation for a collisionless plasma with a bi-Maxwellian proton velocity distribution, we present a unified framework for the four proton temperature anisotropy instabilities, identifying the associated stable eigenmodes, highlighting the unstable region of wavevector space, and presenting the properties of the growing eigenfunctions. Based on physical intuition gained from this framework, we address how the proton temperature anisotropy impacts the nonlinear dynamics of the \\Alfvenic fluctuations underlying the dominant cascade of energy from large to small scales and how the fluctuations driven by proton temperature anisotropy instabilities interact nonlinearly with each other and with the fluctuations of the large-scal...

  17. Magnetic Field Rotations in the Solar Wind at Kinetic Scales

    E-Print Network [OSTI]

    Chen, C H K; Burgess, D; Horbury, T S

    2015-01-01

    The solar wind magnetic field contains rotations at a broad range of scales, which have been extensively studied in the MHD range. Here we present an extension of this analysis to the range between ion and electron kinetic scales. The distribution of rotation angles was found to be approximately log-normal, shifting to smaller angles at smaller scales almost self-similarly, but with small, statistically significant changes of shape. The fraction of energy in fluctuations with angles larger than $\\alpha$ was found to drop approximately exponentially with $\\alpha$, with e-folding angle $9.8^\\circ$ at ion scales and $0.66^\\circ$ at electron scales, showing that large angles ($\\alpha > 30^\\circ$) do not contain a significant amount of energy at kinetic scales. Implications for kinetic turbulence theory and the dissipation of solar wind turbulence are discussed.

  18. Dissipation-Scale Turbulence in the Solar Wind

    E-Print Network [OSTI]

    Gregory G. Howes; Steven C. Cowley; William Dorland; Gregory W. Hammett; Eliot Quataert; Alexander A. Schekochihin

    2007-07-20

    We present a cascade model for turbulence in weakly collisional plasmas that follows the nonlinear cascade of energy from the large scales of driving in the MHD regime to the small scales of the kinetic Alfven wave regime where the turbulence is dissipated by kinetic processes. Steady-state solutions of the model for the slow solar wind yield three conclusions: (1) beyond the observed break in the magnetic energy spectrum, one expects an exponential cut-off; (2) the widely held interpretation that this dissipation range obeys power-law behavior is an artifact of instrumental sensitivity limitations; and, (3) over the range of parameters relevant to the solar wind, the observed variation of dissipation range spectral indices from -2 to -4 is naturally explained by the varying effectiveness of Landau damping, from an undamped prediction of -7/3 to a strongly damped index around -4.

  19. Residual energy in magnetohydrodynamic turbulence and in the solar wind

    E-Print Network [OSTI]

    Stanislav Boldyrev; Jean Carlos Perez; Vladimir Zhdankin

    2011-08-30

    Recent observations indicate that kinetic and magnetic energies are not in equipartition in the solar wind turbulence. Rather, magnetic fluctuations are more energetic and have somewhat steeper energy spectrum compared to the velocity fluctuations. This leads to the presence of the so-called residual energy E_r=E_v-E_b in the inertial interval of turbulence. This puzzling effect is addressed in the present paper in the framework of weak turbulence theory. Using a simple model of weakly colliding Alfv\\'en waves, we demonstrate that the kinetic-magnetic equipartition indeed gets broken as a result of nonlinear interaction of Alfv\\'en waves. We establish that magnetic energy is indeed generated more efficiently as a result of these interactions, which proposes an explanation for the solar wind observations.

  20. Magnetic Discontinuities in Magnetohydrodynamic Turbulence and in the Solar Wind

    E-Print Network [OSTI]

    Vladimir Zhdankin; Stanislav Boldyrev; Joanne Mason; Jean Carlos Perez

    2012-04-19

    Recent measurements of solar wind turbulence report the presence of intermittent, exponentially distributed angular discontinuities in the magnetic field. In this Letter, we study whether such discontinuities can be produced by magnetohydrodynamic (MHD) turbulence. We detect the discontinuities by measuring the fluctuations of the magnetic field direction, Delta theta, across fixed spatial increments Delta x in direct numerical simulations of MHD turbulence with an imposed uniform guide field B_0. A large region of the probability density function (pdf) for Delta theta is found to follow an exponential decay, proportional to exp(-Delta theta/theta_*), with characteristic angle theta_* ~ (14 deg) (b_rms/B_0)^0.65 for a broad range of guide-field strengths. We find that discontinuities observed in the solar wind can be reproduced by MHD turbulence with reasonable ratios of b_rms/B_0. We also observe an excess of small angular discontinuities when Delta x becomes small, possibly indicating an increasing statistical significance of dissipation-scale structures. The structure of the pdf in this case closely resembles the two-population pdf seen in the solar wind. We thus propose that strong discontinuities are associated with inertial-range MHD turbulence, while weak discontinuities emerge from near-dissipation-range turbulence. In addition, we find that the structure functions of the magnetic field direction exhibit anomalous scaling exponents, which indicates the existence of intermittent structures.

  1. Scaling anisotropy of the power in parallel and perpendicular components of the solar wind magnetic field

    E-Print Network [OSTI]

    Oughton, Sean

    Scaling anisotropy of the power in parallel and perpendicular components of the solar wind magnetic of the Power in Parallel and Perpendicular Components of the Solar Wind Magnetic Field Miriam A. Forman1 ZLWK GLVWDQFH IURP WKH 6XQ 7KLV GDWD LQFOXGHV WKH VRlar wind whose total power (Pxx + Pyy + Pzz#12; LQ

  2. Kinetic And Potential Sputtering Of Lunar Regolith: The Contribution Of The Heavy (Minority) Solar Wind Ions

    E-Print Network [OSTI]

    Wind Ions F.W. Meyera1 , P.R. Harrisa2 , H.M. Meyer IIIb , H. Hijazia , A.F. Barghoutyc a Physics, Huntsville, AL 35812, USA Abstract. In this paper the sputtering of lunar regolith by protons and solar wind of JSC-1A AGGL lunar regolith simulant at solar wind velocities, and TRIM simulations of kinetic

  3. A SURVEY OF FIELD-ALIGNED MACH NUMBER AND PLASMA BETA IN THE SOLAR WIND

    E-Print Network [OSTI]

    De Sterck, Hans

    A SURVEY OF FIELD-ALIGNED MACH NUMBER AND PLASMA BETA IN THE SOLAR WIND JOHAN DE KEYSER and MICHEL Katholieke Universiteit Leuven, Leuven, Belgium Abstract. We have surveyed solar wind plasma beta and field-aligned Alfvénic Mach number using Ulysses and Wind data. We show the characteristic timescale and occurrence

  4. Kolmogorov versus IroshnikovKraichnan spectra: Consequences for ion heating in the solar wind

    E-Print Network [OSTI]

    Ng, Chung-Sang

    heating in the solar wind C. S. Ng,1 A. Bhattacharjee,2 D. Munsi,2 P. A. Isenberg,2 and C. W. Smith2 wind provides a quantitative, if indirect, observational constraint on the relevant phenomenology. Recently, a solar wind heating model based on Kolmogorov spectral scaling has produced reasonably good

  5. Multiple-spacecraft study of an extended magnetic structure in the solar wind

    E-Print Network [OSTI]

    Wiegelmann, Thomas

    ] studied a small-scale flux rope in the solar wind, which is in close proximity to a heat flux dropoutMultiple-spacecraft study of an extended magnetic structure in the solar wind P. Ruan,1 A. Korth,1. [1] An extended magnetic structure was observed consecutively by five spacecraft (ACE, WIND, STEREO

  6. Sharp boundaries of small-and middle-scale solar wind structures

    E-Print Network [OSTI]

    Richardson, John

    Sharp boundaries of small- and middle-scale solar wind structures M. O. Riazantseva1 and G. N wind ion flux changes which are not due to shocks. These changes are boundaries of small- and middle boundaries of small- and middle-scale solar wind structures, J. Geophys. Res., 110, A12110, doi:10

  7. RAPID MEASUREMENTS OF SOLAR WIND IONS WITH THE TRIANA PLASMAG FARADAY CUP

    E-Print Network [OSTI]

    Richardson, John

    of the solar wind all the time, data in a new energy per charge window can be taken as soon as the power supply for several instruments on various spacecraft (s/c). Instrument s/c stabilization tspec [s] Launch year WIND/SWE/FCRAPID MEASUREMENTS OF SOLAR WIND IONS WITH THE TRIANA PLASMAG FARADAY CUP MATTHIAS R. AELLIG, ALAN

  8. The Solar Wind Interaction with the Earth's Magnetosphere: A Tutorial C. T. Russell

    E-Print Network [OSTI]

    Russell, Christopher T.

    The Solar Wind Interaction with the Earth's Magnetosphere: A Tutorial C. T. Russell Department wind dynamic pressure and the pressure exerted by the magnetosphere, principally that of its magnetic field. The shape of the magnetosphere is additionally influenced by the drag of the solar wind

  9. Solar-wind magnetosphere coupling, including relativistic electron energization, during high-speed streams

    E-Print Network [OSTI]

    Lyons, Larry

    Solar-wind­ magnetosphere coupling, including relativistic electron energization, during high. If this inference is correct, and if it is chorus that energizes the relativistic electrons, then high-speed solar-speed solar wind streams, and fluxes of relativistic electrons observed at geosynchronous orbit enhance

  10. Complementary Effect of Wind and Solar Energy Sources in a Microgrid

    E-Print Network [OSTI]

    Pota, Himanshu Roy

    Complementary Effect of Wind and Solar Energy Sources in a Microgrid M. A. Barik, Student Member. Index Terms--Microgrid, renewable energy sources, reactive power mismatch, solar integration, voltage-mass energy, etc. Of them wind and solar energy is broadly used for their characteristics. This paper presents

  11. Propagation of three--dimensional Alfv'en waves in a stratified, thermally conducting solar wind

    E-Print Network [OSTI]

    Propagation of three--dimensional Alfv'en waves in a stratified, thermally conducting solar wind S to the well--known thermal expansion of the solar corona [Parker, 1958, 1963, 1991]. In particular Alfv'en waves in the solar atmosphere and wind, taking into account relevant physical effects

  12. THE GENESIS SOLAR-WIND COLLECTOR MATERIALS A. J. G. Jurewicz1

    E-Print Network [OSTI]

    THE GENESIS SOLAR-WIND COLLECTOR MATERIALS A. J. G. Jurewicz1 , D. S. Burnett2 , R. C. Wiens3 , T. #12;THE GENESIS SOLAR-WIND COLLECTOR MATERIALS Abstract. Genesis (NASA Discovery Mission #5) is a sample return mission. Collectors comprised of ultra-high purity materials will be exposed to the solar

  13. EPRI conference proceedings: solar and wind power - 1982 status and outlook

    SciTech Connect (OSTI)

    DeMeo, E.A.

    1983-02-01

    Separate abstracts were prepared for 18 papers in this proceedings. Not separately abstracted are speeches and presentations covering: past progress and future directions in solar and wind power research and development, new directions in Federal solar electric programs, Solar Energy Research Institute status and outlook, ARCO Solar Industries' involvement in the production of potential solar electric technologies, wind power status and outlook, utility requirements, roles and rewards, and a panel discussion on solar and wind power status and outlook as viewed from industrial, utility, financial, and government perspectives. (LEW)

  14. Radio Remote Sensing of the Corona and the Solar Wind

    E-Print Network [OSTI]

    Steven R. Spangler; Catherine A. Whiting

    2008-09-26

    Modern radio telescopes are extremely sensitive to plasma on the line of sight from a radio source to the antenna. Plasmas in the corona and solar wind produce measurable changes in the radio wave amplitude and phase, and the phase difference between wave fields of opposite circular polarization. Such measurements can be made of radio waves from spacecraft transmitters and extragalactic radio sources, using radio telescopes and spacecraft tracking antennas. Data have been taken at frequencies from about 80 MHz to 8000 MHz. Lower frequencies probe plasma at greater heliocentric distances. Analysis of these data yields information on the plasma density, density fluctuations, and plasma flow speeds in the corona and solar wind, and on the magnetic field in the solar corona. This paper will concentrate on the information that can be obtained from measurements of Faraday rotation through the corona and inner solar wind. The magnitude of Faraday rotation is proportional to the line of sight integral of the plasma density and the line-of-sight component of the magnetic field. Faraday rotation provides an almost unique means of estimating the magnetic field in this part of space. This technique has contributed to measurement of the large scale coronal magnetic field, the properties of electromagnetic turbulence in the corona, possible detection of electrical currents in the corona, and probing of the internal structure of coronal mass ejections (CMEs). This paper concentrates on the search for small-scale coronal turbulence and remote sensing of the structure of CMEs. Future investigations with the Expanded Very Large Array (EVLA) or Murchison Widefield Array (MWA) could provide unique observational input on the astrophysics of CMEs.

  15. Depth profiling analysis of solar wind helium collected in diamond-like carbon film from Genesis

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

    Bajo, Ken-ichi; Olinger, Chad T.; Jurewicz, Amy J.G.; Burnett, Donald S.; Sakaguchi, Isao; Suzuki, Taku; Itose, Satoru; Ishihara, Morio; Uchino, Kiichiro; Wieler, Rainer; et al

    2015-10-01

    The distribution of solar-wind ions in Genesis mission collectors, as determined by depth profiling analysis, constrains the physics of ion solid interactions involving the solar wind. Thus, they provide an experimental basis for revealing ancient solar activities represented by solar-wind implants in natural samples. We measured the first depth profile of ?He in a collector; the shallow implantation (peaking at more »is consistent with TRIM simulations using the observed ?He velocity distribution during the Genesis mission. It is therefore likely that all solar-wind elements heavier than H are completely intact in this Genesis collector and, consequently, the solar particle energy distributions for each element can be calculated from their depth profiles. Ancient solar activities and space weathering of solar system objects could be quantitatively reproduced by solar particle implantation profiles.« less

  16. Wind Tunnel Tests of Parabolic Trough Solar Collectors: March 2001--August 2003

    SciTech Connect (OSTI)

    Hosoya, N.; Peterka, J. A.; Gee, R. C.; Kearney, D.

    2008-05-01

    Conducted extensive wind-tunnel tests on parabolic trough solar collectors to determine practical wind loads applicable to structural design for stress and deformation, and local component design for concentrator reflectors.

  17. Using Solar Business Models to Expand the Distributed Wind Market (Presentation)

    SciTech Connect (OSTI)

    Savage, S.

    2013-05-01

    This presentation to attendees at Wind Powering America's All-States Summit in Chicago describes business models that were responsible for rapid growth in the solar industry and that may be applicable to the distributed wind industry as well.

  18. Investigating the Correlation Between Wind and Solar Power Forecast Errors in the Western Interconnection: Preprint

    SciTech Connect (OSTI)

    Zhang, J.; Hodge, B. M.; Florita, A.

    2013-05-01

    Wind and solar power generations differ from conventional energy generation because of the variable and uncertain nature of their power output. This variability and uncertainty can have significant impacts on grid operations. Thus, short-term forecasting of wind and solar generation is uniquely helpful for power system operations to balance supply and demand in an electricity system. This paper investigates the correlation between wind and solar power forecasting errors.

  19. Operation of Concentrating Solar Power Plants in the Western Wind and Solar Integration Phase 2 Study

    SciTech Connect (OSTI)

    Denholm, P.; Brinkman, G.; Lew, D.; Hummon, M.

    2014-05-01

    The Western Wind and Solar Integration Study (WWSIS) explores various aspects of the challenges and impacts of integrating large amounts of wind and solar energy into the electric power system of the West. The phase 2 study (WWSIS-2) is one of the first to include dispatchable concentrating solar power (CSP) with thermal energy storage (TES) in multiple scenarios of renewable penetration and mix. As a result, it provides unique insights into CSP plant operation, grid benefits, and how CSP operation and configuration may need to change under scenarios of increased renewable penetration. Examination of the WWSIS-2 results indicates that in all scenarios, CSP plants with TES provides firm system capacity, reducing the net demand and the need for conventional thermal capacity. The plants also reduced demand during periods of short-duration, high ramping requirements that often require use of lower efficiency peaking units. Changes in CSP operation are driven largely by the presence of other solar generation, particularly PV. Use of storage by the CSP plants increases in the higher solar scenarios, with operation of the plant often shifted to later in the day. CSP operation also becomes more variable, including more frequent starts. Finally, CSP output is often very low during the day in scenarios with significant PV, which helps decrease overall renewable curtailment (over-generation). However, the configuration studied is likely not optimal for High Solar Scenario implying further analysis of CSP plant configuration is needed to understand its role in enabling high renewable scenarios in the Western United States.

  20. Reconstruction of Helio-latitudinal Structure of the Solar Wind Proton Speed and Density

    E-Print Network [OSTI]

    Sokó?, Justyna M; Bzowski, Maciej; Tokumaru, Munetoshi

    2015-01-01

    The modeling of the heliosphere requires continuous three-dimensional solar wind data. The in-situ out-of-ecliptic measurements are very rare, so that other methods of solar wind detection are needed. We use the remote sensing data of the solar wind speed from observations of interplanetary scintillation (IPS) to reconstruct spatial and temporal structures of the solar wind proton speed from 1985 to 2013. We developed a method of filling the data gaps in the IPS observations to obtain continuous and homogeneous solar wind speed records. We also present a method to retrieve the solar wind density from the solar wind speed, utilizing the invariance of the solar wind dynamic pressure and energy flux with latitude. To construct the synoptic maps of solar wind speed we use the decomposition into spherical harmonics of each of the Carrington rotation map. To fill the gaps in time we apply the singular spectrum analysis to the time series of the coefficients of spherical harmonics. We obtained helio-latitudinal prof...

  1. The solar wind interaction with Mars: Recent progress and future directions The Sun has a powerful influence on planetary atmospheres.

    E-Print Network [OSTI]

    California at Berkeley, University of

    Editorial The solar wind interaction with Mars: Recent progress and future directions The Sun has field, because the solar wind can interact directly with the upper atmo- sphere. Neutral particles in the upper atmosphere are ionized by solar photons and through interactions with solar wind charged particles

  2. A study of density modulation index in the inner heliospheric solar wind during solar cycle 23

    SciTech Connect (OSTI)

    Bisoi, Susanta Kumar; Janardhan, P.; Ingale, M.; Subramanian, P.; Ananthakrishnan, S.; Tokumaru, M.; Fujiki, K. E-mail: jerry@prl.res.in E-mail: p.subramanian@iiserpune.ac.in E-mail: tokumaru@stelab.nagoya-u.ac.jp

    2014-11-01

    The ratio of the rms electron density fluctuations to the background density in the solar wind (density modulation index, ? {sub N} ? ?N/N) is of vital importance for understanding several problems in heliospheric physics related to solar wind turbulence. In this paper, we have investigated the behavior of ? {sub N} in the inner heliosphere from 0.26 to 0.82 AU. The density fluctuations ?N have been deduced using extensive ground-based observations of interplanetary scintillation at 327 MHz, which probe spatial scales of a few hundred kilometers. The background densities (N) have been derived using near-Earth observations from the Advanced Composition Explorer. Our analysis reveals that 0.001 ? ? {sub N} ? 0.02 and does not vary appreciably with heliocentric distance. We also find that ? {sub N} declines by 8% from 1998 to 2008. We discuss the impact of these findings on problems ranging from our understanding of Forbush decreases to the behavior of the solar wind dynamic pressure over the recent peculiar solar minimum at the end of cycle 23.

  3. Solar/Wind Permitting Standards | 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| Open Energy Information Serbia-Enhancing Capacity forSilicium deEnergyCompany LimitedSolar/Wind Permitting Standards

  4. Power House Solar and 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 Inc Jump to:Newberg,Energy LLC JumpPhonoSolar and Wind Jump to: navigation, search

  5. Global Atlas for Solar and Wind Energy | 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 E LISTStar2-0057-EA Jump to:ofEniaElectric JumpAtlas for Solar and Wind Energy Jump to:

  6. Low-Resolution STELab IPS 3D Reconstructions of the Whole Heliosphere Interval and Comparison with in-Ecliptic Solar Wind Measurements from STEREO and Wind Instrumentation

    E-Print Network [OSTI]

    Bisi, M. M.; Jackson, B. V.; Buffington, A.; Clover, J. M.; Hick, P. P.; Tokumaru, M.

    2009-01-01

    structure of the fast solar wind. J. Geophys. Res. 112,observations of the solar wind. Proc. SPIE 6689, 668911-1.W.A. , Maagoe, S. : 1972, Solar wind velocity from ips

  7. SCALE DEPENDENCE OF MAGNETIC HELICITY IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Brandenburg, Axel; Subramanian, Kandaswamy; Balogh, Andre; Goldstein, Melvyn L. E-mail: kandu@iucaa.ernet.in E-mail: melvyn.l.goldstein@nasa.gov

    2011-06-10

    We determine the magnetic helicity, along with the magnetic energy, at high latitudes using data from the Ulysses mission. The data set spans the time period from 1993 to 1996. The basic assumption of the analysis is that the solar wind is homogeneous. Because the solar wind speed is high, we follow the approach first pioneered by Matthaeus et al. by which, under the assumption of spatial homogeneity, one can use Fourier transforms of the magnetic field time series to construct one-dimensional spectra of the magnetic energy and magnetic helicity under the assumption that the Taylor frozen-in-flow hypothesis is valid. That is a well-satisfied assumption for the data used in this study. The magnetic helicity derives from the skew-symmetric terms of the three-dimensional magnetic correlation tensor, while the symmetric terms of the tensor are used to determine the magnetic energy spectrum. Our results show a sign change of magnetic helicity at wavenumber k {approx} 2 AU{sup -1} (or frequency {nu} {approx} 2 {mu}Hz) at distances below 2.8 AU and at k {approx} 30 AU{sup -1} (or {nu} {approx} 25 {mu}Hz) at larger distances. At small scales the magnetic helicity is positive at northern heliographic latitudes and negative at southern latitudes. The positive magnetic helicity at small scales is argued to be the result of turbulent diffusion reversing the sign relative to what is seen at small scales at the solar surface. Furthermore, the magnetic helicity declines toward solar minimum in 1996. The magnetic helicity flux integrated separately over one hemisphere amounts to about 10{sup 45} Mx{sup 2} cycle{sup -1} at large scales and to a three times lower value at smaller scales.

  8. Resolving the enigmatic solar wind disappearance event of 11 May 1999

    E-Print Network [OSTI]

    Padmanabhan, Janardhan

    ), potential field computations of the solar magnetic fields in the period, and HeI 10830A° observations with global, large-scale solar phenomena like the periodic 11-year solar polar field reversal is most likelyResolving the enigmatic solar wind disappearance event of 11 May 1999 P. Janardhan Astronomy

  9. Your GatewaY

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

    http:www.osti.govnle Your GatewaY to InformatIon across the Department of enerGY The National Library of Energy Beta search tool provides one-stop access to DOE information in...

  10. Temporal Evolution of the Solar-Wind Electron Core Density at Solar Minimum by Correlating SWEA Measurements from STEREO A and B

    E-Print Network [OSTI]

    2010-01-01

    IMPACT instrument suite, the SWEA electron exper- iment provides the solar-windIMPACT) investigation (Luh- mann et al. , 2008) on the STEREO mission provides multipoint solar-wind

  11. Small Scale Energy Cascade of the Solar Wind Turbulence

    E-Print Network [OSTI]

    O. Alexandrova; V. Carbone; P. Veltri; L. Sorriso-Valvo

    2007-10-03

    Magnetic fluctuations in the solar wind are distributed according to Kolmogorov's power law $f^{-5/3}$ below the ion cyclotron frequency $f_{ci}$. Above this frequency, the observed steeper power law is usually interpreted in two different ways: a dissipative range of the solar wind turbulence or another turbulent cascade, the nature of which is still an open question. Using the Cluster magnetic data we show that after the spectral break the intermittency increases toward higher frequencies, indicating the presence of non-linear interactions inherent to a new inertial range and not to the dissipative range. At the same time the level of compressible fluctuations raises. We show that the energy transfer rate and intermittency are sensitive to the level of compressibility of the magnetic fluctuations within the small scale inertial range. We conjecture that the time needed to establish this inertial range is shorter than the eddy-turnover time, and is related to dispersive effects. A simple phenomenological model, based on the compressible Hall MHD, predicts the magnetic spectrum $\\sim k^{-7/3+2\\alpha}$, which depends on the degree of plasma compression $\\alpha$.

  12. The Solar Wind Charge-Exchange Production Factor for Hydrogen

    E-Print Network [OSTI]

    Kuntz, K D; Collier, M R; Connor, H K; Cravens, T E; Koutroumpa, D; Porter, F S; Robertson, I P; Sibeck, D G; Snowden, S L; Thomas, N E; Wash, B M

    2015-01-01

    The production factor, or broad band averaged cross-section, for solar wind charge-exchange with hydrogen producing emission in the ROSAT 1/4 keV (R12) band is $3.8\\pm0.2\\times10^{-20}$ count degree$^{-2}$ cm$^4$. This value is derived from a comparison of the Long-Term (background) Enhancements in the ROSAT All-Sky Survey with magnetohysdrodynamic simulations of the magnetosheath. This value is 1.8 to 4.5 times higher than values derived from limited atomic data, suggesting that those values may be missing a large number of faint lines. This production factor is important for deriving the exact amount of 1/4 keV band flux that is due to the Local Hot Bubble, for planning future observations in the 1/4 keV band, and for evaluating proposals for remote sensing of the magnetosheath. The same method cannot be applied to the 3/4 keV band as that band, being composed primarily of the oxygen lines, is far more sensitive to the detailed abundances and ionization balance in the solar wind. We also show, incidentally,...

  13. Integrating High Penetrations of Solar in the Western United States: Results of the Western Wind and Solar Integration Study Phase 2 (Poster)

    SciTech Connect (OSTI)

    Bird, L.; Lew, D.

    2013-10-01

    This poster presents a summary of the results of the Western Wind and Solar Integration Study Phase 2.

  14. Suprathermal particle addition to solar wind pressure: possible influence on magnetospheric transmissivity of low energy cosmic rays?

    E-Print Network [OSTI]

    Bobik, P; Consolandi, C; Della Torre, S; Gervasi, M; Grandi, D; Kudela, K; La Vacca, G; Mallamaci, M; Pensotti, S; Rancoita, P G; Rozza, D; Tacconi, M

    2013-01-01

    Energetic (suprathermal) solar particles, accelerated in the interplanetary medium, contribute to the solar wind pressure, in particular during high solar activity periods. We estimated the effect of the increase of solar wind pressure due to suprathermal particles on magnetospheric transmissivity of galactic cosmic rays in the case of one recent solar event.

  15. The solar wind neon abundance observed with ACE/SWICS and ULYSSES/SWICS

    SciTech Connect (OSTI)

    Shearer, Paul; Raines, Jim M.; Lepri, Susan T.; Thomas, Jonathan W.; Gilbert, Jason A.; Landi, Enrico; Zurbuchen, Thomas H.; Von Steiger, Rudolf

    2014-07-01

    Using in situ ion spectrometry data from ACE/SWICS, we determine the solar wind Ne/O elemental abundance ratio and examine its dependence on wind speed and evolution with the solar cycle. We find that Ne/O is inversely correlated with wind speed, is nearly constant in the fast wind, and correlates strongly with solar activity in the slow wind. In fast wind streams with speeds above 600 km s{sup –1}, we find Ne/O = 0.10 ± 0.02, in good agreement with the extensive polar observations by Ulysses/SWICS. In slow wind streams with speeds below 400 km s{sup –1}, Ne/O ranges from a low of 0.12 ± 0.02 at solar maximum to a high of 0.17 ± 0.03 at solar minimum. These measurements place new and significant empirical constraints on the fractionation mechanisms governing solar wind composition and have implications for the coronal and photospheric abundances of neon and oxygen. The results are made possible by a new data analysis method that robustly identifies rare elements in the measured ion spectra. The method is also applied to Ulysses/SWICS data, which confirms the ACE observations and extends our view of solar wind neon into the three-dimensional heliosphere.

  16. Energetic plasma sheet electrons and their relationship with the solar wind: A Cluster and Geotail study

    E-Print Network [OSTI]

    Li, Xinlin

    Energetic plasma sheet electrons and their relationship with the solar wind: A Cluster and Geotail February 2009. [1] The statistical relationship between tens of kiloelectron volts plasma sheet electrons and the solar wind, as well as >2 MeV geosynchronous electrons, is investigated using plasma sheet measurements

  17. Modeling the radiation belt electrons with radial diffusion driven by the solar wind

    E-Print Network [OSTI]

    Li, Xinlin

    Modeling the radiation belt electrons with radial diffusion driven by the solar wind A. B. Barker1 October 2005. [1] On the basis of the correlation between the solar wind and radiation belt electron fluxes, we develop a model to simulate the MeV electron phase space density variations from L = 3 to L

  18. Proton aurora dynamics in response to the IMF and solar wind variations

    E-Print Network [OSTI]

    California at Berkeley, University of

    Proton aurora dynamics in response to the IMF and solar wind variations S.-W. Chang,1,2 S. B. Mende; accepted 24 April 2002; published 13 July 2002. [1] On May 23, 2000, proton auroras observed by IMAGE FUV wind parameters. A proton aurora brightened at high latitude poleward from the dayside oval after solar

  19. Magnetic fluctuation power near proton temperature anisotropy instability thresholds in the solar wind

    E-Print Network [OSTI]

    California at Berkeley, University of

    Magnetic fluctuation power near proton temperature anisotropy instability thresholds in the solar wind S. D. Bale, J. C. Kasper, G. G. Howes, E. Quataert,§ C. Salem,¶ and D. Sundkvist¶ (Dated: August 10, 2009) The proton temperature anisotropy in the solar wind is known to be constrained by the theo

  20. A Two-component Transport Model for Solar Wind Fluctuations: Waves plus Quasi-2D Turbulence

    E-Print Network [OSTI]

    Oughton, Sean

    component. Thus, it would seem appropriate, and advantageous, to develop an energy-containing style modelA Two-component Transport Model for Solar Wind Fluctuations: Waves plus Quasi-2D Turbulence Sean for the transport of solar wind fluctuations, based on the assumption that they can be well-represented using two

  1. Heavy noble gases in solar wind delivered by Genesis mission Alex Meshik a,

    E-Print Network [OSTI]

    knowledge of the isotopic composition of the heavy noble gases in solar wind and, by inference, the Sun measured in the Genesis solar wind collectors generally agree with the less precise values obtained from), captured by Genesis Mission collectors (http://genesismis- sion.jpl.nasa.gov/; Burnett et al., 2003

  2. New Report: Integrating More Wind and Solar Reduces Utilities' Carbon Emissions and Fuel Costs

    Broader source: Energy.gov [DOE]

    The National Renewable Energy Laboratory (NREL) released Phase 2 of the Western Wind and Solar Integration Study (WWSIS-2), a follow-up to the initial WWSIS released in May 2010, which examined the viability, benefits, and challenges of integrating as much as 33% wind and solar power into the electricity grid of the western United States.

  3. innovati nNREL Confirms Large Potential for Grid Integration of Wind, Solar Power

    E-Print Network [OSTI]

    innovati nNREL Confirms Large Potential for Grid Integration of Wind, Solar Power To fully harvest, examining the east and west sections of the U.S. power grid. The studies show that it is technically the nation's bountiful wind and solar resources, it is critical to know how much electrical power from

  4. Impact of the solar wind dynamic pressure on the Region 2 field-aligned currents

    E-Print Network [OSTI]

    Higuchi, Tomoyuki

    Impact of the solar wind dynamic pressure on the Region 2 field-aligned currents S. Nakano,1,2 G and the solar wind dynamic pressure is investigated using magnetic field data from Defense Meteorological Satellite Program-F13 (DMSP-F13). The generation of the Region 2 currents is associated with the direction

  5. Recent Ionospheric Observations Relating to Solar-Wind--Magnetosphere Coupling [and Discussion

    E-Print Network [OSTI]

    Lockwood, Mike

    , and build upon a wide range of content in a trusted digital archive. We use information technology and toolsRecent Ionospheric Observations Relating to Solar-Wind--Magnetosphere Coupling [and Discussion Printedin GreatBritain Recent ionosphericobservationsIrelatingto solar-wind-magnetosphere coupling BY M

  6. Regulation of Solar WindMagnetosphere Coupling by Ionospheric Outflows William Lotko, PI for Dartmouth College

    E-Print Network [OSTI]

    Lotko, William

    potential are also reduced, as is the flux of outflowing ionospheric ions, access of solar wind plasmaRegulation of Solar Wind­Magnetosphere Coupling by Ionospheric Outflows William Lotko, PI blunted as shown in the figure 2, which compares proton densities at 1634 UT in global simulations

  7. An empirical model of magnetospheric chorus amplitude using solar wind and geomagnetic indices

    E-Print Network [OSTI]

    potential global models of magnetospheric chorus amplitude: one which uses only instantaneous AE* and Kp, for the first time, the global evolution of chorus amplitude as a function of solar wind and geomagnetic drivingAn empirical model of magnetospheric chorus amplitude using solar wind and geomagnetic indices D. I

  8. A new view on the solar wind interaction with the Moon

    E-Print Network [OSTI]

    Bhardwaj, Anil; Alok, Abhinaw; Barabash, Stas; Wieser, Martin; Futaana, Yoshifumi; Wurz, Peter; Vorburger, Audrey; Holmström, Mats; Lue, Charles; Harada, Yuki; Asamura, Kazushi

    2015-01-01

    Characterised by a surface bound exosphere and localised crustal magnetic fields, the Moon was considered as a passive object when solar wind interacts with it. However, the neutral particle and plasma measurements around the Moon by recent dedicated lunar missions, such as Chandrayaan-1, Kaguya, Chang'E-1, LRO, and ARTEMIS, as well as IBEX have revealed a variety of phenomena around the Moon which results from the interaction with solar wind, such as backscattering of solar wind protons as energetic neutral atoms (ENA) from lunar surface, sputtering of atoms from the lunar surface, formation of a "mini-magnetosphere" around lunar magnetic anomaly regions, as well as several plasma populations around the Moon, including solar wind protons scattered from the lunar surface, from the magnetic anomalies, pick-up ions, protons in lunar wake and more. This paper provides a review of these recent findings and presents the interaction of solar wind with the Moon in a new perspective.

  9. The Western Wind and Solar Integration Study Phase 2 (Executive Summary)

    SciTech Connect (OSTI)

    Lew, Debra; Brinkman, Greg

    2013-09-01

    The electric grid is a highly complex, interconnected machine, and changing one part of the grid can have consequences elsewhere. Adding wind and solar affects the operation of the other power plants and adding high penetrations can induce cycling of fossil-fueled generators. Cycling leads to wear-and-tear costs and changes in emissions. Phase 2 of the Western Wind and Solar Integration Study (WWSIS-2) evaluated these costs and emissions and simulated grid operations for a year to investigate the detailed impact of wind and solar on the fossil-fueled fleet. This built on Phase 1, one of the largest wind and solar integration studies ever conducted, which examined operational impacts of high wind and solar penetrations in the West(GE Energy 2010).

  10. Mars as a comet: Solar wind interaction on a large scale

    E-Print Network [OSTI]

    Holmstrom, Mats

    2015-01-01

    Looking at the Mars-solar wind interaction on a larger spatial scale than the near Mars region, the planet can be seen as an ion source interacting with the solar wind, in many ways like a comet, but with a smaller ion source region. Here we study the interaction between Mars and the solar wind using a hybrid model (particle ions and fluid electrons). We find that the solar wind is disturbed by Mars out to 100 Mars radii downstream of the planet, and beyond. On this large scale it is clear that the escaping ions can be classified into two different populations. A polar plume of ions picked-up by the solar wind, and a more fluid outflow of ions behind the planet. The outflow increases linear with the production up to levels of observed outflow rates, then the escape levels off for higher production rates.

  11. GEOPHYSICAL RESEARCH LETTERS, VOL. 0, NO. 0, PAGES 00, M 0, 2000 Three spacecraft observations of solar wind discontinuities

    E-Print Network [OSTI]

    Horbury, Tim

    of solar wind discontinuities Timothy S. Horbury, 1 David Burgess, and Markus FrË?anz Astronomy Unit, Queen

  12. Three-fluid, three-dimensional magnetohydrodynamic solar wind model with eddy viscosity and turbulent resistivity

    SciTech Connect (OSTI)

    Usmanov, Arcadi V.; Matthaeus, William H.; Goldstein, Melvyn L.

    2014-06-10

    We have developed a three-fluid, three-dimensional magnetohydrodynamic solar wind model that incorporates turbulence transport, eddy viscosity, turbulent resistivity, and turbulent heating. The solar wind plasma is described as a system of co-moving solar wind protons, electrons, and interstellar pickup protons, with separate energy equations for each species. Numerical steady-state solutions of Reynolds-averaged solar wind equations coupled with turbulence transport equations for turbulence energy, cross helicity, and correlation length are obtained by the time relaxation method in the corotating with the Sun frame of reference in the region from 0.3 to 100 AU (but still inside the termination shock). The model equations include the effects of electron heat conduction, Coulomb collisions, photoionization of interstellar hydrogen atoms and their charge exchange with the solar wind protons, turbulence energy generation by pickup protons, and turbulent heating of solar wind protons and electrons. The turbulence transport model is based on the Reynolds decomposition and turbulence phenomenologies that describe the conversion of fluctuation energy into heat due to a turbulent cascade. In addition to using separate energy equations for the solar wind protons and electrons, a significant improvement over our previous work is that the turbulence model now uses an eddy viscosity approximation for the Reynolds stress tensor and the mean turbulent electric field. The approximation allows the turbulence model to account for driving of turbulence by large-scale velocity gradients. Using either a dipole approximation for the solar magnetic field or synoptic solar magnetograms from the Wilcox Solar Observatory for assigning boundary conditions at the coronal base, we apply the model to study the global structure of the solar wind and its three-dimensional properties, including embedded turbulence, heating, and acceleration throughout the heliosphere. The model results are compared with plasma and magnetic field observations on WIND, Ulysses, and Voyager 2 spacecraft.

  13. Radial gradients of phase space density of the outer radiation belt electrons prior to sudden solar wind pressure enhancements

    E-Print Network [OSTI]

    Li, Xinlin

    PSD radial gradient at and beyond GEO prior to a sudden solar wind pressure impact based on the fact by a sudden solar wind pressure enhancement, dayside trapped electrons are transported radially inwards), Radial gradients of phase space density of the outer radiation belt electrons prior to sudden solar wind

  14. Sputtering of lunar regolith simulant by protons and singly and multicharged Ar ions at solar wind energies

    E-Print Network [OSTI]

    Sputtering of lunar regolith simulant by protons and singly and multicharged Ar ions at solar wind 2010 Keywords: Solar wind Sputtering Lunar regolith Ion-surface interactions a b s t r a c t We report charged solar wind ions using quadrupole and time-of-flight (TOF) mass spectrometry approaches. Sputtering

  15. Solar-wind protons and heavy ions sputtering of lunar surface materials A.F. Barghouty a,

    E-Print Network [OSTI]

    Solar-wind protons and heavy ions sputtering of lunar surface materials A.F. Barghouty a, , F Available online 21 December 2010 Keywords: Solar wind sputtering Lunar regolith KREEP soil Potential a c t Lunar surface materials are exposed to $1 keV/amu solar-wind protons and heavy ions on almost

  16. Four-Field Equations: a New Model for Weakly Compressible MHD Turbulence in the Solar Wind and the Interstellar Medium

    E-Print Network [OSTI]

    Ng, Chung-Sang

    Four-Field Equations: a New Model for Weakly Compressible MHD Turbulence in the Solar Wind Flight Center Turbulent plasmas in the solar wind and the interstellar medium of- ten contain a large to be in agreement. The scaling of density uctuations with Mach number are compared with solar wind data from Helios

  17. Solar wind plasma correlations between L1 and Earth J. D. Richardson, F. Dashevskiy, and K. I. Paularena

    E-Print Network [OSTI]

    Richardson, John

    1 Solar wind plasma correlations between L1 and Earth J. D. Richardson, F. Dashevskiy, and K. I. Paularena Center for Space Research, Massachusetts Institute of Technology, Cambridge Abstract. Solar wind correlation coefficients are calculated as a function of lag. The average correlations of solar wind speed

  18. Solar wind structure in the outer heliosphere J.D. Richardson a,b,*, Y. Liu a

    E-Print Network [OSTI]

    California at Berkeley, University of

    Solar wind structure in the outer heliosphere J.D. Richardson a,b,*, Y. Liu a , C. Wang b a Kavli form 8 February 2007; accepted 27 March 2007 Abstract A solar wind parcel evolves as it moves outward, interacting with the solar wind plasma ahead of and behind it and with the inter- stellar neutrals

  19. Discrepancies in the prediction of solar wind using potential field source surface model: An investigation of possible sources

    E-Print Network [OSTI]

    California at Berkeley, University of

    Discrepancies in the prediction of solar wind using potential field source surface model expansion factor (FTE) at the source surface and the solar wind speed (SWS) observed at Earth, which has been made use of in the prediction of solar wind speed near the Earth with reasonable accuracy. However

  20. Loss of solar wind plasma neutrality and affect on surface potentials near the lunar terminator and shadowed polar regions

    E-Print Network [OSTI]

    California at Berkeley, University of

    Loss of solar wind plasma neutrality and affect on surface potentials near the lunar terminator (2008), Loss of solar wind plasma neutrality and affect on surface potentials near the lunar terminator observations confirm a consistent solar wind-to-wake potential difference of many hundreds of volts (negative

  1. RECONNECTION OUTFLOW GENERATED TURBULENCE IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Vörös, Z.; Sasunov, Y. L.; Zaqarashvili, T. V.; Khodachenko, M.; Semenov, V. S.; Bruno, R.

    2014-12-10

    Petschek-type time-dependent reconnection (TDR) and quasi-stationary reconnection (QSR) models are considered to understand reconnection outflow structures and the generation of local turbulence in the solar wind. Comparing TDR/QSR model predictions of the outflow structures with actual measurements shows that both models can explain the data equally well. It is demonstrated that the outflows can often generate more or less spatially extended turbulent boundary layers. The structure of a unique extended reconnection outflow is investigated in detail. The analysis of spectral scalings and spectral break locations shows that reconnection can change the local field and plasma conditions which may support different local turbulent dissipation mechanisms at their characteristic wavenumbers.

  2. Western Wind and Solar Integration Study Phase 2 (Presentation)

    SciTech Connect (OSTI)

    Lew, D.; Brinkman, G.; Ibanez, E.; Kumar, N.; Lefton, S.; Jordan, G.; Venkataraman, S.; King, J.

    2013-06-01

    This presentation accompanies Phase 2 of the Western Wind and Solar Integration Study, a follow-on to Phase 1, which examined the operational impacts of high penetrations of variable renewable generation on the electric power system in the West and was one of the largest variable generation studies to date. High penetrations of variable generation can induce cycling of fossil-fueled generators. Cycling leads to wear-and-tear costs and changes in emissions. Phase 2 calculated these costs and emissions, and simulated grid operations for a year to investigate the detailed impact of variable generation on the fossil-fueled fleet. The presentation highlights the scope of the study and results.

  3. Particle acceleration via reconnection processes in the supersonic solar wind

    SciTech Connect (OSTI)

    Zank, G. P.; Le Roux, J. A.; Webb, G. M.; Dosch, A.; Khabarova, O.

    2014-12-10

    An emerging paradigm for the dissipation of magnetic turbulence in the supersonic solar wind is via localized small-scale reconnection processes, essentially between quasi-2D interacting magnetic islands. Charged particles trapped in merging magnetic islands can be accelerated by the electric field generated by magnetic island merging and the contraction of magnetic islands. We derive a gyrophase-averaged transport equation for particles experiencing pitch-angle scattering and energization in a super-Alfvénic flowing plasma experiencing multiple small-scale reconnection events. A simpler advection-diffusion transport equation for a nearly isotropic particle distribution is derived. The dominant charged particle energization processes are (1) the electric field induced by quasi-2D magnetic island merging and (2) magnetic island contraction. The magnetic island topology ensures that charged particles are trapped in regions where they experience repeated interactions with the induced electric field or contracting magnetic islands. Steady-state solutions of the isotropic transport equation with only the induced electric field and a fixed source yield a power-law spectrum for the accelerated particles with index ? = –(3 + M{sub A} )/2, where M{sub A} is the Alfvén Mach number. Considering only magnetic island contraction yields power-law-like solutions with index –3(1 + ? {sub c}/(8?{sub diff})), where ? {sub c}/?{sub diff} is the ratio of timescales between magnetic island contraction and charged particle diffusion. The general solution is a power-law-like solution with an index that depends on the Alfvén Mach number and the timescale ratio ?{sub diff}/? {sub c}. Observed power-law distributions of energetic particles observed in the quiet supersonic solar wind at 1 AU may be a consequence of particle acceleration associated with dissipative small-scale reconnection processes in a turbulent plasma, including the widely reported c {sup –5} (c particle speed) spectra observed by Fisk and Gloeckler and Mewaldt et al.

  4. CHARGE STATE EVOLUTION IN THE SOLAR WIND. II. PLASMA CHARGE STATE COMPOSITION IN THE INNER CORONA AND ACCELERATING FAST SOLAR WIND

    SciTech Connect (OSTI)

    Landi, E.; Gruesbeck, J. R.; Lepri, S. T.; Zurbuchen, T. H.; Fisk, L. A. [Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, MI 48109 (United States)

    2012-12-10

    In the present work, we calculate the evolution of the charge state distribution within the fast solar wind. We use the temperature, density, and velocity profiles predicted by Cranmer et al. to calculate the ionization history of the most important heavy elements in the solar corona and solar wind: C, N, O, Ne, Mg, Si, S, and Fe. The evolution of each charge state is calculated from the source region in the lower chromosphere to the final freeze-in point. We show that the solar wind velocity causes the plasma to experience significant departures from equilibrium at very low heights, well inside the field of view (within 0.6 R{sub sun} from the solar limb) of nearly all the available remote-sensing instrumentation, significantly affecting observed spectral line intensities. We also study the evolution of charge state ratios with distance from the source region, and the temperature they indicate if ionization equilibrium is assumed. We find that virtually every charge state from every element freezes in at a different height, so that the definition of freeze-in height is ambiguous. We also find that calculated freeze-in temperatures indicated by charge state ratios from in situ measurements have little relation to the local coronal temperature of the wind source region, and stop evolving much earlier than their correspondent charge state ratio. We discuss the implication of our results on plasma diagnostics of coronal holes from spectroscopic measurements as well as on theoretical solar wind models relying on coronal temperatures.

  5. Shock Acceleration of the Energetic Particle Background in the Solar Wind David T. Sodaitis

    E-Print Network [OSTI]

    on planet Earth, the solar wind is an important topic for study because it is strongly influenced by solar activity, and it transfers that solar influence "to planets, comets, dust particles, and cosmic rays of three components, a fluid model of the sun's corona which in it's equilibrium state creates a supersonic

  6. What does it take to create a clean energy future for Washington? Solar, Wind, Hydro

    E-Print Network [OSTI]

    Hochberg, Michael

    Flexible Solar Film Atomic Force Microscope Materials Science Molecule Polymers Nanostructured Solar Cells Solar, Wind, Hydro A Complete Energy System Home and Commercial Generation Demand Response 10-10 m 10 established the Clean Energy Institute to support science & engineering research that sustains Washington

  7. Transmission Benefits of Co-Locating Concentrating Solar Power and Wind

    SciTech Connect (OSTI)

    Sioshansi, R.; Denholm, P.

    2012-03-01

    In some areas of the U.S. transmission constraints are a limiting factor in deploying new wind and concentrating solar power (CSP) plants. Texas is an example of one such location, where the best wind and solar resources are in the western part of the state, while major demand centers are in the east. The low capacity factor of wind is a compounding factor, increasing the relative cost of new transmission per unit of energy actually delivered. A possible method of increasing the utilization of new transmission is to co-locate both wind and concentrating solar power with thermal energy storage. In this work we examine the benefits and limits of using the dispatachability of thermal storage to increase the capacity factor of new transmission developed to access high quality solar and wind resources in remote locations.

  8. Correlation studies between solar wind parameters and the decimetric radio emission from Jupiter

    SciTech Connect (OSTI)

    Bolton, S.J.; Gulkis, S.; Klein, M.J.; De Pater, I.; Thompson, T.J.

    1989-01-01

    Results of a study comparing long-term time variations (years) in Jupiter's synchrotron radio emission with a variety of solar wind parameters and the 10.7-cm solar flux are reported. Data from 1963 through 1985 were analyzed, and the results suggest that many solar wind parameters are correlated with the intensity of the synchrotron emission produced by the relativistic electrons in the Jovian Van Allen radiation belts. Significant nonzero correlation coefficients appear to be associated with solar wind ion density, ram pressure, thermal pressure, flow velocity, momentum, and ion temperature. The highest correlation coefficients are obtained for solar wind ram pressure (NV/sup 2/) and thermal pressure (NT). The correlation analysis suggests that the delay time between fluctuations in the solar wind and changes in the Jovian synchrotron emission is typically about 2 years. The delay time of the correlation places important constraints on the theoretical models describing the radiation belts. The implication of these results, if the correlations are real, is that the solar wind is influencing the supply and/or loss of electrons to Jupiter's inner magnetosphere. We note that the data for this work spans only about two periods of the solar activity cycle, and because of the long time scales of the observed variations, it is important to confirm these results with additional observations. copyright American Geophysical Union 1989

  9. X-RAY EMISSION FROM PLANETS AND COMETS: RELATIONSHIP WITH SOLAR X-RAYS AND SOLAR WIND

    E-Print Network [OSTI]

    Bergen, Universitetet i

    X-RAY EMISSION FROM PLANETS AND COMETS: RELATIONSHIP WITH SOLAR X-RAYS AND SOLAR WIND ANIL BHARDWAJ extraterrestrische Physik, Garching, Germany 6 Applied Physics Laboratory, John Hopkins University, Laurel, MD 20723 planets Jupiter and Saturn in the energy range of 0.2-2 keV. These flares are found to occur in tandem

  10. Probability density functions for the variable solar wind near the solar cycle minimum

    E-Print Network [OSTI]

    Vörös,; Leitner, M; Narita, Y; Consolini, G; Kovács, P; Tóth, A; Lichtenberger, J

    2015-01-01

    Unconditional and conditional statistics is used for studying the histograms of magnetic field multi-scale fluctuations in the solar wind near the solar cycle minimum in 2008. The unconditional statistics involves the magnetic data during the whole year 2008. The conditional statistics involves the magnetic field time series splitted into concatenated subsets of data according to a threshold in dynamic pressure. The threshold separates fast stream leading edge compressional and trailing edge uncompressional fluctuations. The histograms obtained from these data sets are associated with both large-scale (B) and small-scale ({\\delta}B) magnetic fluctuations, the latter corresponding to time-delayed differences. It is shown here that, by keeping flexibility but avoiding the unnecessary redundancy in modeling, the histograms can be effectively described by a limited set of theoretical probability distribution functions (PDFs), such as the normal, log-normal, kappa and logkappa functions. In a statistical sense the...

  11. On Competing Models of Coronal Heating and Solar Wind Acceleration: The Debate in '08

    E-Print Network [OSTI]

    Steven R. Cranmer

    2008-04-18

    In preparation for lively debate at the May 2008 SPD/AGU Meeting in Fort Lauderdale, this document attempts to briefly lay out my own view of the evolving controversy over how the solar wind is accelerated. It is still unknown to what extent the solar wind is fed by flux tubes that remain open (and are energized by footpoint-driven wavelike fluctuations), and to what extent much of the mass and energy is input more intermittently from closed loops into the open-field regions. It may turn out that a combination of the two ideas is needed to explain the full range of observed solar wind phenomena.

  12. On Competing Models of Coronal Heating and Solar Wind Acceleration: The Debate in '08

    E-Print Network [OSTI]

    Cranmer, Steven R

    2008-01-01

    In preparation for lively debate at the May 2008 SPD/AGU Meeting in Fort Lauderdale, this document attempts to briefly lay out my own view of the evolving controversy over how the solar wind is accelerated. It is still unknown to what extent the solar wind is fed by flux tubes that remain open (and are energized by footpoint-driven wavelike fluctuations), and to what extent much of the mass and energy is input more intermittently from closed loops into the open-field regions. It may turn out that a combination of the two ideas is needed to explain the full range of observed solar wind phenomena.

  13. The Impact of Wind and Solar on the Value of Energy Storage

    Broader source: Energy.gov [DOE]

    The purpose of this analysis is to examine how the value proposition for energy storage changes as a function of wind and solar power penetration. It uses a grid modeling approach comparing the operational costs of an electric power system both with and without added storage. It creates a series of scenarios with increasing wind and solar power penetration and examines how the value of storage changes. It also explores the mechanisms behind this change in value, including the change in on-peak and off-peak price differentials and the cost of operating reserves created by increased penetration of wind and solar energy.

  14. 5-minute Solar Oscillations and Ion Cyclotron Waves in the Solar Wind

    E-Print Network [OSTI]

    Guglielmi, Anatol; Dovbnya, Boris

    2015-01-01

    In the present paper we study impact of the photospheric 5-minute oscillations on the ion cyclotron waves in the solar wind. We proceed from the assumption that the ion cyclotron waves in solar wind are experiencing modulation with a characteristic period of 5 minutes under the influence of Alfven waves driven by photospheric motions. The theory presented in our paper predicts a deep frequency modulation of the ion cyclotron waves. The frequency modulation is expected mainly from variations in orientation of the IMF lines. In turn, the variations in orientation are caused by the Alfven waves, propagating from the Sun. To test the theoretical predictions we have analyzed records of the ultra-low-frequency (ULF) geoelectromagnetic waves in order to find the permanent quasi-monochromatic oscillations of natural origin in the Pc1-2 frequency band (0.1-5 Hz), the carrier frequency of which varies with time in a wide range. As a result we found the so-called "serpentine emission" (SE), which was observed in Antarct...

  15. Solar Wind at 33 AU: Setting Bounds on the Pluto Interaction for New Horizons

    E-Print Network [OSTI]

    Bagenal, F; Elliott, H A; Hill, M E; Lisse, C M; McComas, D J; McNutt,, R L; Richardson, J D; Smith, C W; Strobel, D F

    2015-01-01

    The NASA New Horizons spacecraft flies past Pluto on July 14, 2015, carrying two instruments that detect charged particles. Pluto has a tenuous, extended atmosphere that is escaping the weak gravity of the planet. The interaction of the solar wind with the escaping atmosphere of Pluto depends on solar wind conditions as well as the vertical structure of the atmosphere. We have analyzed Voyager 2 particles and fields measurements between 25 and 39 AU and present their statistical variations. We have adjusted these predictions to allow for the declining activity of the Sun and solar wind output. We summarize the range of SW conditions that can be expected at 33 AU and survey the range of scales of interaction that New Horizons might experience. Model estimates for the solar wind stand-off distance vary from approximately 7 to 1000 RP with our best estimate being around 40 RP (where we take the radius of Pluto to be RP=1184 km).

  16. The Western Wind and Solar Integration Study Phase 2 (Fact Sheet), NREL (National Renewable Energy Laboratory)

    Office of Energy Efficiency and Renewable Energy (EERE)

    This is one-page, two-sided fact sheet presents high-level summary results of the Western Wind and Solar Integration Study Phase 2, which examined operational impacts of high penetrations of variable renewable generation in the West.

  17. THE ORIGIN OF NON-MAXWELLIAN SOLAR WIND ELECTRON VELOCITY DISTRIBUTION FUNCTION: CONNECTION TO NANOFLARES IN THE SOLAR CORONA

    SciTech Connect (OSTI)

    Che, H.; Goldstein, M. L.

    2014-11-10

    The formation of the observed core-halo feature in the solar wind electron velocity distribution function is a long-time puzzle. In this Letter, based on the current knowledge of nanoflares, we show that the nanoflare-accelerated electron beams are likely to trigger a strong electron two-stream instability that generates kinetic Alfvén wave and whistler wave turbulence, as we demonstrated in a previous paper. We further show that the core-halo feature produced during the origin of kinetic turbulence is likely to originate in the inner corona and can be preserved as the solar wind escapes to space along open field lines. We formulate a set of equations to describe the heating processes observed in the simulation and show that the core-halo temperature ratio of the solar wind is insensitive to the initial conditions in the corona and is related to the core-halo density ratio of the solar wind and to the quasi-saturation property of the two-stream instability at the time when the exponential decay ends. This relation can be extended to the more general core-halo-strahl feature in the solar wind. The temperature ratio between the core and hot components is nearly independent of the heliospheric distance to the Sun. We show that the core-halo relative drift previously reported is a relic of the fully saturated two-stream instability. Our theoretical results are consistent with the observations while new tests for this model are provided.

  18. Wednesday, March 25, 2009 SOLAR WIND AND GENESIS: MEASUREMENTS AND INTERPRETATION

    E-Print Network [OSTI]

    Rathbun, Julie A.

    and to photospheric data to rule on fractionation between the Sun and the SW. 2:00 p.m. Grimberg A. * Bühler F. Wieler Aluminum Solar Wind Collector on Genesis [#2037] Here we report the results of our Ar-Kr-Xe analysis of solar wind captured by the Genesis Polished Aluminum Collector. 2:45 p.m. Kitts K. * Choi Y. Eng P

  19. The Western Wind and Solar Integration Study Phase 2 (Fact Sheet)

    SciTech Connect (OSTI)

    2013-09-01

    This fact sheet is a basic overview of the Western Wind and Solar Integration Study, Phase 2. The electric grid is a highly complex, interconnected machine, and changing one part of the grid can have consequences elsewhere. Adding wind and solar affects the operation of the other power plants and adding high penetrations can induce cycling of fossil-fueled generators. Cycling leads to wear-and-tear costs and changes in emissions.

  20. The Structure of the Solar Wind in the Inner Heliosphere

    E-Print Network [OSTI]

    Lee, Christina On-Yee

    2010-01-01

    do not occur for more than one solar rotation, as de?ned byof these properties that span one solar rotation (?27 days).the data are taken over one solar ro- tation as viewed from

  1. The Structure of the Solar Wind in the Inner Heliosphere

    E-Print Network [OSTI]

    Lee, Christina On-Yee

    2010-01-01

    Global Solar Magnetohydrodynamic and Potential Field SourcePFSS - Potential Field Source Surface SC - Solar Cycle SEP -N.R. : 1992, On potential ?eld models of the solar corona,

  2. Turbulence-driven coronal heating and improvements to empirical forecasting of the solar wind

    SciTech Connect (OSTI)

    Woolsey, Lauren N.; Cranmer, Steven R.

    2014-06-01

    Forecasting models of the solar wind often rely on simple parameterizations of the magnetic field that ignore the effects of the full magnetic field geometry. In this paper, we present the results of two solar wind prediction models that consider the full magnetic field profile and include the effects of Alfvén waves on coronal heating and wind acceleration. The one-dimensional magnetohydrodynamic code ZEPHYR self-consistently finds solar wind solutions without the need for empirical heating functions. Another one-dimensional code, introduced in this paper (The Efficient Modified-Parker-Equation-Solving Tool, TEMPEST), can act as a smaller, stand-alone code for use in forecasting pipelines. TEMPEST is written in Python and will become a publicly available library of functions that is easy to adapt and expand. We discuss important relations between the magnetic field profile and properties of the solar wind that can be used to independently validate prediction models. ZEPHYR provides the foundation and calibration for TEMPEST, and ultimately we will use these models to predict observations and explain space weather created by the bulk solar wind. We are able to reproduce with both models the general anticorrelation seen in comparisons of observed wind speed at 1 AU and the flux tube expansion factor. There is significantly less spread than comparing the results of the two models than between ZEPHYR and a traditional flux tube expansion relation. We suggest that the new code, TEMPEST, will become a valuable tool in the forecasting of space weather.

  3. Influence of the ambient solar wind flow on the propagation behavior of interplanetary CMEs

    E-Print Network [OSTI]

    Temmer, Manuela; Möstl, Christian; Veronig, Astrid M; Vrsnak, Bojan; Odstrcil, Dusan

    2011-01-01

    We study three CME/ICME events (2008 June 1-6, 2009 February 13-18, 2010 April 3-5) tracked from Sun to 1 AU in remote-sensing observations of STEREO Heliospheric Imagers and in situ plasma and magnetic field measurements. We focus on the ICME propagation in IP space that is governed by two forces, the propelling Lorentz force and the drag force. We address the question at which heliospheric distance range the drag becomes dominant and the CME gets adjusted to the solar wind flow. To this aim we analyze speed differences between ICMEs and the ambient solar wind flow as function of distance. The evolution of the ambient solar wind flow is derived from ENLIL 3D MHD model runs using different solar wind models, namely Wang-Sheeley-Arge (WSA) and MHD-Around-A-Sphere (MAS). Comparing the measured CME kinematics with the solar wind models we find that the CME speed gets adjusted to the solar wind speed at very different heliospheric distances in the three events under study: from below 30 Rs, to beyond 1 AU, depend...

  4. Intense plasma waves at and near the solar wind termination shock

    E-Print Network [OSTI]

    Gurnett, Donald A.

    LETTERS Intense plasma waves at and near the solar wind termination shock D. A. Gurnett1 & W. S wind termination shock. The observations were obtained from the plasma-wave instrument on the Voyager 2 a series of crossings of the termination shock at a heliocentric radial distance of 83.7 AU. The spectrum

  5. Anisotropy of Imbalanced Alfvenic Turbulence in Fast Solar Wind R. T. Wicks,1,* T. S. Horbury,1

    E-Print Network [OSTI]

    California at Berkeley, University of

    energy to yet smaller scales [3­5]. In the fast wind, the turbulence is imbalanced: there is more power solar wind [8] and from numerical simulations [9] that balanced tur- bulence is made up of locallyAnisotropy of Imbalanced Alfve´nic Turbulence in Fast Solar Wind R. T. Wicks,1,* T. S. Horbury,1 C

  6. Assessment of Wind/Solar Co-located Generation in Texas

    SciTech Connect (OSTI)

    Steven M. Wiese

    2009-07-20

    This paper evaluates the opportunity to load co-located wind and solar generation capacity onto a constrained transmission system while engendering only minimal losses. It quantifies the economic and energy opportunities and costs associated with pursuing this strategy in two Texas locations �¢���� one in west Texas and the other in south Texas. The study builds upon previous work published by the American Solar Energy Society (ASES) which illuminated the potential benefits of negative correlation of wind and solar generation in some locations by quantifying the economic and energy losses which would arise from deployment of solar generation in areas with existing wind generation and constrained transmission capacity. Clean Energy Associates (CEA) obtained and incorporated wind and solar resource data and the Electric Reliability Council of Texas (ERCOT)) load and price data into a model which evaluates varying levels of solar thermal, solar photovoltaic (PV) and wind capacity against an assumed transmission capacity limit at each of the two locations.

  7. VLF wave activity in the solar wind and the photoelectron effect in electric field measurements: Ulysses observations

    E-Print Network [OSTI]

    California at Berkeley, University of

    solar wind streams, Ulysses observed nearly continuous electric wave activity with peak power belowVLF wave activity in the solar wind and the photoelectron effect in electric field measurements present observations of very low frequency (VLF) waves (0.2 to 448 Hz) made by Ulysses during the solar

  8. Charge state evolution in the solar wind. III. Model comparison with observations

    SciTech Connect (OSTI)

    Landi, E.; Oran, R.; Lepri, S. T.; Zurbuchen, T. H.; Fisk, L. A.; Van der Holst, B.

    2014-08-01

    We test three theoretical models of the fast solar wind with a set of remote sensing observations and in-situ measurements taken during the minimum of solar cycle 23. First, the model electron density and temperature are compared to SOHO/SUMER spectroscopic measurements. Second, the model electron density, temperature, and wind speed are used to predict the charge state evolution of the wind plasma from the source regions to the freeze-in point. Frozen-in charge states are compared with Ulysses/SWICS measurements at 1 AU, while charge states close to the Sun are combined with the CHIANTI spectral code to calculate the intensities of selected spectral lines, to be compared with SOHO/SUMER observations in the north polar coronal hole. We find that none of the theoretical models are able to completely reproduce all observations; namely, all of them underestimate the charge state distribution of the solar wind everywhere, although the levels of disagreement vary from model to model. We discuss possible causes of the disagreement, namely, uncertainties in the calculation of the charge state evolution and of line intensities, in the atomic data, and in the assumptions on the wind plasma conditions. Last, we discuss the scenario where the wind is accelerated from a region located in the solar corona rather than in the chromosphere as assumed in the three theoretical models, and find that a wind originating from the corona is in much closer agreement with observations.

  9. Proton Heating in Solar Wind Compressible Turbulence with Collisions between Counter-propagating Waves

    E-Print Network [OSTI]

    He, Jiansen; Marsch, Eckart; Chen, Christopher H K; Wang, Linghua; Pei, Zhongtian; Zhang, Lei; Salem, Chadi S; Bale, Stuart D

    2015-01-01

    Magnetohydronamic turbulence is believed to play a crucial role in heating the laboratorial, space, and astrophysical plasmas. However, the precise connection between the turbulent fluctuations and the particle kinetics has not yet been established. Here we present clear evidence of plasma turbulence heating based on diagnosed wave features and proton velocity distributions from solar wind measurements by the Wind spacecraft. For the first time, we can report the simultaneous observation of counter-propagating magnetohydrodynamic waves in the solar wind turbulence. Different from the traditional paradigm with counter-propagating Alfv\\'en waves, anti-sunward Alfv\\'en waves (AWs) are encountered by sunward slow magnetosonic waves (SMWs) in this new type of solar wind compressible turbulence. The counter-propagating AWs and SWs correspond respectively to the dominant and sub-dominant populations of the imbalanced Els\\"asser variables. Nonlinear interactions between the AWs and SMWs are inferred from the non-orth...

  10. Using Wind and Solar to Reliably Meet Electricity Demand, Greening...

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

    and wind generation technologies. A variety of approaches can be deployed, including demand response, which can be used to shift demand to periods of greater renewable output,...

  11. Missing Money--Will the Current Electricity Market Structure Support High (~50%) Wind/Solar?; NREL (National Renewable Energy Laboratory)

    SciTech Connect (OSTI)

    Milligan, Michael

    2015-05-15

    This presentation summarizes the missing money problem and whether the current electricity market structure will support high penetration levels of wind and solar.

  12. EVIDENCE FOR POLAR X-RAY JETS AS SOURCES OF MICROSTREAM PEAKS IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Neugebauer, Marcia

    2012-05-01

    It is proposed that the interplanetary manifestations of X-ray jets observed in solar polar coronal holes during periods of low solar activity are the peaks of the so-called microstreams observed in the fast polar solar wind. These microstreams exhibit velocity fluctuations of {+-}35 km s{sup -1}, higher kinetic temperatures, slightly higher proton fluxes, and slightly higher abundances of the low-first-ionization-potential element iron relative to oxygen ions than the average polar wind. Those properties can all be explained if the fast microstreams result from the magnetic reconnection of bright-point loops, which leads to X-ray jets which, in turn, result in solar polar plumes. Because most of the microstream peaks are bounded by discontinuities of solar origin, jets are favored over plumes for the majority of the microstream peaks.

  13. Science Gateways : Demos

    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 RoomPreservation ofAlbuquerque| Stanford SynchrotronVideo-Contest December 17, 2015GatewaysDemos

  14. THE SOLAR WIND AS A POSSIBLE SOURCE OF FAST TEMPORAL VARIATIONS OF THE HELIOSPHERIC RIBBON

    SciTech Connect (OSTI)

    Kucharek, H.; Lee, M. A.; Moebius, E.; Schwadron, N.; Fuselier, S. A.; McComas, D.; Wurz, P.; Pogorelov, N.; Borovikov, S.; Reisenfeld, D.; Funsten, H.

    2013-10-20

    We present a possible source of pickup ions (PUIs) the ribbon observed by the Interstellar Boundary EXplorer (IBEX). We suggest that a gyrating solar wind and PUIs in the ramp and in the near downstream region of the termination shock (TS) could provide a significant source of energetic neutral atoms (ENAs) in the ribbon. A fraction of the solar wind and PUIs are reflected and energized during the first contact with the TS. Some of the solar wind may be reflected propagating toward the Sun but most of the solar wind ions form a gyrating beam-like distribution that persists until it is fully thermalized further downstream. Depending on the strength of the shock, these gyrating distributions can exist for many gyration periods until they are scattered/thermalized due to wave-particle interactions at the TS and downstream in the heliosheath. During this time, ENAs can be produced by charge exchange of interstellar neutral atoms with the gyrating ions. In order to determine the flux of energetic ions, we estimate the solar wind flux at the TS using pressure estimates inferred from in situ measurements. Assuming an average path length in the radial direction of the order of a few AU before the distribution of gyrating ions is thermalized, one can explain a significant fraction of the intensity of ENAs in the ribbon observed by IBEX. With a localized source and such a short integration path, this model would also allow fast time variations of the ENA flux.

  15. Superposed epoch analysis of magnetospheric substorms using solar wind, auroral zone, and geostationary orbit data sets

    SciTech Connect (OSTI)

    Bargatze, L.F.; Baker, D.N.; McPherron, R.L.

    1985-01-01

    A primary goal in solar wind-magnetosphere studies is to understand how and what role the solar wind plays in controlling the temporal sequence of events during substorms at many widely separated regions within the magnetosphere. Here, the average, correlated behavior of definitive solar wind, auroral zone, and geostationary orbit parameters during isolated substorms is examined. High time resolution (1 min) measurements of two solar wind quantities: B/sub z/ and VB/sub s/, two auroral electrojet indices: AE and AL, and three parameters which define the energetic (30 to 300 keV) electron distribution at geostationary orbit from 13 events are analyzed by using the superposed epoch technique. The zero epoch time used to organize the analyses were defined by the time of energetic electron injection at geostationary orbit. The average variations of the auroral zone and geostationary orbit parameters in relation to the solar wind are discussed in context of the three phase (growth, expansion, and recovery) model of substorms. Notably, we find an approximate 6 minute time lag of expansion phase onset at geostationary orbit relative to time of expansion phase onset in the auroral zone. A possible explanation for this time lag is briefly discussed. 14 refs., 8 figs., 1 tab.

  16. Western Wind and Solar Integration Study Phase 3A: Low Levels of Synchronous Generation

    SciTech Connect (OSTI)

    Miller, Nicholas W.; Leonardi, Bruno; D'Aquila, Robert; Clark, Kara

    2015-11-17

    The stability of the North American electric power grids under conditions of high penetrations of wind and solar is a significant concern and possible impediment to reaching renewable energy goals. The 33% wind and solar annual energy penetration considered in this study results in substantial changes to the characteristics of the bulk power system. This includes different power flow patterns, different commitment and dispatch of existing synchronous generation, and different dynamic behavior from wind and solar generation. The Western Wind and Solar Integration Study (WWSIS), sponsored by the U.S. Department of Energy, is one of the largest regional solar and wind integration studies to date. In multiple phases, it has explored different aspects of the question: Can we integrate large amounts of wind and solar energy into the electric power system of the West? The work reported here focused on the impact of low levels of synchronous generation on the transient stability performance in one part of the region in which wind generation has displaced synchronous thermal generation under highly stressed, weak system conditions. It is essentially an extension of WWSIS-3. Transient stability, the ability of the power system to maintain synchronism among all elements following disturbances, is a major constraint on operations in many grids, including the western U.S. and Texas systems. These constraints primarily concern the performance of the large-scale bulk power system. But grid-wide stability concerns with high penetrations of wind and solar are still not thoroughly understood. This work focuses on 'traditional' fundamental frequency stability issues, such as maintaining synchronism, frequency, and voltage. The objectives of this study are to better understand the implications of low levels of synchronous generation and a weak grid on overall system performance by: 1) Investigating the Western Interconnection under conditions of both high renewable generation (e.g., wind and solar) and low synchronous generation (e.g., significant coal power plant decommitment or retirement); and 2) Analyzing both the large-scale stability of the Western Interconnection and regional stability issues driven by more geographically dispersed renewable generation interacting with a transmission grid that evolved with large, central station plants at key nodes. As noted above, the work reported here is an extension of the research performed in WWSIS-3.

  17. THIRD MOMENTS AND THE ROLE OF ANISOTROPY FROM VELOCITY SHEAR IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Stawarz, Joshua E.; Vasquez, Bernard J.; Smith, Charles W.; Forman, Miriam A.; Klewicki, Joseph E-mail: Bernie.Vasquez@unh.edu E-mail: Miriam.Forman@sunysb.edu

    2011-07-20

    We have extended the recent analyses of magnetohydrodynamic third moments as they relate to the turbulent energy cascade in the solar wind to consider the effects of large-scale shear flows. Moments from a large set of Advanced Composition Explorer data have been taken, and chosen data intervals are characterized by the rate of change in the solar wind speed. Mean dissipation rates are obtained in accordance with the predictions of homogeneous shear-driven turbulence. Agreement with predictions is best made for rarefaction intervals where the solar wind speed is decreasing with time. For decreasing speed intervals, we find that the dissipation rates increase with increasing shear magnitude and that the shear-induced fluctuation anisotropy is consistent with a relatively small amount.

  18. Anomalous Viscosity, Resistivity, and Thermal Diffusivity of the Solar Wind Plasma

    E-Print Network [OSTI]

    Mahendra K. Verma

    1995-09-05

    In this paper we have estimated typical anomalous viscosity, resistivity, and thermal difffusivity of the solar wind plasma. Since the solar wind is collsionless plasma, we have assumed that the dissipation in the solar wind occurs at proton gyro radius through wave-particle interactions. Using this dissipation length-scale and the dissipation rates calculated using MHD turbulence phenomenology [{\\it Verma et al.}, 1995a], we estimate the viscosity and proton thermal diffusivity. The resistivity and electron's thermal diffusivity have also been estimated. We find that all our transport quantities are several orders of magnitude higher than those calculated earlier using classical transport theories of {\\it Braginskii}. In this paper we have also estimated the eddy turbulent viscosity.

  19. Small-scale anisotropy and intermittency in high and low-latitude solar wind

    E-Print Network [OSTI]

    A. Bigazzi; L. Biferale; S. M. A. Gama; M. Velli

    2004-12-14

    We analyze low and high--latitude fast solar wind data from the Ulysses spacecraft from 1992 to 1994 using a a systematic method to analyse the anisotropic content of the magnetic field fluctuations. We investigate all available frequencies, 1-10^{-6} Hz, for both high and low--latitudes datasets and are able to quantify the relative importance of the anisotropic versus the isotropic fluctuations. We analyse, up to sixth order, longitudinal, transverse and mixed magnetic field correlations. Our results show that strongly intermittent and anisotropic events are present in the solar wind plasma at high frequencies/small scales, indicating the absence of a complete recovery of isotropy. Anisotropic scaling properties are compatible for high and low--latitude data, suggesting a universal behaviour in spite of the different rate of evolution of the fast solar wind streams in the two environments.

  20. Nonlinear interaction of proton whistler with kinetic Alfvén wave to study solar wind turbulence

    SciTech Connect (OSTI)

    Goyal, R.; Sharma, R. P.; Goldstein, M. L.; Dwivedi, N. K.

    2013-12-15

    This paper presents the nonlinear interaction between small but finite amplitude kinetic Alfvén wave (KAW) and proton whistler wave using two-fluid model in intermediate beta plasma, applicable to solar wind. The nonlinearity is introduced by modification in the background density. This change in density is attributed to the nonlinear ponderomotive force due to KAW. The solutions of the model equations, governing the nonlinear interaction (and its effect on the formation of localized structures), have been obtained using semi-analytical method in solar wind at 1AU. It is concluded that the KAW properties significantly affect the threshold field required for the filament formation and their critical size (for proton whistler). The magnetic and electric field power spectra have been obtained and their relevance with the recent observations of solar wind turbulence by Cluster spacecraft has been pointed out.

  1. Seasonal and solar cycle variations in high-latitude thermospheric winds

    SciTech Connect (OSTI)

    Aruliah, A.L.; Rees, D. (University Coll., London (United Kingdom)); Steen, A. (Inst. for Rymdfysik, Kiruna (Sweden))

    1991-11-01

    Thermospheric wind measurements have been collected systematically every winter for over nine years from a high-latitude site at Kiruna, Sweden (67.8{degree}N, 20.4{degree}E). The database contains 1,242 nights of data collected with a Fabry-Perot Interferometer (FPI), perhaps the largest single-site database of thermospheric winds. This analysis shows a marked seasonal and solar cycle variation. Particularly at high solar activity, sunward winds of the evening period (16-20 UT) are more than 50% stronger at Spring than at Autumn equinox. This large asymmetry in the behavior of high-latitude thermospheric winds at spring and autumn equinox has not yet been predicted by model simulations.

  2. Property Tax Exemption for Solar and Wind Energy Systems

    Broader source: Energy.gov [DOE]

    In May 2009 the exemption was amended yet again by H.B. 1171 to add "residential wind energy equipment" as an eligible technology. In order to qualify, equipment must be sited on residential...

  3. Fluctuations in the interplanetary electric potential and energy coupling between the solar-wind and the magnetosphere

    E-Print Network [OSTI]

    Badruddin,

    2013-01-01

    We utilize solar rotation average geomagnetic index ap and various solar wind plasma and field parameters for four solar cycles 20-23. We perform analysis to search for a best possible coupling function at 27-day time resolution. Regression analysis using these data at different phases of solar activity (increasing including maximum/decreasing including minimum) led us to suggest that the time variation of interplanetary electric potential is a better coupling function for solar wind-magnetosphere coupling. We suspect that a faster rate of change in interplanetary electric potential at the magnetopause might enhance the reconnection rate and energy transfer from the solar wind into the magnetosphere. The possible mechanism that involves the interplanetary potential fluctuations in influencing the solar wind-magnetosphere coupling is being investigated.

  4. Turbulence-Driven Coronal Heating and Improvements to Empirical Forecasting of the Solar Wind

    E-Print Network [OSTI]

    Woolsey, Lauren N

    2014-01-01

    Forecasting models of the solar wind often rely on simple parameterizations of the magnetic field that ignore the effects of the full magnetic field geometry. In this paper, we present the results of two solar wind prediction models that consider the full magnetic field profile and include the effects of Alfv\\'en waves on coronal heating and wind acceleration. The one-dimensional MHD code ZEPHYR self-consistently finds solar wind solutions without the need for empirical heating functions. Another 1D code, introduced in this paper (The Efficient Modified-Parker-Equation-Solving Tool, TEMPEST), can act as a smaller, stand-alone code for use in forecasting pipelines. TEMPEST is written in Python and will become a publicly available library of functions that is easy to adapt and expand. We discuss important relations between the magnetic field profile and properties of the solar wind that can be used to independently validate prediction models. ZEPHYR provides the foundation and calibration for TEMPEST, and ultim...

  5. INTERMITTENCY OF SOLAR WIND DENSITY FLUCTUATIONS FROM ION TO ELECTRON SCALES

    SciTech Connect (OSTI)

    Chen, C. H. K.; Sorriso-Valvo, L.; Šafránková, J.; N?me?ek, Z.

    2014-07-01

    The intermittency of density fluctuations in the solar wind at kinetic scales has been examined using high time resolution Faraday cup measurements from the Spektr-R spacecraft. It was found that the probability density functions (PDFs) of the fluctuations are highly non-Gaussian over this range, but do not show large changes in shape with scale. These properties are statistically similar to those of the magnetic fluctuations and are important to understanding the dynamics of small scale turbulence in the solar wind. Possible explanations for the behavior of the density and magnetic fluctuations are discussed.

  6. Effect of wind speed on the growth of the upper convective zone in a solar pond 

    E-Print Network [OSTI]

    McMinn, Steven Lee

    1990-01-01

    EFFECT OF WIND SPEED ON THE GROWTH OF THE UPPER CONVECTIVE ZONE IN A SOLAR POND A Thesis by STEVEN LEE MCMINN Submitted to the Office of Graduate Studies of Texas ASM University in partial fulfillment of the requirements for the degree... of MASTER OF SCIENCE December 1990 Major Subject: Mechanical Engineering EFFECT OF WIND SPEED ON THE GROWTH OF THE UPPER CONVECTIVE ZONE IN A SOLAR POND A Thesis by STEVEN LEE MCMINN Approved as to style and content by: W. R. Laster (Chair...

  7. Depth profiling analysis of solar wind helium collected in diamond-like carbon film from Genesis

    SciTech Connect (OSTI)

    Bajo, Ken-ichi; Olinger, Chad T.; Jurewicz, Amy J.G.; Burnett, Donald S.; Sakaguchi, Isao; Suzuki, Taku; Itose, Satoru; Ishihara, Morio; Uchino, Kiichiro; Wieler, Rainer; Yurimoto, Hisayoshi

    2015-10-01

    The distribution of solar-wind ions in Genesis mission collectors, as determined by depth profiling analysis, constrains the physics of ion solid interactions involving the solar wind. Thus, they provide an experimental basis for revealing ancient solar activities represented by solar-wind implants in natural samples. We measured the first depth profile of ?He in a collector; the shallow implantation (peaking at <20 nm) required us to use sputtered neutral mass spectrometry with post-photoionization by a strong field. The solar wind He fluence calculated using depth profiling is ~8.5 x 10¹? cm?². The shape of the solar wind ?He depth profile is consistent with TRIM simulations using the observed ?He velocity distribution during the Genesis mission. It is therefore likely that all solar-wind elements heavier than H are completely intact in this Genesis collector and, consequently, the solar particle energy distributions for each element can be calculated from their depth profiles. Ancient solar activities and space weathering of solar system objects could be quantitatively reproduced by solar particle implantation profiles.

  8. Western Wind and Solar Integration Study Phase 3 -- Frequency Response and Transient Stability (Report and Executive Summary)

    SciTech Connect (OSTI)

    Miller, N. W.; Shao, M.; Pajic, S.; D'Aquila, R.

    2014-12-01

    The primary objectives of Phase 3 of the Western Wind and Solar Integration Study (WWSIS-3) were to examine the large-scale transient stability and frequency response of the Western Interconnection with high wind and solar penetration, and to identify means to mitigate any adverse performance impacts via transmission reinforcements, storage, advanced control capabilities, or other alternatives.

  9. Energetic electrons, 50 keV 6 MeV, at geosynchronous orbit: their responses to solar wind variations

    E-Print Network [OSTI]

    Li, Xinlin

    1 Energetic electrons, 50 keV ­ 6 MeV, at geosynchronous orbit: their responses to solar wind Short title: ENERGETIC ELECTRONS AT GEOSYNCHRONOUS ORBIT #12;2 Abstract. Using simultaneous measurements of the upstream solar wind and of energetic electrons at geosynchronous orbit, we analyze the response

  10. E-LETTER Earth Planets Space, 65, e5e8, 2013 Doppler shift and broadening in solar wind turbulence

    E-Print Network [OSTI]

    and broadening using magnetic field data in solar wind turbulence. A model of the energy spectrum is constructedE-LETTER Earth Planets Space, 65, e5­e8, 2013 Doppler shift and broadening in solar wind turbulence extraterrestrische Physik, Technische Universit¨at Braunschweig, Mendelssohnstr. 3, D-38106, Germany 3Max

  11. Effects of solar wind magnetosphere coupling recorded at different geomagnetic latitudes: Separation of directly-driven and storage/

    E-Print Network [OSTI]

    Lockwood, Mike

    Effects of solar wind magnetosphere coupling recorded at different geomagnetic latitudes: Separation of directly-driven and storage/ release systems I. D. Finch,1 M. L. Lockwood,1,2 and A. P November 2008. [1] The effect on geomagnetic activity of solar wind speed, compared

  12. Integration Costs: Are They Unique to Wind and Solar Energy? Preprint

    SciTech Connect (OSTI)

    Milligan, M.; Hodge, B.; Kirby, B.; Clark, C.

    2012-05-01

    Over the past several years, there has been considerable interest in assessing wind integration costs. This is understandable because wind energy does increase the variability and uncertainty that must be managed on a power system. However, there are other sources of variability and uncertainty that also must be managed in the power system. This paper describes some of these sources and shows that even the introduction of base-load generation can cause additional ramping and cycling. The paper concludes by demonstrating that integration costs are not unique to wind and solar, and should perhaps instead be assessed by power plant and load performance instead of technology type.

  13. A WIND TUNNEL INVESTIGATION OF THE INFLUENCE OF SOLAR-INDUCED WALL-HEATING ON THE FLOW REGIME

    E-Print Network [OSTI]

    Savory, Eric

    -section canyon model in a wind tunnel. For reference purposes, the neutral case (no wall heating), has also been viscosity of air (m2 s-1 ) 1. Introduction The wind flow field within urban areas has been studiedA WIND TUNNEL INVESTIGATION OF THE INFLUENCE OF SOLAR-INDUCED WALL-HEATING ON THE FLOW REGIME

  14. Observation and modeling of geocoronal charge exchange X-ray emission during solar wind gusts

    SciTech Connect (OSTI)

    Wargelin, B. J.; Kornbleuth, M.; Juda, M.; Martin, P. L.

    2014-11-20

    Solar wind charge exchange (SWCX) X-rays are emitted when highly charged solar wind ions such as O{sup 7{sup +}} collide with neutral gas, including the Earth's tenuous outer atmosphere (exosphere or geocorona) and hydrogen and helium from the local interstellar medium drifting through the heliosphere. This geocoronal and heliospheric emission comprises a significant and varying fraction of the soft X-ray background (SXRB) and is seen in every X-ray observation, with the intensity dependent on solar wind conditions and observation geometry. Under the right conditions, geocoronal emission can increase the apparent SXRB by roughly an order of magnitude for an hour or more. In this work, we study a dozen occasions when the near-Earth solar wind flux was exceptionally high. These gusts of wind lead to abrupt changes in SWCX X-ray emission around Earth, which may or may not be seen by X-ray observatories depending on their line of sight. Using detailed three-dimensional magnetohydrodynamical simulations of the solar wind's interaction with the Earth's magnetosphere, and element abundances and ionization states measured by ACE, we model the time-dependent brightness of major geocoronal SWCX emission lines during those gusts and compare with changes in the X-ray background measured by the Chandra X-ray Observatory. We find reasonably good agreement between model and observation, with measured geocoronal line brightnesses averaged over 1 hr of up to 136 photons s{sup –1} cm{sup –2} sr{sup –1} in the O VII K? triplet around 564 eV.

  15. HAN Attack Surface and the Open Smart Energy Gateway Project

    E-Print Network [OSTI]

    Searle, Justin

    2014-01-01

    Surface  and  the  Open  Smart   Energy  Gateway  Project  Surface  and  the  Open  Smart   Energy  Gateway  Project  home.       The  Open  Smart  Energy  Gateway  (OpenSEG)  

  16. Measuring the Isotopic Composition of Solar Wind Noble Gases

    E-Print Network [OSTI]

    Floss, Christine

    in meteorites are depleted by many orders of magnitude compared with the solar nebula and, although lunar soils the various components, these gases were extracted using stepped pyrolysis and analyzed in sensitive mass

  17. Hybrid Wind and Solar Electric Systems | Department of Energy

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

    the grid in remote locations. | Photo courtesy of Dave Parsons. Off-Grid or Stand-Alone Renewable Energy Systems Whether a home solar electric system will work for you depends on...

  18. GEOPHYSICAL RESEARCH LETTERS, VOL. 0, NO. 0, PAGES 0-0, M 0, 2000 Three spacecraft observations of solar wind discontinuities

    E-Print Network [OSTI]

    Horbury, Tim

    of solar wind discontinuities Timothy S. Horbury,1 David Burgess, and Markus Fr¨anz Astronomy Unit, Queen

  19. Whistler mode waves and the electron heat flux in the solar wind: cluster observations

    SciTech Connect (OSTI)

    Lacombe, C.; Alexandrova, O.; Cornilleau-Wehrlin, N.; Mangeney, A.; De Conchy, Y.; Maksimovic, M.; Matteini, L.; Santolík, O.

    2014-11-20

    The nature of the magnetic field fluctuations in the solar wind between the ion and electron scales is still under debate. Using the Cluster/STAFF instrument, we make a survey of the power spectral density and of the polarization of these fluctuations at frequencies f in [1, 400] Hz, during five years (2001-2005), when Cluster was in the free solar wind. In ?10% of the selected data, we observe narrowband, right-handed, circularly polarized fluctuations, with wave vectors quasi-parallel to the mean magnetic field, superimposed on the spectrum of the permanent background turbulence. We interpret these coherent fluctuations as whistler mode waves. The lifetime of these waves varies between a few seconds and several hours. Here, we present, for the first time, an analysis of long-lived whistler waves, i.e., lasting more than five minutes. We find several necessary (but not sufficient) conditions for the observation of whistler waves, mainly a low level of background turbulence, a slow wind, a relatively large electron heat flux, and a low electron collision frequency. When the electron parallel beta factor ? {sub e?} is larger than 3, the whistler waves are seen along the heat flux threshold of the whistler heat flux instability. The presence of such whistler waves confirms that the whistler heat flux instability contributes to the regulation of the solar wind heat flux, at least for ? {sub e?} ? 3, in slow wind at 1 AU.

  20. The climatological relationships between wind and solar energy supply in Britain

    E-Print Network [OSTI]

    Bett, Philip E

    2015-01-01

    We use reanalysis data to investigate the daily co-variability of wind and solar irradiance in Britain, and its implications for renewable energy supply balancing. The joint distribution of daily-mean wind speeds and irradiances shows that irradiance has a much stronger seasonal cycle than wind, due to the rotational tilt of the Earth. Irradiance is weakly anticorrelated with wind speed throughout the year ($-0.4 \\lesssim \\rho \\lesssim -0.2$): there is a weak tendency for windy days to be cloudier. This is particularly true in Atlantic-facing regions (western Scotland, south-west England). The east coast of Britain has the weakest anticorrelation, particularly in winter, primarily associated with a relative increase in the frequency of clear-but-windy days. We also consider the variability in total power output from onshore wind turbines and solar photovoltaic panels. In all months, daily variability in total power is always reduced by incorporating solar capacity. The scenario with the least seasonal variabi...

  1. The Global Solar and Wind Atlas: a unique Global Spatial Data Infrastructure for all renewable energy

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    @masdar.ac.ae Nicolas Fichaux International Renewable Energy Agency - IRENA Abu Dhabi United Arab Emirates NFichaux in the field of solar and wind energy. The initiative will be expanded to encompass all renewable energies by 2015, and will be the largest information source on renewable energy potentials ever created. It has

  2. An event-based approach to validating solar wind speed predictions: High-speed

    E-Print Network [OSTI]

    California at Berkeley, University of

    December 2005. [1] One of the primary goals of the Center for Integrated Space Weather Modeling (CISM for the Center for Integrated Space Weather Modeling (CISM) solar wind models and suggest an event-based approach-Sheeley-Arge Model [3] CISM is using the Wang-Sheeley-Arge model (WSA) [Arge and Pizzo, 2000; Arge et al., 2003

  3. Value of Geographic Diversity of Wind and Solar: Stochastic Geometry Approach; Preprint

    SciTech Connect (OSTI)

    Diakov, V.

    2012-08-01

    Based on the available geographically dispersed data for the continental U.S. (excluding Alaska), we analyze to what extent the geographic diversity of these resources can offset their variability. A geometric model provides a convenient measure for resource variability, shows the synergy between wind and solar resources.

  4. Solar Wind Particle Distribution Function Fitted via the Generalized Kappa Distribution Function: Cluster

    E-Print Network [OSTI]

    Carlson, Charles W.

    Solar Wind Particle Distribution Function Fitted via the Generalized Kappa Distribution Function Maxwellian distributions as it would be expected for a quasi-collisionless plasma. However, the presence of high energy tail and shoulders in the profile of distribution function stimulate to look for a better

  5. Understanding electron heat flux signatures in the solar wind N. U. Crooker,1

    E-Print Network [OSTI]

    California at Berkeley, University of

    continuously modify heat flux. This is inconsistent with magnetic disconnection as the primary cause of heat most of the heat flux away from the Sun due to their high mobility. The rate at which heat flux dropsUnderstanding electron heat flux signatures in the solar wind C. Pagel,1 N. U. Crooker,1 D. E

  6. Systematic Measurements of Ion-Proton Differential Streaming in the Solar Wind

    SciTech Connect (OSTI)

    Berger, L.; Wimmer-Schweingruber, R. F.; Gloeckler, G. [Extraterrestrial Physics, Institute for Experimental and Applied Physics, Christian-Albrechts-University Kiel, Leibnizstrasse 11-19, 24118 Kiel (Germany); Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Ann Arbor, Michigan 48109-2143 (United States)

    2011-04-15

    The small amount of heavy ions in the highly rarefied solar wind are sensitive tracers for plasma-physics processes, which are usually not accessible in the laboratory. We have analyzed differential streaming between heavy ions and protons in the solar wind at 1 AU. 3D velocity vector and magnetic field measurements from the Solar Wind Electron Proton Alpha Monitor and the Magnetometer aboard the Advanced Composition Explorer were used to reconstruct the ion-proton difference vector v{sub ip}=v{sub i}-v{sub p} from the 12 min 1D Solar Wind Ion Composition Spectrometer observations. We find that all 44 analyzed heavy ions flow along the interplanetary magnetic field at velocities which are smaller than, but comparable to, the local Alfven speed C{sub A}. The flow speeds of 35 of the 44 ion species lie within the range of {+-}0.15C{sub A} around 0.55C{sub A}, the flow speed of He{sup 2+}.

  7. Proposed model for Saturn's auroral response to the solar wind: Centrifugal instability model

    E-Print Network [OSTI]

    Richardson, John

    Proposed model for Saturn's auroral response to the solar wind: Centrifugal instability model E. C in the intensity of Saturn Kilometric Radiation (SKR). Our model, referred to as the centrifugal instability model by centrifugally driven flux tube interchange motions, when the magnetosphere spins up, outward transport

  8. Pierre’s Prototype for Wind and Solar- Capitol Lake Plaza

    Broader source: Energy.gov [DOE]

    Capitol Lake Plaza sits centrally on Pierre, S.D.’s government plaza. Originally built in 1974, the building has been undergoing major energy renovations since being purchased by the state two years ago. Two major components of the renovation are about to appear at the building’s highest point: solar panels and wind turbines are being installed on the roof.

  9. NREL Energy Models Examine the Potential for Wind and Solar Grid Integration (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2013-11-01

    As renewable energy generating sources, such as wind turbines and solar power systems, reach high levels of penetration in parts of the United States, the National Renewable Energy Laboratory (NREL) is helping the utility industry to peer into the future. Using software modeling tools that the lab developed, NREL is examining the future operation of the electrical grid as renewable energy continues to grow.

  10. Langmuir wave-packet generation from an electron beam propagating in the inhomogeneous solar wind.

    E-Print Network [OSTI]

    California at Berkeley, University of

    Langmuir wave-packet generation from an electron beam propagating in the inhomogeneous solar wind of an electron beam in an homogeneous plasma leads to the generation of Lang- muir waves, that are electrostatic of the generation of plasma waves during type III radio bursts or close to the electron foreshock. It is also known

  11. Electron and proton heating by solar wind turbulence B. Breech,1

    E-Print Network [OSTI]

    Oughton, Sean

    magnetohydrodynamic (MHD) turbulence are generalized to incorporate separate internal energy equations for electronsElectron and proton heating by solar wind turbulence B. Breech,1 W. H. Matthaeus,2 S. R. Cranmer,3 and protons. Electron heat conduction is included. Energy is supplied by turbulent heating that affects both

  12. Magnetic fields at the solar wind termination shock L. F. Burlaga1

    E-Print Network [OSTI]

    Richardson, John

    LETTERS Magnetic fields at the solar wind termination shock L. F. Burlaga1 , N. F. Ness2 , M. H and dynamics of the termination shock, made by Voyager 2 on 31 August­1 September 2007 at a distance of 83.7 AU') at the shock. This Letter discusses three termination shock crossings (TS-2, TS- 3 and TS-4) that were observed

  13. THE DYNAMIC QUIET SUN: CONTRIBUTION TO CORONAL HEATING ANF SOLAR WIND

    E-Print Network [OSTI]

    THE DYNAMIC QUIET SUN: CONTRIBUTION TO CORONAL HEATING ANF SOLAR WIND Maria Madjarska Wednesday, September 19, 2012 #12;The dynamic Sun at all scales Wednesday, September 19, 2012 #12;The dynamic Sun at all scales Wednesday, September 19, 2012 #12;The dynamic Sun at all scales Wednesday, September 19

  14. Impacts of Wind and Solar on Fossil-Fueled Generators: Preprint

    SciTech Connect (OSTI)

    Lew, D.; Brinkman, G.; Kumar, N.; Besuner, P.; Agan, D.; Lefton, S.

    2012-08-01

    High penetrations of wind and solar power will impact the operations of the remaining generators on the power system. Regional integration studies have shown that wind and solar may cause fossil-fueled generators to cycle on and off and ramp down to part load more frequently and potentially more rapidly. Increased cycling, deeper load following, and rapid ramping may result in wear-and-tear impacts on fossil-fueled generators that lead to increased capital and maintenance costs, increased equivalent forced outage rates, and degraded performance over time. Heat rates and emissions from fossil-fueled generators may be higher during cycling and ramping than during steady-state operation. Many wind and solar integration studies have not taken these increased cost and emissions impacts into account because data have not been available. This analysis considers the cost and emissions impacts of cycling and ramping of fossil-fueled generation to refine assessments of wind and solar impacts on the power system.

  15. The Local Energy Indicator: Designing for Wind and Solar Energy Systems in the Home

    E-Print Network [OSTI]

    Paulos, Eric

    The Local Energy Indicator: Designing for Wind and Solar Energy Systems in the Home James Pierce energy for interactive systems design. We characterize local energy in terms of three themes: contextuality, seasonality, and visibility/tangibility. Here we focus on two specific local energy technologies

  16. Solar wind oscillations with a 1.3 year period John D. Richardson, Karolen I. Paularena, John W. Belcher, and Alan J. Lazaru

    E-Print Network [OSTI]

    Richardson, John

    Solar wind oscillations with a 1.3 year period s C John D. Richardson, Karolen I. Paularena, John W Abstract. The IMP-8 and Voyager 2 spacecraft have ecently detected a very strong modulation in the solar. Introduction The Sun emits a continuous stream of ionized particles s d called the solar wind. This wind

  17. A New Model for the Prediction of Dst on the Basis of the Solar Wind Space Sciences Lab., University of California, Berkeley

    E-Print Network [OSTI]

    Li, Xinlin

    1 A New Model for the Prediction of Dst on the Basis of the Solar Wind M. Temerin Space Sciences on solar wind data for the years 1995-1999 gives a good fit with a prediction efficiency of 88%, a linear and a term proportional to the square root of the solar wind dynamic pressure is added to give the predicted

  18. arXiv:0710.0763v1[astro-ph]3Oct2007 Small scale energy cascade of the solar wind turbulence

    E-Print Network [OSTI]

    Alexandrova, Olga

    arXiv:0710.0763v1[astro-ph]3Oct2007 Small scale energy cascade of the solar wind turbulence O depends neither on the energy injection nor on the energy dissipation processes. In the solar wind/CNR, Ponte P. Bucci, Cubo 33B, 87036 Rende (CS), Italy ABSTRACT Magnetic fluctuations in the solar wind

  19. Features of a fully renewable US electricity system: Optimized mixes of wind and solar PV and transmission grid extensions

    E-Print Network [OSTI]

    Becker, Sarah; Andresen, Gorm B; Zeyer, Timo; Schramm, Stefan; Greiner, Martin; Jacobson, Mark Z

    2014-01-01

    Wind and solar PV generation data for the entire contiguous US are calculated, on the basis of 32 years of weather data with temporal resolution of one hour and spatial resolution of 40x40km$^2$, assuming site-suitability-based as well as stochastic wind and solar PV capacity distributions throughout the country. These data are used to investigate a fully renewable electricity system, resting primarily upon wind and solar PV power. We find that the seasonal optimal mix of wind and solar PV comes at around 80% solar PV share, owing to the US summer load peak. By picking this mix, long-term storage requirements can be more than halved compared to a wind only mix. The daily optimal mix lies at about 80% wind share due to the nightly gap in solar PV production. Picking this mix instead of solar only reduces backup energy needs by about 50%. Furthermore, we calculate shifts in FERC (Federal Energy Regulatory Commission)-level LCOE (Levelized Costs Of Electricity) for wind and solar PV due to their differing resour...

  20. 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

  1. Influence of Non-Potential Coronal Magnetic Topology on Solar-Wind Models

    E-Print Network [OSTI]

    Edwards, S J; Bocquet, F -X; Mackay, D H

    2015-01-01

    By comparing a magneto-frictional model of the low coronal magnetic field to a potential-field source-surface model, we investigate the possible impact of non-potential magnetic structure on empirical solar-wind models. These empirical models (such as Wang-Sheeley-Arge) estimate the distribution of solar-wind speed solely from the magnetic-field structure in the low corona. Our models are computed in a domain between the solar surface and 2.5 solar radii, and are extended to 0.1 AU using a Schatten current-sheet model. The non-potential field has a more complex magnetic skeleton and quasi-separatrix structures than the potential field, leading to different sub-structure in the solar-wind speed proxies. It contains twisted magnetic structures that can perturb the separatrix surfaces traced down from the base of the heliospheric current sheet. A significant difference between the models is the greater amount of open magnetic flux in the non-potential model. Using existing empirical formulae this leads to higher...

  2. Understanding of solar wind structure might be wrong

    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 - 19 Publicationsresearch reveals the effects ofSolar

  3. Solar and Wind Contractor Licensing | 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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV inSolarLoan to Invest

  4. Solar and Wind Easements, Local Options, and Severability | Department of

    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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV inSolarLoan to

  5. Solar and Wind Energy Business Franchise Tax Exemption | Department of

    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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV inSolarLoan toEnergy

  6. Solar and Wind Energy Credit (Corporate) | 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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV inSolarLoan

  7. Solar and Wind Energy Credit (Personal) | 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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV inSolarLoanPersonal)

  8. Gold SolarWind GmbH | 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 E LIST OFAMERICA'SHeavy ElectricalsFTL SolarGate SolarGijeon Wintec coInc GSE

  9. CORRELATED STUDIES AT ACTIVITY MAXIMUM: THE SUN AND THE SOLAR WIND H. S. Hudson 1 and A. B. Galvin 2

    E-Print Network [OSTI]

    California at Berkeley, University of

    , University of Maryland, College Park, MD 20742, USA ABSTRACT The breadth and power of the set of solar1 CORRELATED STUDIES AT ACTIVITY MAXIMUM: THE SUN AND THE SOLAR WIND H. S. Hudson 1 and A. B at solar minimum or in the declining phase of the past maxi­ mum, but we anticipate that most

  10. Solar Wind Charge Exchange Studies of Highly Charged Ions on Atomic Hydrogen

    SciTech Connect (OSTI)

    Draganic, Ilija N [ORNL; Seely, D. G. [Albion College; McCammon, D [University of Wisconsin, Madison; Havener, Charles C [ORNL

    2011-01-01

    Accurate studies of low energy charge exchange (CX) are critical to understanding underlying soft X ray radiation processes in the interaction of highly charged ions from the solar wind with the neutral atoms and molecules in the heliosphere, cometary comas, planetary atmospheres, interstellar winds, etc.. Particularly important are the CX cross sections for bare, H like, and He like ions of C, N, O and Ne, which are the dominant charge states for these heavier elements in the solar wind. Absolute total cross sections for single electron capture by H like ions of C, N, O and fully stripped O ions from atomic hydrogen have been measured in an expanded range of relative collision energies (5 eV u 20 keV u) and compared to previous H oven measurements. The present measurements are performed using a merged beams technique with intense highly charged ion beams extracted from a 14.5 GHz ECR ion source installed on a high voltage platform at the Oak Ridge National Laboratory. For the collision energy range of 0.3 keV u 3.3 keV u, which corresponds to typical ion velocities in the solar wind, the new measurements are in good agreement with previous H oven measurements. The experimental results are discussed in detail and compared with theoretical calculations where available.

  11. Solar Wind Charge Exchange Studies Of Highly Charged Ions On Atomic Hydrogen

    SciTech Connect (OSTI)

    Draganic, I. N.; Havener, C. C. [Physics Division, Oak Ridge National Laboratory, Oak Ridge, TN 37831 (United States); Seely, D. G. [Department of Physics, Albion College, Albion, MI 49224 (United States); McCammon, D. [Department of Physics, University of Wisconsin, Madison, WI 53706 (United States)

    2011-06-01

    Accurate studies of low-energy charge exchange (CX) are critical to understanding underlying soft X-ray radiation processes in the interaction of highly charged ions from the solar wind with the neutral atoms and molecules in the heliosphere, cometary comas, planetary atmospheres, interstellar winds, etc.. Particularly important are the CX cross sections for bare, H-like, and He-like ions of C, N, O and Ne, which are the dominant charge states for these heavier elements in the solar wind. Absolute total cross sections for single electron capture by H-like ions of C, N, O and fully-stripped O ions from atomic hydrogen have been measured in an expanded range of relative collision energies (5 eV/u-20 keV/u) and compared to previous H-oven measurements. The present measurements are performed using a merged-beams technique with intense highly charged ion beams extracted from a 14.5 GHz ECR ion source installed on a high voltage platform at the Oak Ridge National Laboratory. For the collision energy range of 0.3 keV/u-3.3 keV/u, which corresponds to typical ion velocities in the solar wind, the new measurements are in good agreement with previous H-oven measurements. The experimental results are discussed in detail and compared with theoretical calculations where available.

  12. Edison Solar & Wind Ltd | 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 SECTIONRobertsdale, AlabamaETEC GmbH Jump to:Providence,New Mexico: Energy ResourcesMaterial TechnologyWind

  13. Solar and Wind Equipment Sales Tax Exemption | 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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PVEquipment Sales Tax

  14. Solar, Wind, and Energy Efficiency Easements and Rights Laws | Department

    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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PVEquipment Salesof

  15. Third Sun Solar and Wind Power | 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 JEnvironmental Jump to:EA EISTJThin Film Solar Technologies Jump to: navigation,

  16. Solar wind suprathermal electron Stahl widths across high-speed stream structures

    SciTech Connect (OSTI)

    Skoug, Ruth M [Los Alamos National Laboratory; Steinberg, John T [Los Alamos National Laboratory; Goodrich, Katherine A [Los Alamos National Laboratory; Anderson, Brett R [DARTMUTH UNIV.

    2011-01-03

    Suprathermal electrons (100-1500 eV) observed in the solar wind typically show a strahl distribution, that is, a beam directed away from the Sun along the magnetic field direction. The strahl width observed at 1 AU is highly variable, ranging from 10-70 degrees. The obsenred finite width of the strahl results from the competition between beam focusing as the interplanetary magnetic field strength drops with distance from the Sun, and pitch-angle scattering as the beam interacts with the solar wind plasma in transit from the sun. Here we examine strahl width, observed with ACE SWEPAM across high-speed stream structures to investigate variations in electron scattering as a function of local plasma characteristics. We find that narrow strahls (less than 20 degrees wide), indicating reduced scattering, are observed within high-speed streams. Narrow strahls are also observed in both very low temperature solar wind, in association with ICMEs. Case studies of high-speed streams typically show the strahl narrowing at the leading edge of the stream. In some cases, the strahl narrows at the reverse shock or pressure wave, in other cases at the stream interface. The narrowing can either occur discontinuously or gradually over a period of hours. Within the high-speed wind, the strahl remains narrow for a period of hours to days, and then gradually broadens. The strahl width is roughly constant at all energies across these structures. For some fraction of high-speed streams, counterstreaming is associated with passage of the corotating interaction region. In these cases, we find the widths of the two counterstreaming beams frequently differ by more than 40 degrees. This dramatic difference in strahl width contrasts with observations in the solar wind as a whole, in which counterstreaming strahls typically differ in width by less than 20 degrees.

  17. Chaotic mean wind in turbulent thermal convection and long-term correlations in solar activity

    E-Print Network [OSTI]

    A. Bershadskii

    2009-12-25

    It is shown that correlation function of the mean wind velocity in a turbulent thermal convection (Rayleigh number $Ra \\sim 10^{11}$) exhibits exponential decay with a very long correlation time, while corresponding largest Lyapunov exponent is certainly positive. These results together with the reconstructed phase portrait indicate presence of a chaotic component in the examined mean wind. Telegraph approximation is also used to study relative contribution of the chaotic and stochastic components to the mean wind fluctuations and an equilibrium between these components has been studied. Since solar activity is based on the thermal convection processes, it is reasoned that the observed solar activity long-term correlations can be an imprint of the mean wind chaotic properties. In particular, correlation function of the daily sunspots number exhibits exponential decay with a very long correlation time and corresponding largest Lyapunov exponent is certainly positive, also relative contribution of the chaotic and stochastic components follows the same pattern as for the convection mean wind.

  18. Validity of the Taylor hypothesis for linear kinetic waves in the weakly collisional solar wind

    SciTech Connect (OSTI)

    Howes, G. G.; Klein, K. G.; TenBarge, J. M.

    2014-07-10

    The interpretation of single-point spacecraft measurements of solar wind turbulence is complicated by the fact that the measurements are made in a frame of reference in relative motion with respect to the turbulent plasma. The Taylor hypothesis—that temporal fluctuations measured by a stationary probe in a rapidly flowing fluid are dominated by the advection of spatial structures in the fluid rest frame—is often assumed to simplify the analysis. But measurements of turbulence in upcoming missions, such as Solar Probe Plus, threaten to violate the Taylor hypothesis, either due to slow flow of the plasma with respect to the spacecraft or to the dispersive nature of the plasma fluctuations at small scales. Assuming that the frequency of the turbulent fluctuations is characterized by the frequency of the linear waves supported by the plasma, we evaluate the validity of the Taylor hypothesis for the linear kinetic wave modes in the weakly collisional solar wind. The analysis predicts that a dissipation range of solar wind turbulence supported by whistler waves is likely to violate the Taylor hypothesis, while one supported by kinetic Alfvén waves is not.

  19. Wireless Gateway Programming Model Qadri Hamarsheh

    E-Print Network [OSTI]

    1 Wireless Gateway Programming Model Qadri Hamarsheh Department of Computer Engineering, Faculty suggests architecture for Wireless Gateway Programming Model that consists of building blocks to solve the technical and business problems of wireless environment. The paper describes various fundamental aspects

  20. Coronal sources and in situ properties of the solar winds sampled by ACE during 1999-2008

    E-Print Network [OSTI]

    Fu, Hui; Li, Xing; Huang, Zhenghua; Mou, Chaozhou; Jiao, Fangran; Xia, Lidong

    2015-01-01

    We identify the coronal sources of the solar winds sampled by the ACE spacecraft during 1999-2008, and examine the in situ solar wind properties as a function of wind sources. The standard two-step mapping technique is adopted to establish the photospheric footpoints of the magnetic flux tubes along which the ACE winds flow. The footpoints are then placed in the context of EIT 284~\\AA\\ images and photospheric magnetograms, allowing us to categorize the sources into four groups: coronal holes (CHs), active regions (ARs), the quiet Sun (QS), and "Undefined". This practice also enables us to establish the response to solar activity of the fractions occupied by each kind of solar winds, and of their speeds and O$^{7+}$/O$^{6+}$ ratios measured in situ. We find that during the maximum phase, the majority of ACE winds originate from ARs. During the declining phase, CHs and ARs are equally important contributors to the ACE solar winds. The QS contribution increases with decreasing solar activity, and maximizes in th...

  1. Solar and Wind Easements & Rights Laws | Department of Energy

    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 Natural GasAdjustmentsShirleyEnergyTher iSlide 1 More Documents &1000radiation, often6 SolarLoan to Invest

  2. Solar and Wind Energy Rebate Program | Department of Energy

    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 Natural GasAdjustmentsShirleyEnergyTher iSlide 1 More Documents &1000radiation, often6 SolarLoanSavings

  3. Solar and Wind Powering Wyoming Home | Department of Energy

    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 Natural GasAdjustmentsShirleyEnergyTher iSlide 1 More Documents &1000radiation, often6 SolarLoanSavings<

  4. NREL: Transmission Grid Integration - Western Wind and Solar 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 Room NewsInformationJessework usesof EnergyY-12WorkingSolarTechnologies AvailableTransfer

  5. Solar, Wind, Hydropower: Home Renewable Energy Installations | Department

    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 RoomPreservation ofAlbuquerque|Sensitive Species3performedValley |Solar PowerofThermalSolarof

  6. Anisotropic MHD Turbulence in the Interstellar Medium and Solar Wind http://scitation.aip.org/getabs/servlet/GetabsServlet?prog=normal&i... 1 of 1 6/18/07 12:12 PM

    E-Print Network [OSTI]

    Ng, Chung-Sang

    Anisotropic MHD Turbulence in the Interstellar Medium and Solar Wind http://scitation, pp. 433-438 SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference Full Text. Anisotropic MHD Turbulence in the Interstellar Medium and Solar Wind A. Bhattacharjee and C. S. Ng Center

  7. Gateway Issue 2 

    E-Print Network [OSTI]

    Multiple Contributors

    1985-01-01

    rooftop lawn. A hot-climate wind tunnel experiment was carried out in order to obtain and analyze the heat and moisture transport in the rooftop lawn. Furthermore, a calculation with the energy conservation equation was carried out using the results...

  8. Suppressing the non-Gaussian statistics of Renewable Power from Wind and Solar

    E-Print Network [OSTI]

    Anvari, M; Tabar, M Reza Rahimi; Wächter, M; Milan, P; Heinemann, D; Peinke, Joachim; Lorenz, E

    2015-01-01

    The power from wind and solar exhibits a nonlinear flickering variability, which typically occurs at time scales of a few seconds. We show that high-frequency monitoring of such renewable powers enables us to detect a transition, controlled by the field size, where the output power qualitatively changes its behaviour from a flickering type to a diffusive stochastic behaviour. We find that the intermittency and strong non-Gaussian behavior in cumulative power of the total field, even for a country-wide installation still survives for both renewable sources. To overcome the short time intermittency, we introduce a time-delayed feedback method for power output of wind farm and solar field that can change further the underlying stochastic process and suppress their strong non- gaussian fluctuations.

  9. Features of a fully renewable US electricity system: Optimized mixes of wind and solar PV and transmission grid extensions

    E-Print Network [OSTI]

    Jacobson, Mark

    in FERC (Federal Energy Regulatory Commission)-level LCOE (Levelized Costs Of Electricity) for wind and solar PV due to differing weather conditions. Regional LCOE vary by up to 29%, and LCOE-optimal mixes

  10. First lunar wake passage of ARTEMIS: Discrimination of wake effects and solar wind fluctuations by 3D hybrid simulations

    E-Print Network [OSTI]

    California at Berkeley, University of

    with the solar wind were found by the IMP-1 satellite (Ness et al., 1964; Ness, 1965). Later, the magnetic field the existence of a lunar wake (Ness et al., 1967). This pioneering mission revealed the low electric

  11. One-point statistics and intermittency of induced electric field in the solar wind

    E-Print Network [OSTI]

    Luca Sorriso-Valvo; Vincenzo Carbone; Roberto Bruno

    2004-05-26

    The interplanetary induced electric field e=vxb is studied, using solar wind time series. The probability distribution functions (PDFs) of the electric field components are measured from the data and their non-gaussianity is discussed. Moreover, for the first time we show that the electric field turbulence is characterized by intermittency. This point is addressed by studying, as usual, the scaling of the PDFs of field increments, which allows a quantitative characterization of intermittency.

  12. Variations in solar wind fractionation as seen by ACE/SWICS over a solar cycle and the implications for Genesis Mission results

    E-Print Network [OSTI]

    Pilleri, P; Zurbuchen, T H; Lepri, S T; Shearer, P; Gilbert, J A; von Steiger, R; Wiens, R C

    2015-01-01

    We use ACE/SWICS elemental composition data to compare the variations in solar wind fractionation as measured by SWICS during the last solar maximum (1999-2001), the solar minimum (2006-2009) and the period in which the Genesis spacecraft was collecting solar wind (late 2001 - early 2004). We differentiate our analysis in terms of solar wind regimes (i.e. originating from interstream or coronal hole flows, or coronal mass ejecta). Abundances are normalized to the low-FIP ion magnesium to uncover correlations that are not apparent when normalizing to high-FIP ions. We find that relative to magnesium, the other low-FIP elements are measurably fractionated, but the degree of fractionation does not vary significantly over the solar cycle. For the high-FIP ions, variation in fractionation over the solar cycle is significant: greatest for Ne/Mg and C/Mg, less so for O/Mg, and the least for He/Mg. When abundance ratios are examined as a function of solar wind speed, we find a strong correlation, with the remarkable ...

  13. Statistical study of reconnection exhausts in the solar wind

    SciTech Connect (OSTI)

    Enžl, J.; P?ech, L.; Šafránková, J.; N?me?ek, Z.

    2014-11-20

    Magnetic reconnection is a fundamental process that changes magnetic field configuration and converts a magnetic energy to flow energy and plasma heating. This paper presents a survey of the plasma and magnetic field parameters inside 418 reconnection exhausts identified in the WIND data from 1995-2012. The statistical analysis is oriented on the re-distribution of the magnetic energy released due to reconnection between a plasma acceleration and its heating. The results show that both the portion of the energy deposited into heat as well as the energy spent on the acceleration of the exhaust plasma rise with the magnetic shear angle in accord with the increase of the magnetic flux available for reconnection. The decrease of the normalized exhaust speed with the increasing magnetic shear suggests a decreasing efficiency of the acceleration and/or the increasing efficiency of heating in high-shear events. However, we have found that the already suggested relation between the exhaust speed and temperature enhancement would be rather considered as an upper limit of the plasma heating during reconnection regardless of the shear angle.

  14. SELF-CONSISTENT ION CYCLOTRON ANISOTROPY-BETA RELATION FOR SOLAR WIND PROTONS

    SciTech Connect (OSTI)

    Isenberg, Philip A.; Maruca, Bennett A.; Kasper, Justin C. E-mail: bmaruca@ssl.berkeley.edu

    2013-08-20

    We derive a set of self-consistent marginally stable states for a system of ion-cyclotron waves propagating parallel to the large-scale magnetic field through a homogeneous proton-electron plasma. The proton distributions and the wave dispersions are related through the condition that no further ion-cyclotron resonant particle scattering or wave growth/damping may take place. The thermal anisotropy of the protons in these states therefore defines the threshold value for triggering the proton-cyclotron anisotropy instability. A number of recent papers have noted that the anisotropy of solar wind protons at 1 AU does not seem to be limited by the proton-cyclotron anisotropy threshold, even at low plasma beta. However, this puzzle seems to be due solely to the estimation of this anisotropy threshold under the assumption that the protons have a bi-Maxwellian distribution. We note that bi-Maxwellian distributions are never marginally stable to the resonant cyclotron interaction, so these estimates do not represent physically valid thresholds. The threshold anisotropies obtained from our marginally stable states are much larger, as a function of proton parallel beta, than the bi-Maxwellian estimates, and we show that the measured data remains below these more rigorous thresholds. Thus, the results of this paper resolve the apparent contradiction presented by the solar wind anisotropy observations at 1 AU: the bi-Maxwellian anisotropies are not rigorous thresholds, and so do not limit the proton distributions in the solar wind.

  15. Variable cascade dynamics and intermittency in the solar wind at 1 AU

    SciTech Connect (OSTI)

    Coburn, Jesse T.; Smith, Charles W.; Vasquez, Bernard J.; Forman, Miriam A.; Stawarz, Julia E. E-mail: Charles.Smith@unh.edu E-mail: Miriam.Forman@sunysb.edu

    2014-05-01

    In recent studies by ourselves and others of third-moment expressions for the rate of energy cascade in the solar wind, it has been shown that relatively large volumes of data are needed to produce convergent averages. These averages are in good agreement with independently obtained estimates for the average heating rate for a solar wind plasma under those conditions. The unanswered question has been whether the convergence issue is the result of intermittent dynamics or simple measurement uncertainties. In other words, is the difficulty in obtaining a single result that characterizes many similarly prepared samples due to in situ dynamics that create physically real variations or simple statistics? There have been publications showing evidence of intermittent dynamics in the solar wind. Here we show that the third-moment expressions and the computed energy cascade for relatively small samples of data comparable to the correlation length are generally well-formed estimates of the local dynamics. This leads us to conclude that intermittency and not simple measurement uncertainties are responsible for the slow convergence to expected heating rates. We partially characterize the scale size of the intermittency to be comparable to or smaller than the correlation length of the turbulence and we attempt to rephrase the discussion of third moments in terms of intermittent dynamics.

  16. The global morphology of the solar wind interaction with comet Churyumov-Gerasimenko

    SciTech Connect (OSTI)

    Mendis, D. A.; Horányi, M.

    2014-10-10

    The forthcoming Rosetta-Philae mission to comet 67P/Churyumov-Gerasimenko provides a novel opportunity to observe the variable nature of the solar wind interaction with a comet over an extended range of heliocentric distance. We use a simple analytical one-dimensional MHD model to estimate the sizes of the two most prominent features in the global structure of the solar wind interaction with a comet. When the heliocentric distance of the comet reaches d ? 1.51 AU, we expect a sharp shock to be observed, whose size would increase monotonically as the comet approaches the Sun, reaching a value ? 15, 000 km at perihelion (d ? 1.29 AU). Upstream of the shock, we expect the velocity-space distribution of the picked up cometary ions to be essentially gyrotropic. A well-defined ionopause is predicted when d ?1.61 AU, though its size is expected to be only ?25 km at perihelion, and it is expected to be susceptible to the 'flute' instability due to its small size. Consequently, we expect the magnetic field to penetrate all the way to the surface of the nucleus. We conclude with a brief discussion of the response of the comet's plasma environment to fast temporal variations in the solar wind.

  17. THE NONLINEAR AND NONLOCAL LINK BETWEEN MACROSCOPIC ALFVÉNIC AND MICROSCOPIC ELECTROSTATIC SCALES IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Valentini, F.; Vecchio, A.; Donato, S.; Carbone, V.; Veltri, P.; Briand, C.; Bougeret, J.

    2014-06-10

    The local heating of the solar-wind gas during its expansion represents one of the most intriguing problems in space plasma physics and is at present the subject of a relevant scientific effort. The possible mechanisms that could account for local heat production in the interplanetary medium are most likely related to the turbulent character of the solar-wind plasma. Nowadays, many observational and numerical analyses are devoted to the identification of fluctuation channels along which energy is carried from large to short wavelengths during the development of the turbulent cascade; these fluctuation channels establish the link between macroscopic and microscopic scales. In this Letter, by means of a quantitative comparison between in situ measurements in the solar wind from the STEREO spacecraft and numerical results from kinetic simulations, we identify an electrostatic channel of fluctuations that develops along the turbulent cascade in a direction parallel to the ambient magnetic field. This channel appears to be efficient in transferring the energy from large Alfvénic to short electrostatic acoustic-like scales up to a range of wavelengths where it can finally be turned into heat, even when the electron to proton temperature ratio is of the order of unity.

  18. THE GENESIS SOLAR WIND CONCENTRATOR TARGET: MASS FRACTIONATION CHARACTERISED BY NE ISOTOPES

    SciTech Connect (OSTI)

    WIENS, ROGER C.; OLINGER, C.; HEBER, V.S.; REISENFELD, D.B.; BURNETT, D.S.; ALLTON, J.H.; BAUR, H.; WIECHERT, U.; WIELER, R.

    2007-01-02

    The concentrator on Genesis provides samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition of the solar wind. The concentration process caused mass fractionation as function of the radial target position. They measured the fractionation using Ne released by UV laser ablation along two arms of the gold cross from the concentrator target to compare measured Ne with modeled Ne. The latter is based on simulations using actual conditions of the solar wind during Genesis operation. Measured Ne abundances and isotopic composition of both arms agree within uncertainties indicating a radial symmetric concentration process. Ne data reveal a maximum concentration factor of {approx} 30% at the target center and a target-wide fractionation of Ne isotopes of 3.8%/amu with monotonously decreasing {sup 20}Ne/{sup 22}Ne ratios towards the center. The experimentally determined data, in particular the isotopic fractionation, differ from the modeled data. They discuss potential reasons and propose future attempts to overcome these disagreements.

  19. Solar wind-magnetosphere coupling during intense magnetic storms (1978--1979)

    SciTech Connect (OSTI)

    Gonzalez, W.D. ); Tsurutani, B.T.; Gonzalez, A.L.C.; Smith, E.J.; Tang, F.; Akasofu, S.

    1989-07-01

    The solar wind-magnetosphere coupling problem is investigated for the ten intense magnetic storms (Dst {lt}{minus}100 nT) that occurred during the 500 days (August 16, 1978 to December 28, 1979) studied by Gonzalez and Tsurutani (1987). This investigation concentrates on the ring current energization in terms of solar wind parameters, in order to explain the {vert bar} {minus}Dst {vert bar} growth observed during these storms. Thus several coupling functions are tested as energy input and several sets of the ring current decay time-constant {tau} are searched to find best correlations with the Dst response. From the fairly large correlation coefficients found in this study, there is strong evidence that large scale magnetopause reconnection operates during such intense storm events and that the solar wind ram pressure plays an important role in the ring current energization. Thus a ram pressure correction factor is suggested for expressions concerning the reconnection power during time intervals with large ram pressure variations.

  20. ON THE LOW-FREQUENCY BOUNDARY OF SUN-GENERATED MAGNETOHYDRODYNAMIC TURBULENCE IN THE SLOW SOLAR WIND

    SciTech Connect (OSTI)

    Shergelashvili, Bidzina M.; Fichtner, Horst

    2012-06-20

    New aspects of the slow solar wind turbulent heating and acceleration are investigated. A physical meaning of the lower boundary of the Alfven wave turbulent spectra in the solar atmosphere and the solar wind is studied and the significance of this natural parameter is demonstrated. Via an analytical and quantitative treatment of the problem we show that a truncation of the wave spectra from the lower frequency side, which is a consequence of the solar magnetic field structure and its cyclic changes, results in a significant reduction of the heat production and acceleration rates. An appropriate analysis is presented regarding the link of the considered problem with existing observational data and slow solar wind initiation scenarios.

  1. Features of a fully renewable US electricity system: Optimized mixes of wind and solar PV and transmission grid extensions

    E-Print Network [OSTI]

    Jacobson, Mark

    . To quantify general features of such a weather dependent electricity supply in the contiguous US, windFeatures of a fully renewable US electricity system: Optimized mixes of wind and solar PV and transmission grid extensions Sarah Becker a, b, * , Bethany A. Frew b , Gorm B. Andresen d, b , Timo Zeyer c

  2. The evolution of 1 AU equatorial solar wind and its association with the morphology of the heliospheric current sheet from solar cycles 23 to 24

    SciTech Connect (OSTI)

    Zhao, L.; Landi, E.; Zurbuchen, T. H.; Fisk, L. A.; Lepri, S. T.

    2014-09-20

    The solar wind can be categorized into three types based on its 'freeze-in' temperature (T {sub freeze-in}) in the coronal source: low T {sub freeze-in} wind mostly from coronal holes, high T {sub freeze-in} wind mostly from regions outside of coronal holes, including streamers (helmet streamer and pseudostreamer), active regions, etc., and transient interplanetary coronal mass ejections (ICMEs) usually possessing the hottest T {sub freeze-in}. The global distribution of these three types of wind has been investigated by examining the most effective T {sub freeze-in} indicator, the O{sup 7+}/O{sup 6+} ratio, as measured by the Solar Wind Ion Composition Spectrometer on board the Advanced Composition Explorer (ACE) during 1998-2008 by Zhao et al. In this study, we extend the previous investigation to 2011 June, covering the unusual solar minimum between solar cycles 23 and 24 (2007-2010) and the beginning of solar cycle 24. We find that during the entire solar cycle, from the ascending phase of cycle 23 in 1998 to the ascending phase of cycle 24 in 2011, the average fractions of the low O{sup 7+}/O{sup 6+} ratio (LOR) wind, the high O{sup 7+}/O{sup 6+} ratio (HOR) wind, and ICMEs at 1 AU are 50.3%, 39.4%, and 10.3%, respectively; the contributions of the three types of wind evolve with time in very different ways. In addition, we compare the evolution of the HOR wind with two heliospheric current sheet (HCS) parameters, which indicate the latitudinal standard deviation (SD) and the slope (SL) of the HCS on the synoptic Carrington maps at 2.5 solar radii surface. We find that the fraction of HOR wind correlates with SD and SL very well (slightly better with SL than with SD), especially after 2005. This result verifies the link between the production of HOR wind and the morphology of the HCS, implying that at least one of the major sources of the HOR wind must be associated with the HCS.

  3. Figure 1. The net load, or power load minus wind and solar generation, for the state of California on March 31.

    E-Print Network [OSTI]

    Nehorai, Arye

    increase in solar and wind installations. This graph, often called a "Duck Curve" in the industry because can have. When a power grid has a large #12;2 amount of solar power capacity, the middle of this curve1 Figure 1. The net load, or power load minus wind and solar generation, for the state

  4. Corotating solar wind structures and recurrent trains of enhanced diurnal variation in galactic cosmic rays

    SciTech Connect (OSTI)

    Yeeram, T.; Ruffolo, D.; Sáiz, A.; Kamyan, N.; Nutaro, T. E-mail: david.ruf@mahidol.ac.th E-mail: p_chang24@hotmail.com

    2014-04-01

    Data from the Princess Sirindhorn Neutron Monitor at Doi Inthanon, Thailand, with a vertical cutoff rigidity of 16.8 GV, were utilized to determine the diurnal anisotropy (DA) of Galactic cosmic rays (GCRs) near Earth during solar minimum conditions between 2007 November and 2010 November. We identified trains of enhanced DA over several days, which often recur after a solar rotation period (?27 days). By investigating solar coronal holes as identified from synoptic maps and solar wind parameters, we found that the intensity and anisotropy of cosmic rays are associated with the high-speed streams (HSSs) in the solar wind, which are in turn related to the structure and evolution of coronal holes. An enhanced DA was observed after the onset of some, but not all, HSSs. During time periods of recurrent trains, the DA was often enhanced or suppressed according to the sign of the interplanetary magnetic field B, which suggests a contribution from a mechanism involving a southward gradient in the GCR density, n, and a gradient anisotropy along B × ?n. In one non-recurrent and one recurrent sequence, an HSS from an equatorial coronal hole was merged with that from a trailing mid-latitude extension of a polar coronal hole, and the slanted HSS structure in space with suppressed GCR density can account for the southward GCR gradient. We conclude that the gradient anisotropy is a source of temporary changes in the GCR DA under solar minimum conditions, and that the latitudinal GCR gradient can sometimes be explained by the coronal hole morphology.

  5. The energy market is diversifying. In addition to traditional power sources, decision makers can choose among solar, wind, and

    E-Print Network [OSTI]

    the steps of analyzing the energy outputs and economics of a solar, wind, or geothermal project. NREL power towers. SAM even calculates the value of saved energy from a domestic solar water heating systeminnovati n The energy market is diversifying. In addition to traditional power sources, decision

  6. Cross polar cap potentials measured with Super Dual Auroral Radar Network during quasi-steady solar wind and interplanetary magnetic

    E-Print Network [OSTI]

    Shepherd, Simon

    Cross polar cap potentials measured with Super Dual Auroral Radar Network during quasi-steady solar, or cross polar cap potential, ÈPC. Periods are chosen to satisfy the criteria that (1) the solar wind-based radars to functional forms of the electrostatic potential [Ruohoniemi and Baker, 1998]; and global mag

  7. Evolution of turbulence in the expanding solar wind, a numerical study

    SciTech Connect (OSTI)

    Dong, Yue; Grappin, Roland; Verdini, Andrea E-mail: verdini@arcetri.astro.it

    2014-10-01

    We study the evolution of turbulence in the solar wind by solving numerically the full three-dimensional (3D) magnetohydrodynamic (MHD) equations embedded in a radial mean wind. The corresponding equations (expanding box model or EBM) have been considered earlier but never integrated in 3D simulations. Here, we follow the development of turbulence from 0.2 AU up to about 1.5 AU. Starting with isotropic spectra scaling as k {sup –1}, we observe a steepening toward a k {sup –5/3} scaling in the middle of the wave number range and formation of spectral anisotropies. The advection of a plasma volume by the expanding solar wind causes a non-trivial stretching of the volume in directions transverse to radial and the selective decay of the components of velocity and magnetic fluctuations. These two effects combine to yield the following results. (1) Spectral anisotropy: gyrotropy is broken, and the radial wave vectors have most of the power. (2) Coherent structures: radial streams emerge that resemble the observed microjets. (3) Energy spectra per component: they show an ordering in good agreement with the one observed in the solar wind at 1 AU. The latter point includes a global dominance of the magnetic energy over kinetic energy in the inertial and f {sup –1} range and a dominance of the perpendicular-to-the-radial components over the radial components in the inertial range. We conclude that many of the above properties are the result of evolution during transport in the heliosphere, and not just the remnant of the initial turbulence close to the Sun.

  8. One-Up On L1: Can X-rays Provide Longer Advanced Warning of Solar Wind Flux Enhancements Than Upstream Monitors?

    E-Print Network [OSTI]

    M. R. Collier; T. E. Moore; S. L. Snowden; K. D. Kuntz

    2005-02-17

    Observations of strong solar wind proton flux correlations with ROSAT X-ray rates along with high spectral resolution Chandra observations of X-rays from the dark Moon show that soft X-ray emission mirrors the behavior of the solar wind. In this paper, based on an analysis of an X-ray event observed by XMM-Newton resulting from charge exchange of high charge state solar wind ions and contemporaneous neutral solar wind data, we argue that X-ray observations may be able to provide reliable advance warning, perhaps by as much as half a day, of dramatic increases in solar wind flux at Earth. Like neutral atom imaging, this provides the capability to monitor the solar wind remotely rather than in-situ.

  9. A STEADY-STATE PICTURE OF SOLAR WIND ACCELERATION AND CHARGE STATE COMPOSITION DERIVED FROM A GLOBAL WAVE-DRIVEN MHD MODEL

    E-Print Network [OSTI]

    Landi, E.

    The higher charge states found in slow (<400 km s[superscript ?1]) solar wind streams compared to fast streams have supported the hypothesis that the slow wind originates in closed coronal loops and is released intermittently ...

  10. STOCHASTIC HEATING, DIFFERENTIAL FLOW, AND THE ALPHA-TO-PROTON TEMPERATURE RATIO IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Chandran, B. D. G.; Verscharen, D.; Isenberg, P. A.; Bourouaine, S.; Quataert, E.; Kasper, J. C. E-mail: s.bourouaine@unh.edu E-mail: daniel.verscharen@unh.edu E-mail: jkasper@cfa.harvard.edu

    2013-10-10

    We extend previous theories of stochastic ion heating to account for the motion of ions along the magnetic field B . We derive an analytic expression for the temperature ratio T{sub i}/T{sub p} in the solar wind assuming that stochastic heating is the dominant ion heating mechanism, where T{sub i} is the perpendicular temperature of species i and T{sub p} is the perpendicular proton temperature. This expression describes how T{sub i}/T{sub p} depends upon U{sub i} and ?{sub ?p}, where U{sub i} is the average velocity along B of species i in the proton frame and ?{sub ?p} is the ratio of the parallel proton pressure to the magnetic pressure, which we take to be ?< 1. We compare our model with previously published measurements of alpha particles and protons from the Wind spacecraft. We find that stochastic heating offers a promising explanation for the dependence of T{sub ?}/T{sub p} on U{sub ?} and ?{sub ?p} when the fractional cross helicity and Alfvén ratio at the proton-gyroradius scale have values that are broadly consistent with solar-wind measurements. We also predict how the temperatures of other ion species depend on their drift speeds.

  11. Radial evolution of the intermittency of density fluctuations in the fast solar wind

    SciTech Connect (OSTI)

    Bruno, R.; D'Amicis, R.; Telloni, D.; Primavera, L.; Sorriso-Valvo, L.; Carbone, V.; Malara, F.; Veltri, P.

    2014-05-01

    We study the radial evolution of the intermittency of density fluctuations in the fast solar wind. The study is performed by analyzing the plasma density measurements provided by Helios 2 in the inner heliosphere between 0.3 and 0.9 AU. The analysis is carried out by means of a complete set of diagnostic tools, including the flatness factor at different timescales to estimate intermittency, the Kolmogorov-Smirnov test to estimate the degree of intermittency, and the Fourier transform to estimate the power spectral densities of these fluctuations. Density fluctuations within the fast wind are rather intermittent and their level of intermittency, together with the amplitude of intermittent events, decreases with the distance from the Sun, at odds with the intermittency of both magnetic field and all other plasma parameters. Furthermore, the intermittent events are strongly correlated, exhibiting temporal clustering. This indicates that the mechanism underlying their generation departs from a time-varying Poisson process. A remarkable, qualitative similarity with the behavior of plasma density fluctuations obtained from a numerical study of the nonlinear evolution of parametric instability in the solar wind supports the idea that this mechanism has an important role in governing density fluctuations in the inner heliosphere.

  12. Impact of dispersed solar and wind systems on electric distribution planning and operation

    SciTech Connect (OSTI)

    Boardman, R.W.; Patton, R.; Curtice, D.H.

    1981-02-01

    Small-scale dispersed solar photovoltaic and wind generation (DSW) will affect the generation, transmission, and distribution systems of an electric utility. This study examines the technical and economic impacts of dispersing DSW devices within the distribution system. Dispersed intermittent generation is included. Effects of DSW devices on capital investments, reliability, operating and maintenance costs, protection requirements, and communication and control requirements are examined. A DSW operation model is developed to help determine the dependable capacity of fluctuating solar photovoltaic and wind generation as part of the distribution planning process. Specific case studies using distribution system data and renewable resource data for Southern California Edison Company and Consumers Power Company are analyzed to gain insights into the effects of interconnecting DSW devices. The DSW devices were found to offer some distribution investment savings, depending on their availability during peak loads. For a summer-peaking utility, for example, dispersing photovoltaic systems is more likely to defer distribution capital investments than dispersing wind systems. Dispersing storage devices to increase DSW's dependable capacity for distribution systems needs is not economically attractive. Substation placement of DSW and storage devices is found to be more cost effective than feeder or customer placement. Examination of the effects of DSW on distribution system operation showed that small customer-owned DSW devices are not likely to disrupt present time-current distribution protection coordination. Present maintenance work procedures, are adequate to ensure workmen's safety. Regulating voltages within appropriate limits will become more complex with intermittent generation along the distribution feeders.

  13. A NEW THREE-DIMENSIONAL SOLAR WIND MODEL IN SPHERICAL COORDINATES WITH A SIX-COMPONENT GRID

    SciTech Connect (OSTI)

    Feng, Xueshang; Zhang, Man; Zhou, Yufen

    2014-09-01

    In this paper, we introduce a new three-dimensional magnetohydrodynamics numerical model to simulate the steady state ambient solar wind from the solar surface to 215 R {sub s} or beyond, and the model adopts a splitting finite-volume scheme based on a six-component grid system in spherical coordinates. By splitting the magnetohydrodynamics equations into a fluid part and a magnetic part, a finite volume method can be used for the fluid part and a constrained-transport method able to maintain the divergence-free constraint on the magnetic field can be used for the magnetic induction part. This new second-order model in space and time is validated when modeling the large-scale structure of the solar wind. The numerical results for Carrington rotation 2064 show its ability to produce structured solar wind in agreement with observations.

  14. Recent Observations of Plasma and Alfvenic Wave Energy Injection at the Base of the Fast Solar Wind

    E-Print Network [OSTI]

    McIntosh, Scott W

    2012-01-01

    We take stock of recent observations that identify the episodic plasma heating and injection of Alfvenic energy at the base of fast solar wind (in coronal holes). The plasma heating is associated with the occurrence of chromospheric spicules that leave the lower solar atmosphere at speeds of order 100km/s, the hotter coronal counterpart of the spicule emits radiation characteristic of root heating that rapidly reaches temperatures of the order of 1MK. Furthermore, the same spicules and their coronal counterparts ("Propagating Coronal Disturbances"; PCD) exhibit large amplitude, high speed, Alfvenic (transverse) motion of sufficient energy content to accelerate the material to high speeds. We propose that these (disjointed) heating and accelerating components form a one-two punch to supply, and then accelerate, the fast solar wind. We consider some compositional constraints on this concept, extend the premise to the slow solar wind, and identify future avenues of exploration.

  15. Your GatewaY

    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 SolarAboutXu Named| Princeton Plasma Physics LabYour

  16. Proton Kinetic Effects and Turbulent Energy Cascade Rate in the Solar Wind

    E-Print Network [OSTI]

    Osman, Kareem T; Kiyani, Khurom H; Hnat, Bogdan; Chapman, Sandra C

    2013-01-01

    The first observed connection between kinetic instabilities driven by proton temperature anisotropy and estimated energy cascade rates in the turbulent solar wind is reported using measurements from the Wind spacecraft at 1 AU. We find enhanced cascade rates are concentrated along the boundaries of the ($\\beta_{\\parallel}$, $T_{\\perp}/T_{\\parallel}$)-plane, which includes regions theoretically unstable to the mirror and firehose instabilities. A strong correlation is observed between the estimated cascade rate and kinetic effects such as temperature anisotropy and plasma heating, resulting in protons 5-6 times hotter and 70-90% more anisotropic than under typical isotropic plasma conditions. These results offer new insights into kinetic processes in a turbulent regime.

  17. Imaging the heliosphere using neutral atoms from solar wind energy down to 15 eV

    SciTech Connect (OSTI)

    Galli, A.; Wurz, P.; Fuselier, S. A.; McComas, D. J.; Bzowski, M.; Sokó?, J. M.; Kubiak, M. A.; Möbius, E.

    2014-11-20

    We study the spatial and temporal distribution of hydrogen energetic neutral atoms (ENAs) from the heliosheath observed with the IBEX-Lo sensor of the Interstellar Boundary EXplorer (IBEX) from solar wind energies down to the lowest available energy (15 eV). All available IBEX-Lo data from 2009 January until 2013 June were included. The sky regions imaged when the spacecraft was outside of Earth's magnetosphere and when the Earth was moving toward the direction of observation offer a sufficient signal-to-noise ratio even at very low energies. We find that the ENA ribbon—a 20° wide region of high ENA intensities—is most prominent at solar wind energies whereas it fades at lower energies. The maximum emission in the ribbon is located near the poles for 2 keV and closer to the ecliptic plane for energies below 1 keV. This shift is an evidence that the ENA ribbon originates from the solar wind. Below 0.1 keV, the ribbon can no longer be identified against the globally distributed ENA signal. The ENA measurements in the downwind direction are affected by magnetospheric contamination below 0.5 keV, but a region of very low ENA intensities can be identified from 0.1 keV to 2 keV. The energy spectra of heliospheric ENAs follow a uniform power law down to 0.1 keV. Below this energy, they seem to become flatter, which is consistent with predictions. Due to the subtraction of local background, the ENA intensities measured with IBEX agree with the upper limit derived from Ly? observations.

  18. Integrating Wind and Solar Energy in the U.S. Bulk Power System: Lessons from Regional Integration Studies

    SciTech Connect (OSTI)

    Bird, L.; Lew, D.

    2012-09-01

    Two recent studies sponsored by the U.S. Department of Energy (DOE) and the National Renewable Energy Laboratory (NREL) have examined the impacts of integrating high penetrations of wind and solar energy on the Eastern and Western electric grids. The Eastern Wind Integration and Transmission Study (EWITS), initiated in 2007, examined the impact on power system operations of reaching 20% to 30% wind energy penetration in the Eastern Interconnection. The Western Wind and Solar Integration Study (WWSIS) examined the operational implications of adding up to 35% wind and solar energy penetration to the Western Interconnect. Both studies examined the costs of integrating variable renewable energy generation into the grid and transmission and operational changes that might be necessary to address higher penetrations of wind or solar generation. This paper identifies key insights from these regional studies for integrating high penetrations of renewables in the U.S. electric grid. The studies share a number of key findings, although in some instances the results vary due to differences in grid operations and markets, the geographic location of the renewables, and the need for transmission.

  19. NREL Confirms Large Potential for Grid Integration of Wind, Solar Power (Fact Sheet)

    SciTech Connect (OSTI)

    Not Available

    2011-10-01

    To fully harvest the nation's bountiful wind and solar resources, it is critical to know how much electrical power from these renewable resources could be integrated reliably into the grid. To inform the discussion about the potential of such variable sources, the National Renewable Energy Laboratory (NREL) launched two key regional studies, examining the east and west sections of the U.S. power grid. The studies show that it is technically possible for U.S. power systems to integrate 20%-35% renewable electricity if infrastructure and operational improvements can be made.

  20. Analysis of Cycling Costs in Western Wind and Solar Integration Study

    SciTech Connect (OSTI)

    Jordan, G.; Venkataraman, S.

    2012-06-01

    The Western Wind and Solar Integration Study (WWSIS) examined the impact of up to 30% penetration of variable renewable generation on the Western Electricity Coordinating Council system. Although start-up costs and higher operating costs because of part-load operation of thermal generators were included in the analysis, further investigation of additional costs associated with thermal unit cycling was deemed worthwhile. These additional cycling costs can be attributed to increases in capital as well as operations and maintenance costs because of wear and tear associated with increased unit cycling. This analysis examines the additional cycling costs of the thermal fleet by leveraging the results of WWSIS Phase 1 study.

  1. Final Solar and Wind H2 Report EPAct 812.doc | 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:FinancingPetroleum12, 2015Executive Order14,Energy 9,UNIVERSITY OF TEXAS AT||Solar and Wind H2

  2. WHITE-LIGHT OBSERVATIONS OF SOLAR WIND TRANSIENTS AND COMPARISON WITH AUXILIARY DATA SETS

    SciTech Connect (OSTI)

    Howard, T. A.; DeForest, C. E.; Reinard, A. A.

    2012-08-01

    This paper presents results utilizing a new data processing pipeline for STEREO/SECCHI. The pipeline is used to identify and track 24 large- and small-scale solar wind transients from the Sun out to 1 AU. This comparison was performed during a few weeks around the minimum at the end of Solar Cycle 23 and the start of Cycle 24 (2008 December to 2009 January). We use coronagraph data to identify features near the Sun, track them through HI-2A, and identify their signatures with in situ data at the Earth and STEREO-B. We provide measurements and preliminary analysis of the in situ signatures of these features near 1 AU. Along with the demonstration of the utility of heliospheric imagers for tracking even small-scale structures, we identify and discuss an important limitation in using geometric triangulation for determining three-dimensional properties.

  3. Suprathermal electron loss cone distributions in the solar wind: Ulysses observations

    SciTech Connect (OSTI)

    Phillips, J.L.; Feldman, W.C.; Gosling, J.T. [Los Alamos National Lab., NM (United States); Hammond, C.M. [SRI International, Menlo Park, CA (United States); Forsyth, R.J. [Imperial Coll. of Science and Technology, London (United Kingdom)

    1995-09-01

    We present observations by the Ulysses solar wind plasma experiment of a new class of suprathermal electron signatures. At low solar latitudes and heliocentric distances beyond 3.37 AU Ulysses encountered seven intervals, ranging in duration from 1 hour to 22 hours, in which the suprathermal distributions included an antisunward field-aligned beam and a return population with a flux dropout typically spanning {plus_minus}60 ft from the sunward field-aligned direction. All events occurred between the forward and reverse shocks or waves bounding corotating interaction regions (CIRs). The observations support a scenario in which the sunward-moving electrons result from reflection of the prevailing antisunward field-aligned beam at magnetic field compressions downstream from the spacecraft, with wide loss cones caused by the relatively weak mirror ratio. This hypothesis requires that the field magnitude within the CIRs actually increased locally with increasing field-aligned distance from the Sun.

  4. Graphene 'gateway' discovery opens possibilities for improved...

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

    Dawn Levy Communications 865.576.6448 Graphene 'gateway' discovery opens possibilities for improved energy technologies Computer simulations show a single proton (pink) can cross...

  5. T-566: Citrix Secure Gateway Unspecified Vulnerability

    Broader source: Energy.gov [DOE]

    A vulnerability has been reported in Citrix Secure Gateway, which can be exploited by malicious people to compromise a vulnerable system.

  6. The Smithsonian American Art Museum GATEWAY Demonstration

    Broader source: Energy.gov [DOE]

    View the video about using LEDs in a GATEWAY demonstration at the Smithsonian American Art Museum in Washington, DC, including an interview with lighting designer Scott Rosenfeld.

  7. Effects of electron drift on the collisionless damping of kinetic Alfv\\'en waves in the solar wind

    E-Print Network [OSTI]

    Tong, Yuguang; Chen, Christopher H K; Salem, Chadi S; Verscharen, Daniel

    2015-01-01

    The collisionless dissipation of anisotropic Alfv\\'enic turbulence is a promising candidate to solve the solar wind heating problem. Extensive studies examined the kinetic properties of Alfv\\'en waves in simple Maxwellian or bi-Maxwellian plasmas. However, the observed electron velocity distribution functions in the solar wind are more complex. In this study, we analyze the properties of kinetic Alfv\\'en waves in a plasma with two drifting electron populations. We numerically solve the linearized Maxwell-Vlasov equations and find that the damping rate and the proton-electron energy partition for kinetic Alfv\\'en waves are significantly modified in such plasmas, compared to plasmas without electron drifts. We suggest that electron drift is an important factor to take into account when considering the dissipation of Alfv\\'enic turbulence in the solar wind or other $\\beta \\sim 1$ astrophysical plasmas.

  8. Global Science Gateway Agreement Signed in London | Department...

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

    Global Science Gateway Agreement Signed in London Global Science Gateway Agreement Signed in London January 22, 2006 - 10:15am Addthis DOE Partners With British Library on...

  9. INSTABILITIES DRIVEN BY THE DRIFT AND TEMPERATURE ANISOTROPY OF ALPHA PARTICLES IN THE SOLAR WIND

    SciTech Connect (OSTI)

    Verscharen, Daniel; Bourouaine, Sofiane; Chandran, Benjamin D. G. E-mail: s.bourouaine@unh.edu

    2013-08-20

    We investigate the conditions under which parallel-propagating Alfven/ion-cyclotron (A/IC) waves and fast-magnetosonic/whistler (FM/W) waves are driven unstable by the differential flow and temperature anisotropy of alpha particles in the solar wind. We focus on the limit in which w{sub Parallel-To {alpha}} {approx}> 0.25v{sub A}, where w{sub Parallel-To {alpha}} is the parallel alpha-particle thermal speed and v{sub A} is the Alfven speed. We derive analytic expressions for the instability thresholds of these waves, which show, e.g., how the minimum unstable alpha-particle beam speed depends upon w{sub Parallel-To {alpha}}/v{sub A}, the degree of alpha-particle temperature anisotropy, and the alpha-to-proton temperature ratio. We validate our analytical results using numerical solutions to the full hot-plasma dispersion relation. Consistent with previous work, we find that temperature anisotropy allows A/IC waves and FM/W waves to become unstable at significantly lower values of the alpha-particle beam speed U{sub {alpha}} than in the isotropic-temperature case. Likewise, differential flow lowers the minimum temperature anisotropy needed to excite A/IC or FM/W waves relative to the case in which U{sub {alpha}} = 0. We discuss the relevance of our results to alpha particles in the solar wind near 1 AU.

  10. Use of Solar and Wind as a Physical Hedge against Price Variability within a Generation Portfolio

    SciTech Connect (OSTI)

    Jenkin, T.; Diakov, V.; Drury, E.; Bush, B.; Denholm, P.; Milford, J.; Arent, D.; Margolis, R.; Byrne, R.

    2013-08-01

    This study provides a framework to explore the potential use and incremental value of small- to large-scale penetration of solar and wind technologies as a physical hedge against the risk and uncertainty of electricity cost on multi-year to multi-decade timescales. Earlier studies characterizing the impacts of adding renewable energy (RE) to portfolios of electricity generators often used a levelized cost of energy or simplified net cash flow approach. In this study, we expand on previous work by demonstrating the use of an 8760 hourly production cost model (PLEXOS) to analyze the incremental impact of solar and wind penetration under a wide range of penetration scenarios for a region in the Western U.S. We do not attempt to 'optimize' the portfolio in any of these cases. Rather we consider different RE penetration scenarios, that might for example result from the implementation of a Renewable Portfolio Standard (RPS) to explore the dynamics, risk mitigation characteristics and incremental value that RE might add to the system. We also compare the use of RE to alternative mechanisms, such as the use of financial or physical supply contracts to mitigate risk and uncertainty, including consideration of their effectiveness and availability over a variety of timeframes.

  11. WHERE DOES FLUID-LIKE TURBULENCE BREAK DOWN IN THE SOLAR WIND?

    SciTech Connect (OSTI)

    Perri, S.; Carbone, V.; Veltri, P.

    2010-12-10

    Power spectra of the magnetic field in solar wind display a Kolmogorov law f {sup -5/3} at intermediate range of frequencies f, say within the inertial range. Two spectral breaks are also observed: one separating the inertial range from an f {sup -1} spectrum at lower frequencies, and another one between the inertial range and an f {sup -7/3} spectrum at higher frequencies. The breaking of fluid-like turbulence at high frequencies has been attributed to either the occurrence of kinetic Alfven wave fluctuations above the ion-cyclotron frequency or to whistler turbulence above the frequency corresponding to the proton gyroradius. Using solar wind data, we show that the observed high-frequency spectral break seems to be independent of the distance from the Sun, and then of both the ion-cyclotron frequency and the proton gyroradius. We suppose that the observed high-frequency break could be either caused by a combination of different physical processes or associated with a remnant signature of coronal turbulence.

  12. Eastern Renewable Generation Integration Study: Flexibility and High Penetrations of Wind and Solar; NREL (National Renewable Energy Laboratory)

    SciTech Connect (OSTI)

    Bloom, Aaron; Townsend, Aaron; Palchak, David

    2015-07-29

    Balancing wind and solar in a model is relatively easy. All you need to do is assume a very large system with infinite flexibility! But what if you don't have an infinitely flexible system? What if there are thousands of generators nestled in a handful of regions that are unlikely to change their operational practices? Would you still have enough flexibility to balance hundreds of gigawatts of wind and solar at a 5 minute level? At NREL, we think we can, and our industry partners agree. This presentation was presented at the IEEE Power and Energy Society General Meeting by Aaron Bloom, highlighting results of the Eastern Renewable Generation Integration Study.

  13. A PARALLEL-PROPAGATING ALFVENIC ION-BEAM INSTABILITY IN THE HIGH-BETA SOLAR WIND

    SciTech Connect (OSTI)

    Verscharen, Daniel; Bourouaine, Sofiane; Chandran, Benjamin D. G.; Maruca, Bennett A. E-mail: s.bourouaine@unh.edu E-mail: bmaruca@ssl.berkeley.edu

    2013-08-10

    We investigate the conditions under which parallel-propagating Alfven/ion-cyclotron waves are driven unstable by an isotropic (T{sub {alpha}} = T{sub Parallel-To {alpha}}) population of alpha particles drifting parallel to the magnetic field at an average speed U{sub {alpha}} with respect to the protons. We derive an approximate analytic condition for the minimum value of U{sub {alpha}} needed to excite this instability and refine this result using numerical solutions to the hot-plasma dispersion relation. When the alpha-particle number density is {approx_equal} 5% of the proton number density and the two species have similar thermal speeds, the instability requires that {beta}{sub p} {approx}> 1, where {beta}{sub p} is the ratio of the proton pressure to the magnetic pressure. For 1 {approx}< {beta}{sub p} {approx}< 12, the minimum U{sub {alpha}} needed to excite this instability ranges from 0.7v{sub A} to 0.9v{sub A}, where v{sub A} is the Alfven speed. This threshold is smaller than the threshold of {approx_equal} 1.2v{sub A} for the parallel magnetosonic instability, which was previously thought to have the lowest threshold of the alpha-particle beam instabilities at {beta}{sub p} {approx}> 0.5. We discuss the role of the parallel Alfvenic drift instability for the evolution of the alpha-particle drift speed in the solar wind. We also analyze measurements from the Wind spacecraft's Faraday cups and show that the U{sub {alpha}} values measured in solar-wind streams with T{sub {alpha}} Almost-Equal-To T{sub Parallel-To {alpha}} are approximately bounded from above by the threshold of the parallel Alfvenic instability.

  14. Markets to Facilitate Wind and Solar Energy Integration in the Bulk Power Supply: An IEA Task 25 Collaboration; Preprint

    SciTech Connect (OSTI)

    Milligan, M.; Holttinen, H.; Soder, L.; Clark, C.; Pineda, I.

    2012-09-01

    Wind and solar power will give rise to challenges in electricity markets regarding flexibility, capacity adequacy, and the participation of wind and solar generators to markets. Large amounts of wind power will have impacts on bulk power system markets and electricity prices. If the markets respond to increased wind power by increasing investments in low-capital, high-cost or marginal-cost power, the average price may remain in the same range. However, experiences so far from Denmark, Germany, Spain, and Ireland are such that the average market prices have decreased because of wind power. This reduction may result in additional revenue insufficiency, which may be corrected with a capacity market, yet capacity markets are difficult to design. However, the flexibility attributes of the capacity also need to be considered. Markets facilitating wind and solar integration will include possibilities for trading close to delivery (either by shorter gate closure times or intraday markets). Time steps chosen for markets can enable more flexibility to be assessed. Experience from 5- and 10-minute markets has been encouraging.

  15. Statement of Interest in a New Project, in response to PPARC call of April 26th FHIRN: A next-generation radio network for exploring the 3-dimensional solar wind

    E-Print Network [OSTI]

    spacecraft will build on these successes, with the Japan-UK Solar-B and NASA Solar Dynamics Observatory (SDO-generation radio network for exploring the 3-dimensional solar wind Future Heliospheric Imaging Radio Network The solar wind is a supersonically-expanding extension of the solar atmosphere into interplanetary space

  16. PROBING THE SOLAR WIND ACCELERATION REGION WITH THE SUN-GRAZING COMET C/2002 S2

    SciTech Connect (OSTI)

    Giordano, S.; Raymond, J. C.; Lamy, P.; Uzzo, M.; Dobrzycka, D.

    2015-01-01

    Comet C/2002 S2, a member of the Kreutz family of sungrazing comets, was discovered in white-light images of the Large Angle and Spectromeric Coronagraph Experiment coronagraph on the Solar and Heliospheric Observatory (SOHO) on 2002 September 18 and observed in H I Ly? emission by the SOHO Ultraviolet Coronagraph Spectrometer (UVCS) instrument at four different heights as it approached the Sun. The H I Ly? line profiles detected by UVCS are analyzed to determine the spectral parameters: line intensity, width, and Doppler shift with respect to the coronal background. Two-dimensional comet images of these parameters are reconstructed at the different heights. A novel aspect of the observations of this sungrazing comet data is that, whereas the emission from most of the tail is blueshifted, that along one edge of the tail is redshifted. We attribute these shifts to a combination of solar wind speed and interaction with the magnetic field. In order to use the comet to probe the density, temperature, and speed of the corona and solar wind through which it passes, as well as to determine the outgassing rate of the comet, we develop a Monte Carlo simulation of the H I Ly? emission of a comet moving through a coronal plasma. From the outgassing rate, we estimate a nucleus diameter of about 9 m. This rate steadily increases as the comet approaches the Sun, while the optical brightness decreases by more than a factor of 10 and suddenly recovers. This indicates that the optical brightness is determined by the lifetimes of the grains, sodium atoms, and molecules produced by the comet.

  17. Inward shift of outer radiation belt electrons as a function of Dst index and the influence of the solar wind on electron injections

    E-Print Network [OSTI]

    Li, Xinlin

    Inward shift of outer radiation belt electrons as a function of Dst index and the influence of the solar wind on electron injections into the slot region H. Zhao1 and X. Li1 Received 30 July 2012 electrons as a function of the Dst index and the controlling solar wind parameters for deep penetration

  18. Effect of solar wind pressure enhancements on storm time ring current Y. Shi, E. Zesta, L. R. Lyons, and A. Boudouridis

    E-Print Network [OSTI]

    Lyons, Larry

    Effect of solar wind pressure enhancements on storm time ring current asymmetry Y. Shi, E. Zesta, L; accepted 12 July 2005; published 8 October 2005. [1] The effect of solar wind pressure enhancements be explained by considering the local energization of the preexisting ring current particles by the azimuthal

  19. MEASUREMENTS OF RAPID DENSITY FLUCTUATIONS IN THE SOLAR WIND This article has been downloaded from IOPscience. Please scroll down to see the full text article.

    E-Print Network [OSTI]

    California at Berkeley, University of

    February 9 ABSTRACT The power spectrum of density fluctuations in the solar wind is inferred by trackingMEASUREMENTS OF RAPID DENSITY FLUCTUATIONS IN THE SOLAR WIND This article has been downloaded from is available Home Search Collections Journals About Contact us My IOPscience #12;The Astrophysical Journal, 711

  20. JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 101, NO. A5, PAGES 11,01711,025, MAY 1, 1996 The Distance to the Solar Wind Termination Shock in

    E-Print Network [OSTI]

    Cummings, Alan C.

    to the Solar Wind Termination Shock in 1993 and 1994 from Observations of Anomalous Cosmic Rays E. C. Stone acceleration along the solar wind termination shock. In addition, large propagating interplanetary disturbances) and consistent with a termination shock modified by the pressure of galactic cosmic rays. By comparing these 1994

  1. EAST CAMPUS / MIT GATEWAY Alternative Approaches

    E-Print Network [OSTI]

    Reif, Rafael

    EAST CAMPUS / MIT GATEWAY Alternative Approaches Prepared by The Design Committee July 19. 2013 #12;East Campus / MIT Gateway - Alternative Approaches 1 This report lays out strategic options for design space on the campus south of Main Street. The report examines alternative approaches to achieving

  2. Discrimination and quantification of contamination and implanted solar wind in Genesis collector shards using grazing incidence synchrotron x-ray techniqies: Initial results

    SciTech Connect (OSTI)

    Kitts, K.; Sutton, S.; Eng, P.; Ghose, S.; Burnett, D.

    2006-12-13

    Grazing incidence X-ray fluorescence is a non-destructive technique that can differentiate the embedded solar wind component from surface contamination and collector background in the Genesis shards. Initial solar Fe abundance in D30554 is 8 x 10{sup 12}/cm{sup 2}. Accurate knowledge of the composition of the Sun provides a baseline, which allows an understanding of how the solar system has evolved over time and how solar processes and solar wind mechanics behave. Unfortunately, the errors in photospheric abundances are too large for many planetary science problems and this hampers our understanding of these different processes. Analyses of solar wind implanted in meteorites or lunar soils have provided more precise data but alteration processes on these bodies may complicate such information. In response to this need for pristine solar wind samples, NASA developed and launched the Genesis Probe. Unfortunately, the probe smashed into the Utah desert shattering the 300 collector plates into 15,000+ pieces all of which are now coated in a both a fine terrestrial dust and Si and Ge powder from the disrupted collectors themselves. The solar wind penetration depth is 100-200 nm and the superposed contamination layers are typically 40-50 nm. Stringent cleaning regimes have the potential of removing the solar wind itself. The best solution is to have sufficient spatial resolution to separately analyze the surface contamination and penetrated solar wind. To that end, three Genesis collector array shards and their appropriate flight spares were characterized via grazing incidence x-ray fluorescence and x-ray reflectivity. The goals were (1) to evaluate the various cleaning methods used to eliminate contamination, (2) to identify the collector substrates most suited for this technique, (3) to determine whether the solar wind signature could be deconvolved from the collector background signature, and (4) to measure the relative abundances of Ca to Ge in the embedded solar wind.

  3. Detecting the oldest geodynamo and attendant shielding from the solar wind: Implications for habitability

    E-Print Network [OSTI]

    Tarduno, John A; Mamajek, Eric E

    2015-01-01

    The onset and nature of the earliest geomagnetic field is important for understanding the evolution of the core, atmosphere and life on Earth. A record of the early geodynamo is preserved in ancient silicate crystals containing minute magnetic inclusions. These data indicate the presence of a geodynamo during the Paleoarchean, between 3.4 and 3.45 billion years ago. While the magnetic field sheltered Earth's atmosphere from erosion at this time, standoff of the solar wind was greatly reduced, and similar to that during modern extreme solar storms. These conditions suggest that intense radiation from the young Sun may have modified the atmosphere of the young Earth by promoting loss of volatiles, including water. Such effects would have been more pronounced if the field were absent or very weak prior to 3.45 billion years ago, as suggested by some models of lower mantle evolution. The frontier is thus trying to obtain geomagnetic field records that are >>3.45 billion-years-old, as well as constraining solar wi...

  4. VOL. 79, NO. 28 JOURNAL OF GEOPHYSICAL RESEARCH OCTOBER 1, 1974 On the BackscatterInstability of Solar Wind Alfvn Waves

    E-Print Network [OSTI]

    Dewar, Robert L.

    Instability of Solar Wind Alfvn Waves RONALD H. COHEN x AND ROBERT L. DEWAR ·' Plasma PhysicsLaboratory, Princeton istheambientfieldstrength,andCOoisthefrequencyof thepar- ent wave in the rest frame of the fluid. Using the wind the wind shouldbe observed,particularly at shorterwavelengths.Also, it hasbeensuggested[Jokipii, 1971]that

  5. Application of a solar wind model driven by turbulence dissipation to a 2D magnetic field configuration

    SciTech Connect (OSTI)

    Lionello, Roberto; Downs, Cooper; Linker, Jon A.; Miki?, Zoran; Velli, Marco E-mail: cdowns@predsci.com E-mail: mikic@predsci.com

    2014-12-01

    Although it is widely accepted that photospheric motions provide the energy source and that the magnetic field must play a key role in the process, the detailed mechanisms responsible for heating the Sun's corona and accelerating the solar wind are still not fully understood. Cranmer et al. developed a sophisticated, one-dimensional (1D), time-steady model of the solar wind with turbulence dissipation. By varying the coronal magnetic field, they obtain, for a single choice of wave properties, a realistic range of slow and fast wind conditions with a sharp latitudinal transition between the two streams. Using a 1D, time-dependent model of the solar wind of Lionello et al., which incorporates turbulent dissipation of Alfvén waves to provide heating and acceleration of the plasma, we have explored a similar configuration, obtaining qualitatively equivalent results. However, our calculations suggest that the rapid transition between slow and fast wind suggested by this 1D model may be disrupted in multidimensional MHD simulations by the requirement of transverse force balance.

  6. Evidence that Voyager-I Exited the Solar Wind at ~85 AU S.M. Krimigis1

    E-Print Network [OSTI]

    1 Evidence that Voyager-I Exited the Solar Wind at ~85 AU S.M. Krimigis1 , R.B. Decker1 , M.E. HillV/nuc) and species (H, He, C, N, O, Ne, etc). The double-ended detector telescope system is mounted on a stepping

  7. Studying the Lunar-Solar Wind Interaction with the SARA Experiment aboard the Indian Lunar Mission Chandrayaan-1

    E-Print Network [OSTI]

    Bhardwaj, Anil; Dhanya, M B; Wieser, Martin; Yoshifumi, Futaana; Holmstrom, Mats; Sridharan, R; Wurz, Peter; Schaufelberger, Audrey; Kazushi, Asamura; 10.1063/1.3395916

    2010-01-01

    The first Indian lunar mission Chandrayaan-1 was launched on 22 October 2008. The Sub-keV Atom Reflecting Analyzer (SARA) instrument onboard Chandrayaan-1 consists of an energetic neutral atom (ENA) imaging mass analyzer called CENA (Chandrayaan-1 Energetic Neutrals Analyzer), and an ion-mass analyzer called SWIM (Solar wind Monitor). CENA performed the first ever experiment to study the solar wind-planetary surface interaction via detection of sputtered neutral atoms and neutralized backscattered solar wind protons in the energy range ~0.01-3.0 keV. SWIM measures solar wind ions, magnetosheath and magnetotail ions, as well as ions scattered from lunar surface in the ~0.01-15 keV energy range. The neutral atom sensor uses conversion of the incoming neutrals to positive ions, which are then analyzed via surface interaction technique. The ion mass analyzer is based on similar principle. This paper presents the SARA instrument and the first results obtained by the SWIM and CENA sensors. SARA observations suggest...

  8. 2006 LWS TR & T Solar Wind Focused Science Topic Team: The ... http://www.agu.org/cgi-bin/SFgate/SFgate?language=English&verb... 1 of 2 11/14/06 11:27 AM

    E-Print Network [OSTI]

    Ng, Chung-Sang

    2006 LWS TR & T Solar Wind Focused Science Topic Team: The ... http://www=ng HR: 0800h AN: SH11A-0371 TI: 2006 LWS TR & T Solar Wind Focused Science Topic Team: The Beginnings AU;2006 LWS TR & T Solar Wind Focused Science Topic Team: The ... http://www

  9. Anisotropic MHD/EMHD Turbulence in the Solar Wind and the Inte... http://www.agu.org/cgi-bin/SFgate/SFgate?language=English&verb... 1 of 1 3/10/05 11:25 AM

    E-Print Network [OSTI]

    Ng, Chung-Sang

    Anisotropic MHD/EMHD Turbulence in the Solar Wind and the Inte... http://www-0284 TI: Anisotropic MHD/EMHD Turbulence in the Solar Wind and the Interstellar Medium AU 03824 United States AB: The solar wind and the interstellar medium is permeated by large-scale magnetic

  10. Plasma ? scaling of anisotropic magnetic field fluctuations in the solar wind flux tube

    SciTech Connect (OSTI)

    Sarkar, Aveek; Bhattacharjee, Amitava; Ebrahimi, Fatima E-mail: amitava@princeton.edu

    2014-03-10

    Based on various observations, it has been suggested that at 1 AU, solar wind consists of 'spaghetti'-like magnetic field structures that have the magnetic topology of flux tubes. It is also observed that the plasma fluctuation spectra at 1 AU show a plasma ? dependence. Reconciling these two sets of observations and using the Invariance Principle, Bhattacharjee et al. suggested that the plasma inside every flux tube may become unstable with respect to pressure-driven instabilities and gives rise to fluctuation spectra that depend on the local plasma ?. The present work is the first direct numerical simulation of such a flux tube. We solve the full magnetohydrodynamic equations using the DEBS code and show that if the plasma inside the flux tube is driven unstable by spatial inhomogeneities in the background plasma pressure, the observed nature of the fluctuating power spectra agrees reasonably well with observations, as well as the analytical prediction of Bhattacharjee et al.

  11. Nonlinear and linear timescales near kinetic scales in solar wind turbulence

    SciTech Connect (OSTI)

    Matthaeus, W. H.; Wan, M.; Shay, M. A.; Oughton, S.; Osman, K. T.; Chapman, S. C.; Servidio, S.; Valentini, F.; Gary, S. P.; Roytershteyn, V.; Karimabadi, H.

    2014-08-01

    The application of linear kinetic treatments to plasma waves, damping, and instability requires favorable inequalities between the associated linear timescales and timescales for nonlinear (e.g., turbulence) evolution. In the solar wind these two types of timescales may be directly compared using standard Kolmogorov-style analysis and observational data. The estimated local (in scale) nonlinear magnetohydrodynamic cascade times, evaluated as relevant kinetic scales are approached, remain slower than the cyclotron period, but comparable to or faster than the typical timescales of instabilities, anisotropic waves, and wave damping. The variation with length scale of the turbulence timescales is supported by observations and simulations. On this basis the use of linear theory—which assumes constant parameters to calculate the associated kinetic rates—may be questioned. It is suggested that the product of proton gyrofrequency and nonlinear time at the ion gyroscales provides a simple measure of turbulence influence on proton kinetic behavior.

  12. Alternative Approaches to Calculate Benefits of an Energy Imbalance Market With Wind and Solar Energy: Preprint

    SciTech Connect (OSTI)

    Kirby, B.; King, J.; Milligan, M.

    2012-06-01

    The anticipated increase in variable generation in the Western Interconnection over the next several years has raised concerns about how to maintain system balance, especially in smaller Balancing Authority Areas (BAAs). Given renewable portfolio standards in the West, it is possible that more than 50 gigawatts of wind capacity will be installed by 2020. Significant quantities of solar generation are likely to be added as well. The consequent increase in variability and uncertainty that must be managed by the conventional generation fleet and responsive loads has resulted in a proposal for an Energy Imbalance Market (EIM). This paper extends prior work to estimate the reserve requirements for regulation, spinning, and non-spinning reserves with and without the EIM. We also discuss alternative approaches to allocating reserve requirements and show that some apparently attractive allocation methods have undesired consequences.

  13. Kinetic temperatures of iron ions in the solar wind observed with STEREO/PLASTIC

    SciTech Connect (OSTI)

    Bochsler, Peter; Lee, Martin A.; Popecki, Mark A.; Galvin, Antoinette B.; Kistler, Lynn M.; Moebius, Eberhard; Farrugia, Charles J.; Kucharek, Harald; Simunac, Kristin D. C.; Karrer, Reto; Blush, Lisa M.; Daoudi, Hagar; Wurz, Peter; Klecker, Berndt; Wimmer-Schweingruber, Robert F.; Thompson, Barbara; Luhmann, Janet G.; Jian, Lan K.; Russell, Christopher T.; Opitz, Andrea

    2010-03-25

    STEREO/PLASTIC provides detailed information on the three-dimensional velocity distributions of solar wind iron ions with a time resolution of 5 minutes. In general the distributions at 1 AU contain complicated structures showing persistence over several records, i.e., over intervals of up to 30 minutes, but no clear correlation of the properties of these distributions with the direction of the ambient magnetic field is evident. We have performed a statistical analysis using nearly 9000 observations. Iron ions follow the same trends as protons, alpha particles, and electrons: The ratio T{sub perpendicular}/T{sub ||} seems to be limited by the ion cyclotron instability, whereas T{sub ||} /T{sub perpendicular} is bounded by the firehose instability.

  14. Sign-Singularity of the Reduced Magnetic Helicity in the Solar Wind Plasma

    SciTech Connect (OSTI)

    Carbone, V.; Perri, S.; Yordanova, E.; Khotyaintsev, Y.; Andre, M.; Veltri, P.; Bruno, R.

    2010-05-07

    We investigate the scaling laws of a signed measure derived from the reduced magnetic helicity which has been determined from Cluster data in the solar wind. This quantifies the handedness of the magnetic field; namely, it can be related to the polarization of the magnetic field fluctuations (right or left hand). The measure results to be sign-singular; that is, we do not observe any scale-dependent effect at the ion- and at electron-cyclotron frequencies. Cancellations between right- and left-hand polarizations go on in the dispersive or dissipative range, beyond the electron-cyclotron frequency. This means that the mechanism responsible for the generation of the dispersive or dissipative range is rather insensitive to the polarization of the magnetic field fluctuations.

  15. The Complex Structure of Magnetic Field Discontinuities in the Turbulent Solar Wind

    E-Print Network [OSTI]

    Greco, A; Servidio, S; Yordanova, E; Veltri, P

    2015-01-01

    Using high resolution Cluster satellite observations, we show that the turbulent solar wind is populated by magnetic discontinuities at different scales, going from proton down to electron scales. The structure of these layers resembles the Harris equilibrium profile in plasmas. Using a multi-dimensional intermittency technique, we show that these structures are connected through the scales. Supported by numerical simulations of magnetic reconnection, we show that observations are consistent with a scenario where many current layers develop in turbulence, and where the outflow of these reconnection events are characterized by complex sub-proton networks of secondary islands, in a self-similar way. The present work establishes that the picture of "reconnection in turbulence" and "turbulent reconnection", separately invoked as ubiquitous, coexist in space plasmas.

  16. ENSEMBLE SIMULATIONS OF PROTON HEATING IN THE SOLAR WIND VIA TURBULENCE AND ION CYCLOTRON RESONANCE

    SciTech Connect (OSTI)

    Cranmer, Steven R.

    2014-07-01

    Protons in the solar corona and heliosphere exhibit anisotropic velocity distributions, violation of magnetic moment conservation, and a general lack of thermal equilibrium with the other particle species. There is no agreement about the identity of the physical processes that energize non-Maxwellian protons in the solar wind, but a traditional favorite has been the dissipation of ion cyclotron resonant Alfvén waves. This paper presents kinetic models of how ion cyclotron waves heat protons on their journey from the corona to interplanetary space. It also derives a wide range of new solutions for the relevant dispersion relations, marginal stability boundaries, and nonresonant velocity-space diffusion rates. A phenomenological model containing both cyclotron damping and turbulent cascade is constructed to explain the suppression of proton heating at low alpha-proton differential flow speeds. These effects are implemented in a large-scale model of proton thermal evolution from the corona to 1 AU. A Monte Carlo ensemble of realistic wind speeds, densities, magnetic field strengths, and heating rates produces a filled region of parameter space (in a plane described by the parallel plasma beta and the proton temperature anisotropy ratio) similar to what is measured. The high-beta edges of this filled region are governed by plasma instabilities and strong heating rates. The low-beta edges correspond to weaker proton heating and a range of relative contributions from cyclotron resonance. On balance, the models are consistent with other studies that find only a small fraction of the turbulent power spectrum needs to consist of ion cyclotron waves.

  17. Organization of Energetic Particles by the Solar Wind Structure During the Declining to Minimum Phase of Solar Cycle 23

    E-Print Network [OSTI]

    2010-01-01

    do not occur for more than one solar rotation, as de?ned byspanned over 20 solar rotations, where one such sequence ofHCS was north about one quarter of a solar rotation and near

  18. Organization of Energetic Particles by the Solar Wind Structure During the Declining to Minimum Phase of Solar Cycle 23

    E-Print Network [OSTI]

    2010-01-01

    the longitude distribution of solar energetic particles. J.shocks in deter- mining solar energetic particle abundances.J.E. , Dwyer, J.R. : 2006a, Solar cycle variations in the

  19. LIMITS ON ALPHA PARTICLE TEMPERATURE ANISOTROPY AND DIFFERENTIAL FLOW FROM KINETIC INSTABILITIES: SOLAR WIND OBSERVATIONS

    SciTech Connect (OSTI)

    Bourouaine, Sofiane; Verscharen, Daniel; Chandran, Benjamin D. G.; Maruca, Bennett A.; Kasper, Justin C.

    2013-11-01

    Previous studies have shown that the observed temperature anisotropies of protons and alpha particles in the solar wind are constrained by theoretical thresholds for pressure and anisotropy driven instabilities such as the Alfvén/ion-cyclotron (A/IC) and fast-magnetosonic/whistler (FM/W) instabilities. In this Letter, we use a long period of in situ measurements provided by the Wind spacecraft's Faraday cups to investigate the combined constraint on the alpha proton differential flow velocity and the alpha particle temperature anisotropy due to A/IC and FM/W instabilities. We show that the majority of the data are constrained to lie within the region of parameter space in which A/IC and FM/W waves are either stable or have extremely low growth rates. In the minority of observed cases in which the growth rate of the A/IC (FM/W) instability is comparatively large, we find relatively higher values of T {sub ?}/T {sub p} (T {sub ??}/T {sub ?p}) when the alpha proton differential flow velocity is small, where T {sub ?} and T {sub p} (T {sub ??} and T {sub ?p}) are the perpendicular (parallel) temperatures of alpha particles and protons. We conjecture that this observed feature might arise from preferential alpha particle heating which can drive the alpha particles beyond the instability thresholds.

  20. From solar to stellar corona: the role of wind, rotation and magnetism

    E-Print Network [OSTI]

    Réville, Victor; Strugarek, Antoine; Matt, Sean P; Bouvier, Jérôme; Folsom, Colin P; Petit, Pascal

    2015-01-01

    Observations of surface magnetic fields are now within reach for many stellar types thanks to the development of Zeeman-Doppler Imaging. These observations are extremely useful for constraining rotational evolution models of stars, as well as for characterizing the generation of magnetic field. We recently demonstrated that the impact of coronal magnetic field topology on the rotational braking of a star can be parametrized with a scalar parameter: the open magnetic flux. However, without running costly numerical simulations of the stellar wind, reconstructing the coronal structure of the large scale magnetic field is not trivial. An alternative -broadly used in solar physics- is to extrapolate the surface magnetic field assuming a potential field in the corona, to describe the opening of the field lines by the magnetized wind. This technique relies on the definition of a so-called source surface radius, which is often fixed to the canonical value of 2.5Rsun. However this value likely varies from star to star...

  1. Comment on "Air Emissions Due to Wind and Solar Power" and Supporting Information

    E-Print Network [OSTI]

    Mills, Andrew D.

    2011-01-01

    The Effects of Integrating Wind Power on Transmission SystemH. On methodology for modelling wind power impact on powerwith Large Amounts of Wind Power; VTT Working Paper 82,

  2. Gross Receipts Tax Exemption for Sales of Wind and Solar Systems...

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

    Photovoltaics Wind (All) Wind (Small) Program Info Sector Name State Administrator New Mexico Taxation & Revenue Department Website http:www.emnrd.state.nm.usECMD...

  3. Dust Detection by the Wave Instrument on STEREO: Nanoparticles Picked up by the Solar Wind?

    E-Print Network [OSTI]

    2009-01-01

    including the large solar panels which contribute to amaterial, kap- ton, solar panel mylar, and a few metallic

  4. Oxygen Loss from Venus and the Influence of Extreme Solar Wind Conditions

    E-Print Network [OSTI]

    McEnulty, Tess

    2012-01-01

    observations of geoeffective solar flare events in Decemberare the location of solar flares and coronal mass ejections

  5. SSL GATEWAY UNIVERSITY OF FLORIDA DANCE SHOWCASE

    Broader source: Energy.gov [DOE]

    View the video showing side-by-side dance performances with halogen and LED sidelighting as part of the Solid-State Lighting GATEWAY demonstration at the University of Florida.

  6. VELOCITY-SHEAR-INDUCED MODE COUPLING IN THE SOLAR ATMOSPHERE AND SOLAR WIND: IMPLICATIONS FOR PLASMA HEATING AND MHD TURBULENCE

    SciTech Connect (OSTI)

    Hollweg, Joseph V.; Chandran, Benjamin D. G.; Kaghashvili, Edisher Kh. E-mail: ekaghash@aer.com

    2013-06-01

    We analytically consider how velocity shear in the corona and solar wind can cause an initial Alfven wave to drive up other propagating signals. The process is similar to the familiar coupling into other modes induced by non-WKB refraction in an inhomogeneous plasma, except here the refraction is a consequence of velocity shear. We limit our discussion to a low-beta plasma, and ignore couplings into signals resembling the slow mode. If the initial Alfven wave is propagating nearly parallel to the background magnetic field, then the induced signals are mainly a forward-going (i.e., propagating in the same sense as the original Alfven wave) fast mode, and a driven signal propagating like a forward-going Alfven wave but polarized like the fast mode; both signals are compressive and subject to damping by the Landau resonance. For an initial Alfven wave propagating obliquely with respect to the magnetic field, the induced signals are mainly forward- and backward-going fast modes, and a driven signal propagating like a forward-going Alfven wave but polarized like the fast mode; these signals are all compressive and subject to damping by the Landau resonance. A backward-going Alfven wave, thought to be important in the development of MHD turbulence, is also produced, but it is very weak. However, we suggest that for oblique propagation of the initial Alfven wave the induced fast-polarized signal propagating like a forward-going Alfven wave may interact coherently with the initial Alfven wave and distort it at a strong-turbulence-like rate.

  7. OBSERVATIONAL TEST OF STOCHASTIC HEATING IN LOW-{beta} FAST-SOLAR-WIND STREAMS

    SciTech Connect (OSTI)

    Bourouaine, Sofiane; Chandran, Benjamin D. G.

    2013-09-10

    Spacecraft measurements show that protons undergo substantial perpendicular heating during their transit from the Sun to the outer heliosphere. In this paper, we use Helios 2 measurements to investigate whether stochastic heating by low-frequency turbulence is capable of explaining this perpendicular heating. We analyze Helios 2 magnetic field measurements in low-{beta} fast-solar-wind streams between heliocentric distances r = 0.29 AU and r = 0.64 AU to determine the rms amplitude of the fluctuating magnetic field, {delta}B{sub p}, near the proton gyroradius scale {rho}{sub p}. We then evaluate the stochastic heating rate Q{sub stoch} using the measured value of {delta}B{sub p} and a previously published analytical formula for Q{sub stoch}. Using Helios measurements we estimate the ''empirical'' perpendicular heating rate Q{sub Up-Tack emp} = (k{sub B}/m{sub p}) BV (d/dr) (T{sub Up-Tack p}/B) that is needed to explain the T{sub p} profile. We find that Q{sub stoch} {approx} Q{sub emp}, but only if a key dimensionless constant appearing in the formula for Q{sub stoch} lies within a certain range of values. This range is approximately the same throughout the radial interval that we analyze and is consistent with the results of numerical simulations of the stochastic heating of test particles in reduced magnetohydrodynamic turbulence. These results support the hypothesis that stochastic heating accounts for much of the perpendicular proton heating occurring in low-{beta} fast-wind streams.

  8. ON THE ORIGIN OF THE 1/f SPECTRUM IN THE SOLAR WIND MAGNETIC FIELD

    SciTech Connect (OSTI)

    Verdini, Andrea [Solar-Terrestrial Center of Excellence-SIDC, Royal Observatory of Belgium, Bruxelles (Belgium); Grappin, Roland [LUTH, Observatoire de Paris, CNRS, Universite Paris-Diderot, 92190 Meudon (France); Pinto, Rui [Laboratoire AIM Paris-Saclay, CEA/Irfu, and Universite Paris-Diderot CNRS/INSU, Gis-sur-Yvette (France); Velli, Marco, E-mail: verdini@oma.be, E-mail: Roland.Grappin@obspm.fr, E-mail: rui.pinto@cea.fr, E-mail: mvelli@jpl.nasa.gov [Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA (United States)

    2012-05-10

    We present a mechanism for the formation of the low-frequency 1/f magnetic spectrum based on numerical solutions of a shell-reduced MHD model of the turbulent dynamics inside the sub-Alfvenic solar wind. We assign reasonably realistic profiles to the wind speed and the density along the radial direction, and a radial magnetic field. Alfven waves of short periodicity (600 s) are injected at the base of the chromosphere, penetrate into the corona, and are partially reflected, thus triggering a turbulent cascade. The cascade is strong for the reflected wave while it is weak for the outward propagating waves. Reflection at the transition region recycles the strong turbulent spectrum into the outward weak spectrum, which is advected beyond the Alfvenic critical point without substantial evolution. There, the magnetic field has a perpendicular power-law spectrum with slope close to the Kolmogorov -5/3. The parallel spectrum is inherited from the frequency spectrum of large (perpendicular) eddies. The shape is a double power law with slopes of {approx_equal} - 1 and -2 at low and high frequencies, respectively, with the position of the break depending on the injected spectrum. We suggest that the double power-law spectrum measured by Helios at 0.3 AU, where the average magnetic field is not aligned with the radial (contrary to our assumptions), results from the combination of such different spectral slopes. At low frequency the parallel spectrum dominates with its characteristic 1/f shape, while at higher frequencies its steep spectral slope (-2) is masked by the more energetic perpendicular spectrum (slope -5/3).

  9. Bi-Directional Energy Cascades and the Origin of Kinetic Alfv\\'enic and Whistler Turbulence in the Solar Wind

    E-Print Network [OSTI]

    Che, H; Viñas, A F

    2013-01-01

    The observed sub-proton scale turbulence spectrum in the solar wind raises the question of how that turbulence originates. Observations of keV energetic electrons during solar quite-time suggest them as possible source of free energy to drive the turbulence. Using particle-in-cell simulations, we explore how free energy in energetic electrons, released by an electron two-stream instability drives Weibel-like electromagnetic waves that excite wave-wave interactions. Consequently, both kinetic Alfv\\'enic and whistler waves are excited that evolve through inverse and forward magnetic energy cascades.

  10. The Dependence of the Strength and Thickness of Field-Aligned Currents on Solar Wind and Ionospheric Parameters

    SciTech Connect (OSTI)

    Johnson, Jay R.; Wing, Simon

    2014-08-01

    Sheared plasma flows at the low-latitude boundary layer correlate well with early afternoon auroral arcs and #12;eld-aligned currents [Sonnerup, 1980; Lundin and Evans, 1985]. We present a simple analytic model that relates solar wind and ionospheric parameters to the strength and thickness of field-aligned currents in a region of sheared velocity, such as the low latitude boundary layer. We compare the predictions of the model with DMSP observations and #12;nd remarkably good scaling of the currents with solar wind and ionospheric parameters. The sheared boundary layer thickness is inferred to be around 3000km consistent with observational studies. The analytic model provides a simple way to organize data and to infer boundary layer structures from ionospheric data.

  11. Collisionless damping of circularly polarized nonlinear Alfvén waves in solar wind plasmas with and without beam protons

    SciTech Connect (OSTI)

    Nariyuki, Y.; Hada, T.; Tsubouchi, K.

    2014-10-01

    The damping process of field-aligned, low-frequency right-handed polarized nonlinear Alfvén waves (NAWs) in solar wind plasmas with and without proton beams is studied by using a two-dimensional ion hybrid code. The numerical results show that the obliquely propagating kinetic Alfvén waves (KAWs) excited by beam protons affect the damping of the low-frequency NAW in low beta plasmas, while the nonlinear wave-wave interaction between parallel propagating waves and nonlinear Landau damping due to the envelope modulation are the dominant damping process in high beta plasmas. The nonlinear interaction between the NAWs and KAWs does not cause effective energy transfer to the perpendicular direction. Numerical results suggest that while the collisionless damping due to the compressibility of the envelope-modulated NAW plays an important role in the damping of the field-aligned NAW, the effect of the beam instabilities may not be negligible in low beta solar wind plasmas.

  12. Linear and Non-Linear Landau Resonance of Kinetic Alfv\\'en Waves: Consequences for Electron Distribution and Wave Spectrum in the Solar Wind

    E-Print Network [OSTI]

    Rudakov, Leonid; Ganguli, Gurudas; Crabtree, Chris

    2010-01-01

    Kinetic Alfven wave turbulence in solar wind is considered and it is shown that non-Maxwellian electron distribution function has a significant effect on the dynamics of the solar wind plasmas. Linear Landau damping leads to the formation of a plateau in the parallel electron distribution function which diminishes the Landau damping rate significantly. Nonlinear scattering of waves by plasma particles is generalized to short wavelengths and it is found that for the solar wind parameters this scattering is the dominant process as compared to three wave decay and coalescence in the wave vector range . Incorporation of these effects lead to the steepening of the wave spectrum between the inertial and the dissipation ranges with a spectral index between 2 and 3. This region can be labeled as the scattering range. Such steepening has been observed in the solar wind plasmas.

  13. Solar cyclical trend study of the mid-latitude, quiet-time, meridional, neutral winds at winter solstice conditions. Master's thesis

    SciTech Connect (OSTI)

    Breninger, R.L.

    1989-01-01

    Located within the region of the thermosphere is the major portion of the ionosphere. Distribution of the ionospheric plasma within this region is a function of atmospheric mass and energy transport. For the current study, the component of the neutral wind along the magnetic meridian is derived from ground-based ionosonde measurements of the F2 peak layer height. Meridional wind variations with respect to location, universal time, and level of solar activity are the focal points on this investigation. The primary timescale of interest covers a period of one solar cycle, from 1977 to 1987. Data from one station have been extended to 1965 to study the repetitive nature of solar activity on the meridional winds. Results of this study indicate a definite variation of wind speed and direction, which correlates with changing levels of solar activity. It is hoped that the results of this study will aid current efforts to develop ionospheric models and enhance their forecasting capabilities.

  14. Variations of 0.7-6.0 MeV Electrons at Geosynchronous Orbit as a Function of Solar Wind

    E-Print Network [OSTI]

    Li, Xinlin

    1 Variations of 0.7-6.0 MeV Electrons at Geosynchronous Orbit as a Function of Solar Wind Xinlin Li, Boulder Short title: VARIATIONS OF 0.7-6.0 MEV ELECTRONS #12;2 Abstract. The variations of MeV electron.4% and a linear correlation of 0.81 were achieved for the logarithm of average daily flux of 0.7-1.8 MeV electrons

  15. Stochastic Methods for Planning and Operating Power Systems with Large Amounts of Wind and Solar Power: Preprint

    SciTech Connect (OSTI)

    Milligan, M.; Donohoo, P.; O'Malley, M.

    2012-09-01

    Wind and solar generators differ in their generation characteristics than conventional generators. The variable output and imperfect predictability of these generators face a stochastic approach to plan and operate the power system without fundamentally changing the operation and planning problems. This paper overviews stochastic modeling challenges in operations, generation planning, and transmission planning, with references to current industry and academic work. Different stochastic problem formulations, including approximations, are also discussed.

  16. Details of a Hybrid Model for the Interaction between the Solar Wind and Planets Implemented in FLASH

    E-Print Network [OSTI]

    Holmstrom, M

    2015-01-01

    A hybrid plasma solver treats ions as particles and electrons as a fluid. We have implemented a parallel hybrid solver in the FLASH open source software framework. The solver has been applied to studies of the interaction between the solar wind and planets. Here we discuss the implementation of different model features, such as permanent magnetic fields, ionospheric chemistry, and exospheres. Mars is used as an example.

  17. Strategies to Mitigate Declines in the Economic Value of Wind and Solar at High Penetration in California

    Broader source: Energy.gov [DOE]

    This resource evaluates several options to reduce and eliminate the decline in the value of wind and solar PV technology, as a previous study had quantified the decline as penetration levels increased. Researchers found that largest increase in the value of PV at high penetration levels comes from assuming that low-cost bulk power storage is an investment option. Other attractive options, particularly at more modest penetration levels, include real-time pricing and technology diversity.

  18. Print http://us.mg4.mail.yahoo.comfneo/launch?.rand=deOsgk04ks40i Subject: Re: [s-w-h] Solar verses wind efficiency

    E-Print Network [OSTI]

    . A single nominal 100 watt solar panel for 4 sun hours/day would yield -4 kWh/day or 12 kWh/month. At $2Print http://us.mg4.mail.yahoo.comfneo/launch?.rand=deOsgk04ks40i Subject: Re: [s-w-h] Solar verses wind efficiency From: David Raine (dave@dyocore.com) To: wind4energy@yahoo.com; Date: Thursday

  19. ON QUIET-TIME SOLAR WIND ELECTRON DISTRIBUTIONS IN DYNAMICAL EQUILIBRIUM WITH LANGMUIR TURBULENCE

    SciTech Connect (OSTI)

    Zaheer, S.; Yoon, P. H.

    2013-10-01

    A recent series of papers put forth a self-consistent theory of an asymptotically steady-state electron distribution function and Langmuir turbulence intensity. The theory was developed in terms of the ? distribution which features Maxwellian low-energy electrons and a non-Maxwellian energetic power-law tail component. The present paper discusses a generalized ? distribution that features a Davydov-Druyvesteyn type of core component and an energetic power-law tail component. The physical motivation for such a generalization is so that the model may reflect the influence of low-energy electrons interacting with low-frequency kinetic Alfvénic turbulence as well as with high-frequency Langmuir turbulence. It is shown that such a solution and the accompanying Langmuir wave spectrum rigorously satisfy the balance requirement between the spontaneous and induced emission processes in both the particle and wave kinetic equations, and approximately satisfy the similar balance requirement between the spontaneous and induced scattering processes, which are nonlinear. In spite of the low velocity modification of the electron distribution function, it is shown that the resulting asymptotic velocity power-law index ?, where f{sub e} ? v {sup –?} is close to the average index observed during the quiet-time solar wind condition, i.e., ? ? O(6.5) whereas ?{sub average} ? 6.69, according to observation.

  20. Time-Dependent Turbulent Heating of Open Flux Tubes in the Chromosphere, Corona, and Solar Wind

    E-Print Network [OSTI]

    Woolsey, Lauren N

    2015-01-01

    We investigate several key questions of plasma heating in open-field regions of the corona that connect to the solar wind. We present results for a model of Alfven-wave-driven turbulence for three typical open magnetic field structures: a polar coronal hole, an open flux tube neighboring an equatorial streamer, and an open flux tube near a strong-field active region. We compare time-steady, one-dimensional turbulent heating models (Cranmer et al., 2007) against fully time-dependent three-dimensional reduced-magnetohydrodynamics modeling of BRAID (van Ballegooijen et al., 2011). We find that the time-steady results agree well with time-averaged results from BRAID. The time-dependence allows us to investigate the variability of the magnetic fluctuations and of the heating in the corona. The high-frequency tail of the power spectrum of fluctuations forms a power law whose exponent varies with height, and we discuss the possible physical explanation for this behavior. The variability in the heating rate is bursty...

  1. Interplanetary Scintillation Observations of Stream Interaction Regions in the Solar Wind

    E-Print Network [OSTI]

    Bisi, M. M.; Fallows, R. A.; Breen, A. R.; O’Neill, I. J.

    2010-01-01

    persist for more than one solar rotation – have long beenscintillation from one of the IPS Observations of Solar Windone Carrington rotation of in-situ data. The Sun is now at solar

  2. Comment on"Air Emissions Due to Wind and Solar Power" and Supporting Information

    SciTech Connect (OSTI)

    Mills, Andrew D.; Wiser, Ryan H.; Milligan, Michael; O'Malley, Mark

    2009-03-18

    Katzenstein and Apt investigate the important question of pollution emission reduction benefits from variable generation resources such as wind and solar. Their methodology, which couples an individual variable generator to a dedicated gas plant to produce a flat block of power is, however, inappropriate. For CO{sub 2}, the authors conclude that variable generators 'achieve {approx} 80% of the emission reductions expected if the power fluctuations caused no additional emissions.' They find even lower NO{sub x} emission reduction benefits with steam-injected gas turbines and a 2-4 times net increase in NO{sub x} emissions for systems with dry NO{sub x} control unless the ratio of energy from natural gas to variable plants is greater than 2:1. A more appropriate methodology, however, would find a significantly lower degradation of the emissions benefit than suggested by Katzenstein and Apt. As has been known for many years, models of large power system operations must take into account variable demand and the unit commitment and economic dispatch functions that are practiced every day by system operators. It is also well-known that every change in wind or solar power output does not need to be countered by an equal and opposite change in a dispatchable resource. The authors recognize that several of their assumptions to the contrary are incorrect and that their estimates therefore provide at best an upper bound to the emissions degradation caused by fluctuating output. Yet they still present the strong conclusion: 'Carbon dioxide emissions reductions are likely to be 75-80% of those presently assumed by policy makers. We have shown that the conventional method used to calculate emissions is inaccurate, particularly for NO{sub x} emissions.' The inherently problematic methodology used by the authors makes such strong conclusions suspect. Specifically, assuming that each variable plant requires a dedicated natural gas backup plant to create a flat block of power ignores the benefits of diversity. In real power systems, operators are required to balance only the net variations of all loads and all generators, not the output of individual loads or generators; doing otherwise would ensure an enormous amount of unnecessary investment and operating costs. As a result, detailed studies that aggregate the variability of all loads and generators to the system level find that the amount of operating reserves required to reliably integrate variable resources into the grid are on the order of 10% of the nameplate capacity of the variable generators, even when upto25%of gross demand is being met by variable generation. The authors implicit assumption that incremental operating reserves must be 100% of the nameplate capacity of the variable generation, and be available at all times to directly counter that variability, excludes the option of decommitting conventional units when the load net of variable generation is low. In real power systems, generation response to wind variation can typically be met by a combination of committed units, each operating at a relatively efficient point of their fuel curves. In the Supporting Information, we conceptually demonstrate that the CO{sub 2} and NO{sub x} efficiency penalty found by the authors can be significantly reduced by considering the unit commitment decision with just five plants. Real systems often have tens to hundreds of plants that can be committed and decommitted over various time frames. Ignoring the flexibility of the unit commitment decision therefore leads to unsupportable results. Anumber of analyses of the fuel savings and CO{sub 2} emission benefits of variable generation have considered realistic operating reserve requirements and unit commitment decisions in models that include the reduction in part load efficiency of conventional plants. The efficiency penalty due to the variability of wind in four studies considered by Gross et al. is negligible to 7%, for up to a 20% wind penetration level. In short, for moderate wind penetration levels, 'there is no evidence available to

  3. Appeared in 1999 ASME Wind Energy Symp, 37th ASME/AIAA Annual Mtg. Submitted for review, Journal of Solar Energy, ASME.

    E-Print Network [OSTI]

    Sweetman, Bert

    Appeared in 1999 ASME Wind Energy Symp, 37th ASME/AIAA Annual Mtg. Submitted for review, Journal of Solar Energy, ASME. MOMENT-BASED LOAD AND RESPONSE MODELS WITH WIND ENGINEERING APPLICATIONS Steven R characterizes the short-term loads and responses by a few summary statistics: speci#12;cally, by a limited num

  4. Structure and dynamics of the solar wind/ionosphere interface on Mars: MEX-ASPERA-3 and MEX-MARSIS observations

    E-Print Network [OSTI]

    Gurnett, Donald A.

    mass and charge) in the energy range 0.01­36 keV/q. The ELS sensor measures 2D distributions ofStructure and dynamics of the solar wind/ionosphere interface on Mars: MEX-ASPERA-3 and MEX wind plasmas and the magnetic field strength carried out by the ASPERA-3 and MARSIS experiments onboard

  5. CONNECTING THE SUN AND THE SOLAR WIND: THE FIRST 2.5-DIMENSIONAL SELF-CONSISTENT MHD SIMULATION UNDER THE ALFVEN WAVE SCENARIO

    SciTech Connect (OSTI)

    Matsumoto, Takuma; Suzuki, Takeru Ken

    2012-04-10

    The solar wind emanates from the hot and tenuous solar corona. Earlier studies using 1.5-dimensional simulations show that Alfven waves generated in the photosphere play an important role in coronal heating through the process of nonlinear mode conversion. In order to understand the physics of coronal heating and solar wind acceleration together, it is important to consider the regions from photosphere to interplanetary space as a single system. We performed 2.5-dimensional, self-consistent magnetohydrodynamic simulations, covering from the photosphere to the interplanetary space for the first time. We carefully set up the grid points with spherical coordinates to treat the Alfven waves in the atmosphere with huge density contrast and successfully simulate the solar wind streaming out from the hot solar corona as a result of the surface convective motion. The footpoint motion excites Alfven waves along an open magnetic flux tube, and these waves traveling upward in the non-uniform medium undergo wave reflection, nonlinear mode conversion from Alfven mode to slow mode, and turbulent cascade. These processes lead to the dissipation of Alfven waves and acceleration of the solar wind. It is found that the shock heating by the dissipation of the slow-mode wave plays a fundamental role in the coronal heating process, whereas the turbulent cascade and shock heating drive the solar wind.

  6. Solid State Lighting: GATEWAY and CALiPER

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

    National Laboratory Marc.Ledbetter@pnnl.gov 503.417.7557 April 3, 2013 Solid State Lighting: GATEWAY & CALiPER Solid State Lighting: GATEWAY & CALiPER 2 | Building Technologies...

  7. Analyzing and simulating the variability of solar irradiance and solar PV powerplants

    E-Print Network [OSTI]

    Lave, Matthew S.

    2012-01-01

    output of distant wind turbines, Wind Energy, 7 (2004) 75-dispersed wind turbine systems, Solar energy. , 50 (1993)

  8. Text-Alternative Version: Smithsonian GATEWAY Demonstration Video

    Broader source: Energy.gov [DOE]

    Following is a text version of a video about the GATEWAY demonstration project at the Smithsonian American Art Museum.

  9. White Knights: Will wind and solar come to the rescue of a looming capacity gap from nuclear phase-out or

    E-Print Network [OSTI]

    Paris-Sud XI, Université de

    rapidly but faces grid integration problems; yet the cost of PV solar panels has plummeted thanks1 White Knights: Will wind and solar come to the rescue of a looming capacity gap from nuclear. Carbon capture and storage (CCS) technology has yet to become a commercially viable technology

  10. Where, when and how much solar is available? A provincial-scale solar resource assessment for China

    E-Print Network [OSTI]

    He, G; Kammen, DM

    2016-01-01

    and optimization of solar and other complimentary resources, such as solar and wind, solar and storage, solar and hydro,

  11. Magnetohydrodynamic slow mode with drifting He{sup ++}: Implications for coronal seismology and the solar wind

    SciTech Connect (OSTI)

    Hollweg, Joseph V.; Verscharen, Daniel; Chandran, Benjamin D. G. E-mail: daniel.verscharen@unh.edu

    2014-06-10

    The MHD slow mode wave has application to coronal seismology, MHD turbulence, and the solar wind where it can be produced by parametric instabilities. We consider analytically how a drifting ion species (e.g. He{sup ++}) affects the linear slow mode wave in a mainly electron-proton plasma, with potential consequences for the aforementioned applications. Our main conclusions are as follows. 1. For wavevectors highly oblique to the magnetic field, we find solutions that are characterized by very small perturbations of total pressure. Thus, our results may help to distinguish the MHD slow mode from kinetic Alfvén waves and non-propagating pressure-balanced structures, which can also have very small total pressure perturbations. 2. For small ion concentrations, there are solutions that are similar to the usual slow mode in an electron-proton plasma, and solutions that are dominated by the drifting ions, but for small drifts the wave modes cannot be simply characterized. 3. Even with zero ion drift, the standard dispersion relation for the highly oblique slow mode cannot be used with the Alfvén speed computed using the summed proton and ion densities, and with the sound speed computed from the summed pressures and densities of all species. 4. The ions can drive a non-resonant instability under certain circumstances. For low plasma beta, the threshold drift can be less than that required to destabilize electromagnetic modes, but damping from the Landau resonance can eliminate this instability altogether, unless T{sub e} /T{sub p} >> 1.

  12. Utility-Scale Wind & Solar Power in the U.S.: Where it stands...

    Energy Savers [EERE]

    solar market has been dominated in recent years by Feed-in-Tariffs (FiT) in Western Europe * At year-end 2013, just over 70 GW of utility-scale and rooftop solar PV was...

  13. Comment on "Air Emissions Due to Wind and Solar Power" and Supporting Information

    E-Print Network [OSTI]

    Mills, Andrew D.

    2011-01-01

    Berkeley, CA, National Renewable Energy Laboratory, Golden,Energy Ef?ciency and Renewable Energy (Wind & Hy- dropowerwith the National Renewable Energy S12 Andrew Mills et al.

  14. Power law burst and inter-burst interval distributions in the solar wind: turbulence or dissipative SOC ?

    E-Print Network [OSTI]

    M. P. Freeman; N. W. Watkins; D. J. Riley

    2000-06-28

    We calculate for the first time the probability density functions (PDFs) P of burst energy e, duration T and inter-burst interval tau for a known turbulent system in nature. Bursts in the earth-sun component of the Poynting flux at 1 AU in the solar wind were measured using the MFI and SWE experiments on the NASA WIND spacecraft. We find P(e) and P(T) to be power laws, consistent with self-organised criticality (SOC). We find also a power law form for P(tau) that distinguishes this turbulent cascade from the exponential P(tau) of ideal SOC, but not from some other SOC-like sandpile models. We discuss the implications for the relation between SOC and turbulence.

  15. ELECTRON HEAT FLUX IN THE SOLAR WIND: ARE WE OBSERVING THE COLLISIONAL LIMIT IN THE 1 AU DATA?

    SciTech Connect (OSTI)

    Landi, S.; Matteini, L.; Pantellini, F.

    2014-07-20

    Using statistically significant data at 1 AU, it has recently been shown (Bale et al.) that in the solar wind, when the Knudsen number K {sub T} (the ratio between the electron mean free path and the electron temperature scale height) drops below about 0.3, the electron heat flux q intensity rapidly approaches the classical collisional Spitzer-Härm limit. Using a fully kinetic model including the effect of Coulomb collisions and the expansion of the solar wind with heliocentric distance, we observe that the heat flux strength does indeed approach the collisional value for Knudsen numbers smaller than about 0.3 in very good agreement with the observations. However, closer inspection of the heat flux properties, such as its variation with the heliocentric distance and its dependence on the plasma parameters, shows that for Knudsen numbers between 0.02 and 0.3 the heat flux is not conveniently described by the Spitzer-Härm formula. We conclude that even though observations at 1 AU seem to indicate that the electron heat flux intensity approaches the collisional limit when the Knudsen drops below ?0.3, the collisional limit is not a generally valid closure for a Knudsen larger than 0.01. Moreover, the good agreement between the heat flux from our model and the heat flux from solar wind measurements in the high-Knudsen number regime seems to indicate that the heat flux at 1 AU is not constrained by electromagnetic instabilities as both wave-particle and wave-wave interactions are neglected in our calculations.

  16. Drivers for the Value of Demand Response under Increased Levels of Wind and Solar Power; NREL (National Renewable Energy Laboratory)

    SciTech Connect (OSTI)

    Hale, Elaine

    2015-07-30

    Demand response may be a valuable flexible resource for low-carbon electric power grids. However, there are as many types of possible demand response as there are ways to use electricity, making demand response difficult to study at scale in realistic settings. This talk reviews our state of knowledge regarding the potential value of demand response in several example systems as a function of increasing levels of wind and solar power, sometimes drawing on the analogy between demand response and storage. Overall, we find demand response to be promising, but its potential value is very system dependent. Furthermore, demand response, like storage, can easily saturate ancillary service markets.

  17. Mitigating the effects of intermittency and variability of wind and solar power

    E-Print Network [OSTI]

    Lavaei, Javad

    farms are broken into two general categories: onshore and offshore. Onshore wind farms are built on land different characteristics. Wind speed is less variable for offshore farms than it is for onshore farms, while offshore farms are built over bodies of water. Though the operation of the turbines is identical

  18. Geek-Up[4.29.2011]: Boosting the Efficiency of Wind and Solar Power

    Broader source: Energy.gov [DOE]

    It’s a big month for the National Wind Technology Center.   Earlier this week, the Department of Energy’s National Renewable Energy Laboratory (NREL) commemorated the successful installation and full capacity operation of a 3 megawatt Alstom ECO 100 wind turbine at the center. As part of a long-term collaboration between NREL and Alstom, engineers from the two institutions will perform a series of analyses and tests to evaluate Alstom’s unique drive train configuration technology.   After this initial testing is complete, the joint team will continue research and development on other advanced technologies including controls and offshore wind energy.   Researchers from the Department’s Lawrence Livermore National Laboratory (LLNL) will also be hanging out at the National Wind Technology Center in the coming months. They’re launching a study to improve the efficiency of wind farms.  

  19. A nuclear wind/solar oil-shale system for variable electricity and liquid fuels production

    SciTech Connect (OSTI)

    Forsberg, C.

    2012-07-01

    The recoverable reserves of oil shale in the United States exceed the total quantity of oil produced to date worldwide. Oil shale contains no oil, rather it contains kerogen which when heated decomposes into oil, gases, and a carbon char. The energy required to heat the kerogen-containing rock to produce the oil is about a quarter of the energy value of the recovered products. If fossil fuels are burned to supply this energy, the greenhouse gas releases are large relative to producing gasoline and diesel from crude oil. The oil shale can be heated underground with steam from nuclear reactors leaving the carbon char underground - a form of carbon sequestration. Because the thermal conductivity of the oil shale is low, the heating process takes months to years. This process characteristic in a system where the reactor dominates the capital costs creates the option to operate the nuclear reactor at base load while providing variable electricity to meet peak electricity demand and heat for the shale oil at times of low electricity demand. This, in turn, may enable the large scale use of renewables such as wind and solar for electricity production because the base-load nuclear plants can provide lower-cost variable backup electricity. Nuclear shale oil may reduce the greenhouse gas releases from using gasoline and diesel in half relative to gasoline and diesel produced from conventional oil. The variable electricity replaces electricity that would have been produced by fossil plants. The carbon credits from replacing fossil fuels for variable electricity production, if assigned to shale oil production, results in a carbon footprint from burning gasoline or diesel from shale oil that may half that of conventional crude oil. The U.S. imports about 10 million barrels of oil per day at a cost of a billion dollars per day. It would require about 200 GW of high-temperature nuclear heat to recover this quantity of shale oil - about two-thirds the thermal output of existing nuclear reactors in the United States. With the added variable electricity production to enable renewables, additional nuclear capacity would be required. (authors)

  20. Analyzing and simulating the variability of solar irradiance and solar PV powerplants

    E-Print Network [OSTI]

    Lave, Matthew S.

    2012-01-01

    The intermittency of wind, solar, and renewable electricitySolar Variabiltiy and Interconnection Locations, World Renewableharnessing renewable energy sources such as wind and solar

  1. MULTI-SPACECRAFT OBSERVATIONS OF LINEAR MODES AND SIDEBAND WAVES IN ION-SCALE SOLAR WIND TURBULENCE

    SciTech Connect (OSTI)

    Perschke, Christopher; Motschmann, Uwe; Narita, Yasuhito; Glassmeier, Karl-Heinz

    2014-10-01

    In the scenario of weak turbulence, energy is believed to be cascaded from smaller to larger wave numbers and frequencies due to weak wave-wave interactions. Based on its perturbative treatment one may regard plasma turbulence as a superposition of linear modes (or normal modes) and sideband waves (or nonlinear modes). In this study, we use magnetic field and plasma measurements of nine solar wind events obtained by the Cluster spacecraft and make extensive use of a high-resolution wave vector analysis method, the Multi-point Signal Resonator technique, to find frequencies and wave vectors of discrete modes on ion kinetic scales in the plasma rest frame. The primarily unstructured wave observations in the frequency-wave number diagram are classified into three distinct linear modes (proton Bernstein modes, helium-alpha Bernstein modes, and kinetic Alfvén waves) and the sideband waves by comparing with the dispersion relations derived theoretically from linear Vlasov theory using observational values of the plasma parameter beta and the propagation angle from the mean magnetic field. About 60% of the observed discrete modes can be explained by the linear modes, primarily as the proton Bernstein and the kinetic Alfvén waves, within the frequency uncertainties, while the rest of the population (about 40%) cannot be classified as linear modes due to the large deviation from dispersion relations. We conclude that both the linear modes and sideband wave components are needed to construct the wave picture of solar wind turbulence on ion-kinetic scales.

  2. TRANSPORT OF THE FIRST ROCKS OF THE SOLAR SYSTEM BY X-WINDS

    E-Print Network [OSTI]

    Hu, Renyu

    It has been suggested that chondrules and calcium-aluminum-rich inclusions (CAIs) were formed at the inner edge of the protoplanetary disk and then entrained in magnetocentrifugal X-winds. We study trajectories of such ...

  3. Energy Transfer via Solar Wind Driven Ultra Low Frequency Waves in the Earth's Magnetosphere

    E-Print Network [OSTI]

    Hartinger, Michael David

    2012-01-01

    wind to various sinks of wave energy in the magnetosphere.magnetosphere (where wave energy can exit the magnetospheresource and a sink for ULF wave energy. One of the most well-

  4. Analyzing and simulating the variability of solar irradiance and solar PV powerplants

    E-Print Network [OSTI]

    Lave, Matthew S.

    2012-01-01

    in spatially dispersed wind turbine systems, Solar energy. ,Smoothing effects of distributed wind turbines. Part 2.power output of distant wind turbines, Wind Energy, 7 (2004)

  5. Summary of Time Period-Based and Other Approximation Methods for Determining the Capacity Value of Wind and Solar in the United States: September 2010 - February 2012

    SciTech Connect (OSTI)

    Rogers, J.; Porter, K.

    2012-03-01

    This paper updates previous work that describes time period-based and other approximation methods for estimating the capacity value of wind power and extends it to include solar power. The paper summarizes various methods presented in utility integrated resource plans, regional transmission organization methodologies, regional stakeholder initiatives, regulatory proceedings, and academic and industry studies. Time period-based approximation methods typically measure the contribution of a wind or solar plant at the time of system peak - sometimes over a period of months or the average of multiple years.

  6. BASSET: Scalable Gateway Finder in Large Graphs

    SciTech Connect (OSTI)

    Tong, H; Papadimitriou, S; Faloutsos, C; Yu, P S; Eliassi-Rad, T

    2010-11-03

    Given a social network, who is the best person to introduce you to, say, Chris Ferguson, the poker champion? Or, given a network of people and skills, who is the best person to help you learn about, say, wavelets? The goal is to find a small group of 'gateways': persons who are close enough to us, as well as close enough to the target (person, or skill) or, in other words, are crucial in connecting us to the target. The main contributions are the following: (a) we show how to formulate this problem precisely; (b) we show that it is sub-modular and thus it can be solved near-optimally; (c) we give fast, scalable algorithms to find such gateways. Experiments on real data sets validate the effectiveness and efficiency of the proposed methods, achieving up to 6,000,000x speedup.

  7. JOURNAL OF GEOPHYSICAL RESEARCH: SPACE PHYSICS, VOL. 118, 112, doi:10.1002/2013JA019188, 2013 Prediction of the AU, AL, and AE indices using solar wind parameters

    E-Print Network [OSTI]

    Li, Xinlin

    Prediction of the AU, AL, and AE indices using solar wind parameters Bingxian Luo,1,2 Xinlin Li,2 M. Temerin] An empirical model that predicts the AU index, a measure of the Earth's east electrojet, derived from with the AU model, produces an AE model. All models are based on solar wind and interplanetary magnetic field

  8. PSW1-C0.2-D0.1-E2.4-F0.1-PSRB2-0021-02 SOLAR WIND-DRIVEN ELECTRON RADIATION BELT

    E-Print Network [OSTI]

    PSW1-C0.2-D0.1-E2.4-F0.1-PSRB2-0021-02 SOLAR WIND-DRIVEN ELECTRON RADIATION BELT RESPONSE FUNCTIONS linear filters, to remove unwanted "col- ored noise" from solar wind and radiation belt electron data prediction filters to represent the driven portion of the linear dynamics that describe the coupling between

  9. Spectral Features of Magnetic Fluctuations at Proton Scales from Fast to Slow Solar Wind

    E-Print Network [OSTI]

    Bruno, R

    2015-01-01

    This Letter investigates the spectral characteristics of the interplanetary magnetic field fluctuations at proton scales during several time intervals chosen along the speed profile of a fast stream. The character of the fluctuations within the first frequency decade, beyond the high frequency break located between the fluid and the kinetic regime, strongly depends on the type of wind. While the fast wind shows a clear signature of both right handed and left handed polarized fluctuations, possibly associated with KAW and Ion-Cyclotron waves, respectively, the rarefaction region, where the wind speed and the Alfv\\'{e}nicity of low frequency fluctuations decrease, shows a rapid disappearance of the ion-cyclotron signature followed by a more gradual disappearance of the KAWs. Moreover, also the power associated to perpendicular and parallel fluctuations experiences a rapid depletion, keeping, however, the power anisotropy in favour of the perpendicular spectrum.

  10. T-701: Citrix Access Gateway Enterprise Edition Input Validation...

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

    ABSTRACT: Citrix Access Gateway Enterprise Edition Input Validation Flaw in Logon Portal Permits Cross-Site Scripting Attacks. reference LINKS: SecurityTracker Alert ID:...

  11. V-153: Symantec Brightmail Gateway Input Validation Flaw Permits...

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

    T-701: Citrix Access Gateway Enterprise Edition Input Validation Flaw in Logon Portal Permits Cross-Site Scripting Attacks U-001:Symantec IM Manager Input Validation Flaws...

  12. DOE Publishes GATEWAY Report on Pedestrian Friendly Outdoor Lighting...

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

    Energy (DOE) has published a new GATEWAY report entitled Pedestrian Friendly Outdoor Lighting. Recognizing that pedestrian lighting has different criteria for success than street...

  13. V-106: Citrix Access Gateway Unspecified Security Bypass Vulnerability

    Broader source: Energy.gov [DOE]

    A vulnerability has been reported in Citrix Access Gateway, which can be exploited by malicious people to bypass certain security restrictions.

  14. Alaska Gateway School District Adopts Combined Heat and Power...

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

    Tok, Alaska, the economic impact of high fuel prices was crippling the community's economy, especially for the Alaska Gateway School District, with staff laid off and double...

  15. Solar wind and geomagnetism: toward a standard classification of geomagnetic activity from 1868 to 2009

    E-Print Network [OSTI]

    Zerbo, J. L.

    We examined solar activity with a large series of geomagnetic data from 1868 to 2009. We have revisited the geomagnetic activity classification scheme of Legrand and Simon (1989) and improve their scheme by lowering the ...

  16. Wind Energy Data and Information Gateway (WENDI) | 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 JEnvironmental Jump to:EAand Dalton Jump to: navigation, search Name: Wilson andAmerica

  17. Submitted to Journal of Geophysical Research (Space Physics): September 21, 2000. Heating of the Low-Latitude Solar Wind by Dissipation

    E-Print Network [OSTI]

    Richardson, John

    of magnetic uctuation energy in the solar wind and the related dissipation and heating of the ambient ion. For this reason, there is a natural limit to the heating rate Schwartz et al., 1981]. The tur- bulence viewpoint mechanism. The heating rate is at least partially dictated by the spectral transfer rate from the large

  18. Cost-minimized combinations of wind power, solar power and electrochemical storage, powering the grid up to 99.9% of the time

    E-Print Network [OSTI]

    Firestone, Jeremy

    Cost-minimized combinations of wind power, solar power and electrochemical storage, powering the grid up to 99.9% of the time Cory Budischak a,b,*, DeAnna Sewell c , Heather Thomson c , Leon Mach d, Newark, DE 19713, USA c Center for Carbon-Free Power Integration, School of Marine Science and Policy

  19. A model for the non-universal power-law of the solar wind sub-ion scale magnetic spectrum

    E-Print Network [OSTI]

    Passot, T

    2015-01-01

    A phenomenological turbulence model for kinetic Alfv\\'en waves in a magnetized collisionless plasma, able to reproduce the non-universal power-law spectra observed at the sub-ion scales in the solar wind and the terrestrial magnetosphere, is presented. Nonlocal interactions are retained, and critical balance, characteristic of a strong turbulence regime, establishes dynamically as the cascade proceeds. The process of temperature homogenization along distorted magnetic field lines, induced by Landau damping, affects the turbulence transfer time and results in a steepening of the sub-ion power-law spectrum of critically-balanced turbulence, whose exponent is in particular sensitive to the ratio between the Alfv\\'en wave period and the nonlinear timescale.

  20. Power Flow Controller for Renewables: Transformer-less Unified Power Flow Controller for Wind and Solar Power Transmission

    SciTech Connect (OSTI)

    2012-02-08

    GENI Project: MSU is developing a power flow controller to improve the routing of electricity from renewable sources through existing power lines. The fast, innovative, and lightweight circuitry that MSU is incorporating into its controller will eliminate the need for a separate heavy and expensive transformer, as well as the construction of new transmission lines. MSU’s controller is better suited to control power flows from distributed and intermittent wind and solar power systems than traditional transformer-based controllers are, so it will help to integrate more renewable energy into the grid. MSU‘s power flow controller can be installed anywhere in the existing grid to optimize energy transmission and help reduce transmission congestion.

  1. PICKUP ION MEDIATED PLASMAS. I. BASIC MODEL AND LINEAR WAVES IN THE SOLAR WIND AND LOCAL INTERSTELLAR MEDIUM

    SciTech Connect (OSTI)

    Zank, G. P.; Hunana, P.; Mostafavi, P.; Goldstein, M. L.

    2014-12-20

    Pickup ions (PUIs) in the outer heliosphere and the local interstellar medium are created by charge exchange between protons and hydrogen (H) atoms, forming a thermodynamically dominant component. In the supersonic solar wind beyond >10 AU, in the inner heliosheath (IHS), and in the very local interstellar medium (VLISM), PUIs do not equilibrate collisionally with the background plasma. Using a collisionless form of Chapman-Enskog expansion, we derive a closed system of multi-fluid equations for a plasma comprised of thermal protons and electrons, and suprathermal PUIs. The PUIs contribute an isotropic scalar pressure to leading order, a collisionless heat flux at the next order, and a collisionless stress tensor at the second-order. The collisionless heat conduction and viscosity in the multi-fluid description results from a non-isotropic PUI distribution. A simpler one-fluid MHD-like system of equations with distinct equations of state for both the background plasma and the PUIs is derived. We investigate linear wave properties in a PUI-mediated three-fluid plasma model for parameters appropriate to the VLISM, the IHS, and the solar wind in the outer heliosphere. Five distinct wave modes are possible: Alfvén waves, thermal fast and slow magnetoacoustic waves, PUI fast and slow magnetoacoustic waves, and an entropy mode. The thermal and PUI acoustic modes propagate at approximately the combined thermal magnetoacoustic speed and the PUI sound speed respectively. All wave modes experience damping by the PUIs through the collisionless PUI heat flux. The PUI-mediated plasma model yields wave properties, including Alfvén waves, distinctly different from those of the standard two-fluid model.

  2. Cosmic ray transport in heliospheric magnetic structures. I. Modeling background solar wind using the CRONOS magnetohydrodynamic code

    SciTech Connect (OSTI)

    Wiengarten, T.; Kleimann, J.; Fichtner, H.; Kühl, P.; Kopp, A.; Heber, B.; Kissmann, R.

    2014-06-10

    The transport of energetic particles such as cosmic rays is governed by the properties of the plasma being traversed. While these properties are rather poorly known for galactic and interstellar plasmas due to the lack of in situ measurements, the heliospheric plasma environment has been probed by spacecraft for decades and provides a unique opportunity for testing transport theories. Of particular interest for the three-dimensional (3D) heliospheric transport of energetic particles are structures such as corotating interaction regions, which, due to strongly enhanced magnetic field strengths, turbulence, and associated shocks, can act as diffusion barriers on the one hand, but also as accelerators of low energy CRs on the other hand as well. In a two-fold series of papers, we investigate these effects by modeling inner-heliospheric solar wind conditions with a numerical magnetohydrodynamic (MHD) setup (this paper), which will serve as an input to a transport code employing a stochastic differential equation approach (second paper). In this first paper, we present results from 3D MHD simulations with our code CRONOS: for validation purposes we use analytic boundary conditions and compare with similar work by Pizzo. For a more realistic modeling of solar wind conditions, boundary conditions derived from synoptic magnetograms via the Wang-Sheeley-Arge (WSA) model are utilized, where the potential field modeling is performed with a finite-difference approach in contrast to the traditional spherical harmonics expansion often utilized in the WSA model. Our results are validated by comparing with multi-spacecraft data for ecliptical (STEREO-A/B) and out-of-ecliptic (Ulysses) regions.

  3. Print http://us.mg4.mail.yahoo.com/neo/launch?.rand=deOsgk04ks40i Subject: RE: [s-w-h] b Solar verses wind efficiency

    E-Print Network [OSTI]

    .yahoo.com/neo/launch?.rand=deOsgk04ks40i Subject: RE: [s-w-h] b Solar verses wind efficiency From: Michael Klemen (wind4energy;Print http://us.rng4.mail.yahoo.comlneo/launch?.rand=deOsgko4ks4 energy in the wind is proportional://www.ndsu.edu/ndsu/klemen/Perfect_Turbine.htm You can see that for an ideal real life wind turbine ("good turbine") the increase in energy

  4. Solar Impulsive Energetic Electron Events

    E-Print Network [OSTI]

    Wang, Linghua

    2009-01-01

    coronal mass ejections and solar energetic proton events, J.Voyager observations of solar wind proton temperature:1- 10Howard (2004), Variability of solar eruptions during cycle

  5. Ion kinetic energy conservation and magnetic field strength constancy in multi-fluid solar wind Alfv\\'enic turbulence

    E-Print Network [OSTI]

    Matteini, L; Pantellini, F; Velli, M; Schwartz, S J

    2015-01-01

    We investigate properties of the plasma fluid motion in the large amplitude low frequency fluctuations of highly Alfv\\'enic fast solar wind. We show that protons locally conserve total kinetic energy when observed from an effective frame of reference comoving with the fluctuations. For typical properties of the fast wind, this frame can be reasonably identified by alpha particles, which, owing to their drift with respect to protons at about the Alfv\\'en speed along the magnetic field, do not partake in the fluid low frequency fluctuations. Using their velocity to transform proton velocity into the frame of Alfv\\'enic turbulence, we demonstrate that the resulting plasma motion is characterized by a constant absolute value of the velocity, zero electric fields, and aligned velocity and magnetic field vectors as expected for unidirectional Alfv\\'enic fluctuations in equilibrium. We propose that this constraint, via the correlation between velocity and magnetic field in Alfv\\'enic turbulence, is at the origin of ...

  6. RADIAL DEPENDENCE OF THE FREQUENCY BREAK BETWEEN FLUID AND KINETIC SCALES IN THE SOLAR WIND FLUCTUATIONS

    SciTech Connect (OSTI)

    Bruno, R.; Trenchi, L.

    2014-06-01

    We investigate the radial dependence of the spectral break separating the inertial from the dissipation range in power density spectra of interplanetary magnetic field fluctuations, between 0.42 and 5.3 AU, during radial alignments between MESSENGER and WIND for the inner heliosphere and between WIND and ULYSSES for the outer heliosphere. We found that the spectral break moves to higher and higher frequencies as the heliocentric distance decreases. The radial dependence of the corresponding wavenumber is of the kind ? {sub b} ? R {sup –1.08}, in good agreement with that of the wavenumber derived from the linear resonance condition for proton cyclotron damping. These results support conclusions from previous studies which suggest that a cyclotron-resonant dissipation mechanism must participate in the spectral cascade together with other possible kinetic noncyclotron-resonant mechanisms.

  7. Wind and Solar Energy Curtailment: Experience and Practices in the United States

    SciTech Connect (OSTI)

    Bird, L.; Cochran, J.; Wang, X.

    2014-03-01

    This report examines U.S. curtailment practices, with a particular emphasis on utilities in the Western states. The information presented here is based on a series of interviews conducted with utilities, system operators, wind energy developers, and non-governmental organizations. The report provides case studies of curtailment experience and examines the reasons for curtailment, curtailment procedures, compensation, and practices that can minimize curtailment.

  8. Residential Solar and Wind Energy Systems Tax Credit | 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 RankADVANCED MANUFACTURINGEnergy BillsNo. 195 - Oct.7, 2015VerizonResidentialRebateTaxforRewardsTaxand Wind

  9. SPECTRAL SLOPE VARIATION AT PROTON SCALES FROM FAST TO SLOW SOLAR WIND

    SciTech Connect (OSTI)

    Bruno, R.; Trenchi, L.; Telloni, D.

    2014-09-20

    We investigated the behavior of the spectral slope of interplanetary magnetic field fluctuations at proton scales for selected high-resolution time intervals from the WIND and MESSENGER spacecraft at 1 AU and 0.56 AU, respectively. The analysis was performed within the profile of high-speed streams, moving from fast to slow wind regions. The spectral slope showed a large variability between –3.75 and –1.75 and a robust tendency for this parameter to be steeper within the trailing edge, where the speed is higher, and to be flatter within the subsequent slower wind, following a gradual transition between these two states. The value of the spectral index seems to depend firmly on the power associated with the fluctuations within the inertial range; the higher the power, the steeper the slope. Our results support previous analyses suggesting that there must be some response of the dissipation mechanism to the level of the energy transfer rate along the inertial range.

  10. High-performance parallel interface to synchronous optical network gateway

    DOE Patents [OSTI]

    St. John, W.B.; DuBois, D.H.

    1996-12-03

    Disclosed is a system of sending and receiving gateways interconnects high speed data interfaces, e.g., HIPPI interfaces, through fiber optic links, e.g., a SONET network. An electronic stripe distributor distributes bytes of data from a first interface at the sending gateway onto parallel fiber optics of the fiber optic link to form transmitted data. An electronic stripe collector receives the transmitted data on the parallel fiber optics and reforms the data into a format effective for input to a second interface at the receiving gateway. Preferably, an error correcting syndrome is constructed at the sending gateway and sent with a data frame so that transmission errors can be detected and corrected in a real-time basis. Since the high speed data interface operates faster than any of the fiber optic links the transmission rate must be adapted to match the available number of fiber optic links so the sending and receiving gateways monitor the availability of fiber links and adjust the data throughput accordingly. In another aspect, the receiving gateway must have sufficient available buffer capacity to accept an incoming data frame. A credit-based flow control system provides for continuously updating the sending gateway on the available buffer capacity at the receiving gateway. 7 figs.

  11. High-performance parallel interface to synchronous optical network gateway

    DOE Patents [OSTI]

    St. John, Wallace B. (Los Alamos, NM); DuBois, David H. (Los Alamos, NM)

    1996-01-01

    A system of sending and receiving gateways interconnects high speed data interfaces, e.g., HIPPI interfaces, through fiber optic links, e.g., a SONET network. An electronic stripe distributor distributes bytes of data from a first interface at the sending gateway onto parallel fiber optics of the fiber optic link to form transmitted data. An electronic stripe collector receives the transmitted data on the parallel fiber optics and reforms the data into a format effective for input to a second interface at the receiving gateway. Preferably, an error correcting syndrome is constructed at the sending gateway and sent with a data frame so that transmission errors can be detected and corrected in a real-time basis. Since the high speed data interface operates faster than any of the fiber optic links the transmission rate must be adapted to match the available number of fiber optic links so the sending and receiving gateways monitor the availability of fiber links and adjust the data throughput accordingly. In another aspect, the receiving gateway must have sufficient available buffer capacity to accept an incoming data frame. A credit-based flow control system provides for continuously updating the sending gateway on the available buffer capacity at the receiving gateway.

  12. Assessment of Wind/Solar Co-Located Generation in Texas

    Broader source: Energy.gov [DOE]

    As part of the Solar America Cities program, Austin Energy proposed to perform an assessment of the rooftop area available for PV development within its service area. Austin Energy contracted with Clean Energy Associates (CEA) to perform the analysis. This report summarizes the project objectives, data sources and methodological approach employed, and results.

  13. On the Parallel and Perpendicular Propagating Motions Visible in Polar Plumes: An Incubator For (Fast) Solar Wind Acceleration?

    E-Print Network [OSTI]

    Liu, Jiajia; De Moortel, Ineke; Wang, Yuming

    2015-01-01

    We combine observations of the Coronal Multi-channel Polarimeter (CoMP) and the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) to study the characteristic properties of (propagating) Alfvenic motions and quasi-periodic intensity disturbances in polar plumes. This unique combination of instruments highlights the physical richness of the processes taking place at the base of the (fast) solar wind. The (parallel) intensity perturbations with intensity enhancements around 1% have an apparent speed of 120 km/s (in both the 171A and 193A passbands) and a periodicity of 15 minutes, while the (perpendicular) Alfvenic wave motions have a velocity amplitude of 0.5 km/s, a phase speed of 830 km/s, and a shorter period of 5 minutes on the same structures. These observations illustrate a scenario where the excited Alfvenic motions are propagating along an inhomogeneously loaded magnetic field structure such that the combination could be a potential progenitor of the magnetohydrodynamic tur...

  14. 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.

  15. Mathematics 122 -Gateway Exam -Fall 96 The Gateway exam will consist of ten randomly chosen problems about integra-

    E-Print Network [OSTI]

    Torres, Rodolfo

    Mathematics 122 - Gateway Exam - Fall 96 The Gateway exam will consist of ten randomly nine pro* *blems without any mistakes. You need not simplify your answers, but if you do, the si* *m- plification must be error-free. If you fail to pass the exam you will be allow* *ed to retake it. When you

  16. Analyzing and simulating the variability of solar irradiance and solar PV powerplants

    E-Print Network [OSTI]

    Lave, Matthew S.

    2012-01-01

    Optimum tilt of a solar collector, Solar & Wind Technology,and orientation for solar collector in Brunei Darussalam,Optimum tilt angle for solar collectors. , Energy Sources,

  17. THE VIOLATION OF THE TAYLOR HYPOTHESIS IN MEASUREMENTS OF SOLAR WIND TURBULENCE

    SciTech Connect (OSTI)

    Klein, K. G.; Howes, G. G.; TenBarge, J. M.

    2014-08-01

    Motivated by the upcoming Solar Orbiter and Solar Probe Plus missions, qualitative and quantitative predictions are made for the effects of the violation of the Taylor hypothesis on the magnetic energy frequency spectrum measured in the near-Sun environment. The synthetic spacecraft data method is used to predict observational signatures of the violation for critically balanced Alfvénic turbulence or parallel fast/whistler turbulence. The violation of the Taylor hypothesis can occur in the slow flow regime, leading to a shift of the entire spectrum to higher frequencies, or in the dispersive regime, in which the dissipation range spectrum flattens at high frequencies. It is found that Alfvénic turbulence will not significantly violate the Taylor hypothesis, but whistler turbulence will. The flattening of the frequency spectrum is therefore a key observational signature for fast/whistler turbulence.

  18. Hybrid Solar-Wind Generates Savings for South Dakota City | Department of

    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 Natural GasAdjustmentsShirley Ann JacksonDepartment ofOffice ofofWindUpcomingcanGridDoes

  19. Wind and solar power electric generation to see strong growth over the next two years

    Gasoline and Diesel Fuel Update (EIA)

    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 Natural GasAdjustments (Billion Cubic Feet) Wyoming Dry NaturalPrices Globaldieselgasolinemonthlysummer1Net ProductionWind

  20. Solar and Wind Energy Device Franchise Tax Deduction | 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 RankADVANCED MANUFACTURINGEnergy BillsNo.Hydrogen4Energy SmoothEquipmentSolar PV