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3 edition of Modeling of the coupled magnetospheric and neutral wind dynamos found in the catalog.

Modeling of the coupled magnetospheric and neutral wind dynamos

Modeling of the coupled magnetospheric and neutral wind dynamos

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  • 38 Currently reading

Published by SRI International, National Aeronautics and Space Administration, National Technical Information Service, distributor in Menlo Park, CA, [Washington, DC, Springfield, Va .
Written in English

    Subjects:
  • Electric generators.,
  • Magnetosphere.

  • Edition Notes

    Statementsubmitted by Jeff P. Thayer.
    Series[NASA contractor report] -- NASA CR-194728., NASA contractor report -- NASA CR-194728.
    ContributionsUnited States. National Aeronautics and Space Administration.
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL14706535M

    Disclaimer. All content on this website, including dictionary, thesaurus, literature, geography, and other reference data is for informational purposes only. Theory and Modeling of Planetary Dynamos for thermal convection. Other potential sources are secular cooling and the heat production from radiogenic elements. Only the temperature variations that exceed the adiabatic gradient have to be considered in the .

    The `wind frame' sketches of Fig. 1 also represent the ion and electron motions produced by an electrostatic field in the magnetic west-to-east direction. The electric field in the ionosphere can originate in various ways (Section 4). As already discussed, an electric field is Cited by: The importance of entropy parameter PV5/3 where S is the kinetic theory definition of entropy; C 1 is a constant related to the number of particles in the flux tube, the shape of the plasma distribution function and the particle mass; C 2 is a constant related to number of particles in the flux tube [Wolf et al., ]. • In ideal MHD, PV5/3 is conserved along a flowFile Size: 5MB.

    Self-consistent modeling of magnetic fields and plasmas in the inner magnetosphere: Application to a geomagnetic storm Sorin Zaharia,1 V. K. Jordanova,2,3 M. F. Thomsen,1 and G. D. Reeves1 Received 16 January ; revised 29 May ; accepted 29 June ; published 5 October magnetospheric states causes deviations from equilibrium in such models. Therefore, for applications in which force balance is required, equilibrium configurations have to be explicitly computed. [4] Two major approaches have been developed in the area of 3-D numerical magnetospheric equilibrium model-.


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Modeling of the coupled magnetospheric and neutral wind dynamos Download PDF EPUB FB2

"Modeling of the Coupled Magnetospheric and Neutral Wind Dynamos." Over the past four years of funding, SRI, in collaboration with the University of Texas at Dallas, has been involved in assessing the influence of thermospheric neutral winds on the electric field and current systems at high latitudes.

However, the contribution of the neutral wind to the high-latitude electric field and current systems and their seasonal and local time dependence has yet to be quantitatively evaluated.

In this program, we are evaluating the coupled magneto-spheric and neutral wind dynamos at high latitudes under various conditions. For example, in. @article{osti_, title = {Modeling of the coupled magnetospheric and neutral wind dynamos.

Annual Technical status report No. 2, 1 April March}, author = {Thayer, J P and Vickrey, J F and Heelis, R A and Gary, J B}, abstractNote = {Work at SRI involved modeling the exchange of electromagnetic energy between the ionosphere and magnetosphere to help interpret the DE-B.

Get this from a library. Modeling of the coupled magnetospheric and neutral wind dynamos. [Jeffrey P Thayer; United States. National Aeronautics and Space Administration.;].

As a result of the mechanical energy stored within the neutral wind (caused in part by Lorentz--and pressure gradient--forces set up by the magnetospheric flux of electrical energy), electric currents and fields can be generated in the ionosphere through the neutral wind dynamo mechanism.

We discuss quasi-static and dynamic models of the magnetotail response to perturbations imposed by the solar wind, focusing particularly on the formation of thin current sheets, their structure and breakup. Modeling of the Magnetospheric Response to the Dynamic Solar by: 6. Birn J., Hesse M., Schindler K.

() Modeling of the Magnetospheric Response to the Dynamic Solar Wind. In: Baker D.N., Klecker B., Schwartz S.J., Schwenn R., Von Steiger R. (eds) Solar Dynamics and Its Effects on the Heliosphere and Earth.

Space Sciences Series of ISSI, vol Springer, New York, NY. Received 11 October ; Accepted 14 Cited by: 6. Results from the first Sun‐to‐Earth coupled numerical model developed at the Center for Integrated Space Weather Modeling are presented.

The model simulates physical processes occurring in space sp Cited by: CMIT is a coupled magnetosphere, ionosphere, and thermosphere model.

It includes the TIEGCM v and the Lyon-Fedder-Mobarry (LFM) global magnetohydrodynamic. That the Earth's dipole axis is offset from the Earth's spin vector by ~11 degrees and presents a changing orientation to the oncoming solar wind with a daily periodicity is well illustrated in the visuals.

Additional graphics illustrate concepts of magnetic field line reconnection and magnetospheric substorms. the magnetic field, based on magnetospheric and interplanetary data and allowing one to reproduce and forecast the entire process of a geomagnetic storm, as it unfolds in time and space.

Citation: Tsyganenko, N. A., and M. Sitnov (), Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, J.

by: A further modeling study by Huang () showed longitudinal, seasonal, and solar cycle variations of the disturbance-dynamo effects. Maruyama et al. ( Maruyama et al. (, coupled CTIPE. About Magnetospheric Field Models at CCMC. Beyond four Earth radii, the Earth's magnetic field is increasingly affected by the solar wind interaction with the earth's magnetosphere.

The distortions can be described by several external source fields caused by magnetospheric current systems. a current system in the neutral sheet of the. combined into a coupled model of the solar corona and solar wind, CORHEL model [Luhmann et al., ; Odstrcil et al., ].

The LFM model can use as the upstream boundary condition either in situ observations of the solar wind from spacecraft (i.e., ACE or Wind) or, as a component of the CISM model, the output from the CORHEL model. In the height region between about 85 and km altitude on Earth, the ionospheric plasma is electrically conducting.

Atmospheric tidal winds due to differential solar heating or due to gravitational lunar forcing move the ionospheric plasma against the geomagnetic field lines thus generating electric fields and currents just like a dynamo coil moving against magnetic field lines.

Solar Wind Parameters for Magnetospheric Magnetic Field Modeling Z. Qin 1, R. Denton 1, N. Tsyganenko 2, S. Wolf 3 Abstract. Magnetospheric magnetic fleld models are crucial for many space weather applications. However, the latest empirical models require solar wind and IMF data, which are not always available.

Data gaps are especially. Mathematical Aspects of Natural Dynamos (The Fluid Mechanics of Astrophysics and Geophysics Book 13) - Kindle edition by Dormy, Emmanuel, Soward, Andrew M.

Download it once and read it on your Kindle device, PC, phones or tablets. Use features like bookmarks, note taking and highlighting while reading Mathematical Aspects of Natural Dynamos (The Fluid Mechanics of Astrophysics and Manufacturer: Chapman and Hall/CRC.

showcases the RAM‐SCB capability as an inner magnetosphere module coupled with a global MHD model. Citation: Zaharia, S., V. Jordanova, D. Welling, and G. Tóth (), Self‐consistent inner magnetosphere simulation drivenCited by: Geodynamo, Solar Wind, and Magnetopause to Billion Years Ago John A.

Tarduno,1,2*Rory D. Cottrell,1 Michael K. Watkeys, 3Axel Hofmann, vine, 1,4 Eric E. Mamajek, 2Dunji Liu,5 David G. Sibeck,6 Levi P. Neukirch, Yoichi Usui1,7 Stellar wind standoff by a planetary magnetic field prevents atmospheric erosion and water Size: KB.

List of Responses to Request for Information. Listed in Table I.1 are the responses received by the Committee on a Decadal Strategy for Solar and Space Physics (Heliophysics) in response to its request for information (RFI) sent in September to the solar and space physics community (see Appendix H).The full-text versions of the RFI responses are included in the compact disk that.

Modeling magnetospheric current response to solar wind dynamic pressure enhancements during magnetic storms: 1. Methodology and results of the 25 September peak main phase case Yong Shi, 1 Eftyhia Zesta,1 and Larry R.

Lyons1 Received 21 February ; revised 22 May ; accepted 16 July ; published 31 October This leads into a thorough description of the Sun and the solar wind, and, finally, the author addresses magnetospheric physics.

Among the topics covered here are magnetospheric morphology, bow shocks, magnetospheric convection and electrical currents, substorms, ionospheric physics, magnetosphere-ionosphere coupling, auroral physics and the Cited by: Highlights This study presents the ionospheric effects of DDEF, PPEF and overshielding.

Dynamo electric field, DDEF and PPEF lead to the EIA intensification. The DDEF leads to increase in T e during storm recovery phase. DDEF leads to more pronounce additional layers over F2 peak at equatorial latitudes.

PPEF and overshielding occur in active and recovery phases of storm, by: