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4 edition of Modeling of the coupled magnetospheric and neutral wind dynamics found in the catalog.

Modeling of the coupled magnetospheric and neutral wind dynamics

Modeling of the coupled magnetospheric and neutral wind dynamics

annual technical status report 2

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  • 36 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


Edition Notes

Statementsubmitted by: Jeff P. Thayer.
Series[NASA contractor report] -- NASA CR-197861., NASA contractor report -- NASA CR-197861.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL17008592M
OCLC/WorldCa33069929

Solar Wind Parameters for Magnetospheric Magnetic Field Modeling Z. Qin 1, R. E. Denton 1, N. A. 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. We present a case study of the 25 December substorm which occurred between and Universal Time. During this interval, fast particle flows and field geometry consistent with magnetic reconnection were detected in the mid-tail region. An ejected plasmoid was observed by the lunar-orbiting Acceleration, Reconnection, Turbulence and Electrodynamics of Moon’s Interaction with Author: Miles Thomas Bengtson.

Neutral wind and plasma drift effects on low- and mid-latitude Total Electron Content. Journal of Geophysical Research, A4; Scherliess, L., Thompson, D.C, Schunk, R., (). Ionospheric dynamics and drivers obtained from a physics-based data assimilation model. Radio Science, 44, doi: / RS 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.

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   The ionosphere and thermosphere (IT) constitutes a coupled, complex and dynamical electromagnetic and photochemical system, which is sensitive to a combination of external factors: particle precipitation and electrical currents from the Earth's magnetosphere and incoming solar radiation produce dramatic effects in the IT and significantly alter its energetics, dynamics and chemistry in a Cited by: 2.


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Modeling of the coupled magnetospheric and neutral wind dynamics 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.

Modeling of the Coupled Magnetospheric and Neutral Wind Dynamos Submitted by: Jeff P. Thayer, Research Physicist dominance of the solar wind/magnetospheric dynamo as an electrical energy source to the ionosphere.

However, Thayer and Vickrey () have demonstrated that the available electrical simulate the neutral dynamics, composition. Get this from a library. Modeling of the coupled magnetospheric and neutral wind dynamics: annual technical status report 2.

[United States. National Aeronautics and Space Administration.;]. @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.

Russell C.T. () The Solar Wind and Magnetospheric Dynamics. In: Page D.E. (eds) Correlated Interplanetary and Magnetospheric Observations.

Astrophysics and Space Science Library (A Series of Books on the Recent Developments of Space Science and of General Geophysics and Astrophysics Published in Connection with the Journal Space Science Cited by: 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: the magnetospheric convection pattern as well, owing to the notion of the former being a footprint of the latter in an average sense.

During the first interval, we investigate the dynamics of the magnetosphere using the stand-alone LFM model and the CMIT model driven by the Wind solar wind observations, as well as the CISM model. 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.

At Saturn's orbital distance of ~ astronomical units (AU), the low solar wind dynamic pressure and weak interplanetary magnetic field (IMF) interact with the planet to create a magnetosphere that Cited by: 1.

Black box modeling of magnetospheric dynamics to forecast geomagnetic activity Article in Space Weather: The International Journal of Research and Applications 2(7) July with 16 Reads. Request PDF | Inner Magnetospheric Modeling with the Rice Convection Model | The Rice Convection Model (RCM) is an established physical model of the inner and middle magnetosphere that includes.

The analysis of correlated sets of solar wind and auroral index data suggest a more general framework for modeling the magnetospheric activity. It reveals in particular both the multiscale processes resembling classical critical phenomena in phase transition physics and regular components of dynamics, which resemble first order phase transitions.

is presented in Geocentric Solar Magnetospheric (GSM) co-ordinates. We model this event using a custom, high-resolution grid within the Space Weather Modeling Framework (SWMF)/Block Adaptive Tree Solar-wind Roe Upwind Scheme (BATS-R-US) model hosted by NASA’s Commu-nity Coordinated Modeling Center (CCMC) [T oth et al.,].

Using the University of Michigan's coupled magnetosphere-ionosphere-thermosphere general circulation model, which includes the neutral wind effect, Ridley et al.

() demonstrated that the pressure on the dayside magnetosphere is reduced while the pressure on the nightside is Author: Naomi Maruyama. The interactions and feedbacks that occur between energy deposition, dynamics, radiative cooling, energetic particles, electric fields, and plasma and neutral constituents and temperatures are how the global IT system regulates its response to magnetospheric forcing, and how it also regulates the response of the magnetosphere to solar wind.

7 National Research Council, Vision and Voyages for Planetary Science in the DecadeThe National Academies Press, Washington, D.C., Page Share Cite Suggested Citation: "9 Report of the Panel on Solar Wind-Magnetosphere Interactions.". cal understanding of system dynamics across all scales will ultimately require a two-dimensional station network of spacecraft encompassing the principal regions of interaction between the solar wind and ionospheric plasmas.

This is the function of the Magnetospheric Constellation mission, which, owing to the New Millennium ST–5 trailblazer. 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 physics of wind erosion, from particle entrainment to transport and deposition, is described with rigor from the viewpoints of fluid dynamics and soil physics.

The techniques for quantitative wind- erosion prediction through computational modelling constitutes a unique feature of this book in contrast to others published in the same by: Thermospheric wind data obtained from the Atmosphere Explorer E and Dynamics Explorer 2 satellites have been used to generate an empirical wind model for the upper thermosphere, analogous to the MSIS model for temperature and density, using a limited set of vector spherical harmonics.

D. G. Sibeck, The Magnetospheric and Ionospheric Response to Solar Wind Dynamic Pressure Variations, Modeling Magnetospheric Plasma Processes, (), ().

Wiley Online Library S. M. Petrinec, Nowcasting and Forecasting the Magnetopause and Bow Shock Locations Based on Empirical Models and Real‐Time Solar Wind Data, Space Weather, (showcases the RAM‐SCB capability as an inner magnetosphere module coupled with a global MHD model.

Citation: Zaharia, S., V. K. Jordanova, D. Welling, and G. Tóth (), Self‐consistent inner magnetosphere simulation drivenCited by: @article{osti_, title = {The zonal neutral wind in the equatorial thermosphere}, author = {Louro, A A and Duhau, S}, abstractNote = {A theoretical prediction of zonal neutral winds at the equator at F region heights is presented, using values for the ion velocity calculated with a model also due to the authors.

The results, and the dynamic properties of the thermosphere that may be.