The flow of plasma in the solar terrestrial environment

Details The flow of plasma in the solar terrestrial environment The flow of plasma in the solar terrestrial environment

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990cass.rept.....s&link_type=abstract

Final Technical Report, 1 Jul. 1980 - 30 Sep. 1990 Utah State Univ., Logan. Center for Atmospheric and Space Sciences.

Physics

Geophysics

Magnetohydrodynamic Flow, Magnetohydrodynamics, Plasma Dynamics, Plasmas (Physics), Plasmasphere, Solar Terrestrial Interactions, Thermosphere, Three Dimensional Models, Convection, Feedback, Geophysics, Particle Precipitation, Simulation, Stability, Storms, Time Dependence, Time Lag

Scientific paper

The overall goal of our NASA Theory Program was to study the coupling, time delays, and feedback mechanisms between the various regions of the solar-terrestrial system in a self-consistent, quantitative manner. To accomplish this goal, it will eventually be necessary to have time-dependent macroscopic models of the different regions of the solar-terrestrial system and we are continually working toward this goal. However, with the funding from this NASA program, we concentrated on the near-earth plasma environment, including the ionosphere, the plasmasphere, and the polar wind. In this area, we developed unique global models that allowed us to study the coupling between the different regions. These results are highlighted in the next section. Another important aspect of our NASA Theory Program concerned the effect that localized 'structure' had on the macroscopic flow in the ionosphere, plasmasphere, thermosphere, and polar wind. The localized structure can be created by structured magnetospheric inputs (i.e., structured plasma convection, particle precipitation or Birkland current patterns) or time variations in these input due to storms and substorms. Also, some of the plasma flows that we predicted with our macroscopic models could be unstable, and another one of our goals was to examine the stability of our predicted flows. Because time-dependent, three-dimensional numerical models of the solar-terrestrial environment generally require extensive computer resources, they are usually based on relatively simple mathematical formulations (i.e., simple MHD or hydrodynamic formulations). Therefore, another goal of our NASA Theory Program was to study the conditions under which various mathematical formulations can be applied to specific solar-terrestrial regions. This could involve a detailed comparison of kinetic, semi-kinetic, and hydrodynamic predictions for a given polar wind scenario or it could involve the comparison of a small-scale particle-in-cell (PIC) simulation of a plasma expansion event with a similar macroscopic expansion event. The different mathematical formulations have different strengths and weaknesses and a careful comparison of model predictions for similar geophysical situations provides insight into when the various models can be used with confidence.

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