Magnetic effects in Venus/solar wind interaction

Author:: Steinolfson, Richard S.
Published:: Jul 31, 1993.
Physical Description:: 1 electronic document

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Summary:

The overall objective of this research program is to better understand the interaction of a magnetized solar wind with the Venus atmosphere through the use of numerical solutions of the time-dependent, 2-D and 3-D magnetohydrodynamic (MHD) equations. Due to the more modest CPU requirements for the 2-D simulations, they were used for studies in which useful information not dependent on the third dimension could be obtained. The 2-D simulations served several purposes in addition to providing useful physical insight. They were used to determine the numerical parameters required in the 3-D studies, such as the grid spacing required to resolve particular features, and the damping that must be included to remove high-frequency oscillations. Among the specific studies performed with support from this grant that are discussed in this report are the following: comparison with other available models for purposes of testing the code and obtaining a baseline with which to evaluate the effects of additional physical processes, effects of a finite planet conductivity, bow shock standoff distance, and formation of the magnetic barrier and slippage of the magnetic field around the planet. A brief description of the methodology is presented before discussing the results.

Other Subject(s):

SOLAR PHYSICS

Collection:

NASA Technical Reports Server (NTRS) Collection.

Note:

Document ID: 19940012808.
Accession ID: 94N17281.
NASA-CR-194666.
NAS 1.26:194666.

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