Modeling of Venus, Mars, and Titan

Details Modeling of Venus, Mars, and Titan Modeling of Venus, Mars, and Titan

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ssrv..162..267k&link_type=abstract

Space Science Reviews, Volume 162, Issue 1-4, pp. 267-307

Computer Science

Numerical Modeling, Full Kinetic Model, Hybrid Model, Magnetohydrodynamic Model, Exosphere Model, Venus, Mars, Titan, Planetary Magnetospheres, Planetary Exospheres

Scientific paper

Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn's moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. Chamberlain and Monte Carlo models of the Martian exosphere are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects.

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