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Modeling of Venus, Mars, and Titan |
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| Authors: | Esa Kallio Jean-Yves Chaufray Ronan Modolo Darci Snowden Robert Winglee |
| Institution: | 1. Finnish Meteorological Institute, Helsinki, Finland 2. Laboratoire de M??t??orologie Dynamique, Institut Pierre Simon Laplace, Centre National de la Recherche Scientifique, Paris, France 3. Universit?? de Versailles Saint-Quentin, 45 avenue des Etats-Unis, 78035, Versailles cedex, France 4. Laboratoire Atmosph??res, Milieux et Observations Spatiales, Quartier des Garennes, 11 bd d??Alembert, 78280, Guyancourt, France 5. Centre National de la Recherche Scientifique, Quartier des Garennes, 11 bd d??Alembert, 78280, Guyancourt, France 6. Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA 7. Department of Earth and Space Sciences, University of Washington, Johnson Hall, Box 351310, Seattle, WA, 98195-1310, USA |
| Abstract: | 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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