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| P06: | Comparative Studies of Planetary Magnetospheres |
| Sponsor: |
Planetary Sciences
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| CoSponsor: |
SPA-Magnetospheric Physics |
| Convener: |
Eun-Hwa Kim Princeton Plasma Physics Laboratory, Princeton University Princeton Plasma Physics Laboratory Princeton University P.O. Box 451 Princeton, NJ, USA ehkim@pppl.gov Peter J. Chi Institute of Geophysics and Planetary Physics /UCLA Institute of Geophysics and Planetary Physics University of California, Los Angeles 6877 Slichter Hall 595 Charles Young Dr. E. Los Angeles, CA, USA pchi@igpp.ucla.edu Scott A. Boardsen NASA GSFC/GEST Heliophysics Science Divison, NASA Goddard Space Flight Center, Code 674.0 Greenbelt, MD, USA scott.a.boardsen@nasa.gov Peter Delamere Laboratory for Atmospheric and Space Physics, University of Colorado Laboratory for Atmospheric and Space Physics CB 392 Duane Physics D133 Boulder, CO, USA delamere@lasp.colorado.edu |
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2459 2700 2756 6200 .
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| Description: |
A number of solar system bodies have magnetospheres, and each presents a unique plasma environment around the body. The scaling relations can be tested over a much wider parameter range than that associated with the Earth alone. For example, the ratio between distances from the center of the planet to the subsolar point of magnetopause and the ion inertial length ranges from 85 for Mercury to 5800 for Jupiter. Comparison of Earth’s magnetosphere with other planets’ could provide more insights, such as the significance of kinetic effects, the dependence of the geometrical configuration of rotation axis, magnetic dipole, and solar wind flow direction. This session encompasses observations, theories and modeling of physical process in the magnetospheres of planets, moons, and comets. It also addresses, for any given body, the coupling processes between the magnetosphere and other regions (e.g., ionosphere, exosphere, and solar wind). This session welcomes all presentations on planetary magnetospheres, including: (a) comparative approaches to a phenomenon occurring in different planetary plasma environments; (b) modeling of planetary magnetospheres; (c) simulations and observations of waves, instabilities, and reconnection; and (d) energy transfer between magnetospheres and other regions (e.g., ionosphere and solar wind). New experimental techniques and spacecraft observations are also encouraged. |