Solar wind interaction with Jupiter's magnetosphere

Details Solar wind interaction with Jupiter's magnetosphere Solar wind interaction with Jupiter's magnetosphere

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm23b1618d&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM23B-1618

Physics

[2724] Magnetospheric Physics / Magnetopause And Boundary Layers, [2740] Magnetospheric Physics / Magnetospheric Configuration And Dynamics, [2756] Magnetospheric Physics / Planetary Magnetospheres, [2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions

Scientific paper

We suggest that the solar wind interaction with Jupiter's magnetosphere is dominated by viscous processes at the magnetopause boundary rather than a coherent reconnection-driven Dungey cycle. In particular, we show that shear flow-driven instabilities (e.g. Kelvin-Helmholtz) on Jupiter's magnetopheric flank can account for observations of: 1) flux tubes substantially depleted of energetic particles in regions outside of the plasmasheet, 2) anti-sunward flow in the dawnside ionosphere, 3) an aurorally active polar cap, and 4) a long magnetotail extending ~4 AU downstream. A preliminary analysis of the Kelvin-Helmholtz instability (KHI) as a function of local time will be presented along with initial two-dimensional hybrid code simulations of KHI at Jupiter's magnetopause boundary.

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