Physics – Plasma Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm12a..07o&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM12A-07
Physics
Plasma Physics
[7835] Space Plasma Physics / Magnetic Reconnection, [7836] Space Plasma Physics / Mhd Waves And Instabilities, [7839] Space Plasma Physics / Nonlinear Phenomena, [7863] Space Plasma Physics / Turbulence
Scientific paper
For southward IMF, magnetic reconnection occurs in the dayside magnetopause and plasma sheet, and the process is most dominant in solar wind-magnetosphere interaction. However, magnetic reconnection is not sufficiently understood as transport process. For northward IMF, Kelvin-Helmholtz instability can be excited due to velocity shear at magnetopause and there are several observations reported periodic wavy phenomena which come from the instability. Moreover, local simulations clearly show the vortex formation from the instability. However, there is no global simulation to show occurrence of the instability for northward IMF condition. On the other hand, several global simulations show wavy phenomena and vortex formation during southward IMF. Thus it is needed to study relationship between magnetic reconnection and Kelvin-Helmholtz instability. Therefore, we have studied plasma instabilities and their nonlinear evolution in boundary layers of the earth's magnetosphere by using a high-resolution and 3-dimensional global MHD simulation of interaction between the solar wind and earth's magnetosphere. For southward IMF, filamentary and streamer structure is formed in the plasma sheet due to patchy and intermittent reconnection. Moreover, vortex train appears at the dayside magnetopause. On the other hand, Kelvin-Helmholtz instability is excited to generate wavy train or vortex train rolled up in the low latitude boundary layer for northward IMF. Relationship between the vortex train and high latitude reconnection is also discussed.
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