Inner magnetosphere plasma characteristics in response to interplanetary shock impacts

Details Inner magnetosphere plasma characteristics in response to interplanetary shock impacts Inner magnetosphere plasma characteristics in response to interplanetary shock impacts

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011jgra..11611206y&link_type=abstract

Journal of Geophysical Research, Volume 116, Issue A11, CiteID A11206

Physics

1

Interplanetary Physics: Interplanetary Shocks, Magnetospheric Physics: Magnetosphere: Inner, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions

Scientific paper

In order to characterize plasma (0.03-45 keV) properties in response to interplanetary (IP) shock impact at the geosynchronous orbit, we have examined 95 shock events from 1997 to 2004. These shock events have been categorized into two groups: shock fronts associated with southward interplanetary magnetic field (IMF; 47 cases) and with northward IMF (48 cases). Our results show that under southward IMF, the plasma becomes denser and hotter following the IP shock arrival. The proton (0.1-45 keV) and electron (0.03-45 keV) number densities have peaks of 1.8 and of 2.5 cm-3 at the duskside, respectively (the typical tail plasma sheet density is about 0.7 cm-3). After the IP shock impact, the plasma (proton and electron) temperature anisotropy increases remarkably at the noon sector, decreases toward dawn and dusk, and minimizes at midnight, suggesting that both electromagnetic ion cyclotron and whistler waves can be stimulated mainly at the dayside magnetosphere. In addition, there are more oxygen ions injecting into the inner magnetosphere, and the density of ionospheric oxygen ions is comparable to proton density. However, for IP shocks associated with northward IMF, the plasma density and temperature increases are insignificant, while slight enhancements of the plasma temperature anisotropy are distributed globally.

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