Diffusive ions in the foreshock region: review of GEOTAIL observations

Details Diffusive ions in the foreshock region: review of GEOTAIL observations Diffusive ions in the foreshock region: review of GEOTAIL observations

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh51b..07t&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH51B-07

Physics

2116 Energetic Particles, Planetary, 2154 Planetary Bow Shocks, 7807 Charged Particle Motion And Acceleration, 7851 Shock Waves

Scientific paper

GEOTAIL has been exposed to the upstream solar wind more than 50 % of time on its orbit, and providing a good database for the study of upstream ion populations. It has been shown, (1) that the spatial extent of the diffuse ions is more than 50-60 Re extending to the upstream region of Xgse ~ -60 Re, (2) that the energy spectrum of the diffuse ions is the hardest in the nose region of the bow shock, and softened toward the downwind direction, (3) that the diffuse ions appeared almost instantaneously after the IMF rotation made GEOTAIL connected to the quasi-parallel part of the bow shock while GEOTAIL was separated from the magnetosphere more than 20-30 Re in the cross-field direction, (4) and that the bow shock has a `Cosmic-Ray-Modified' shock nature: well ahead of the main shock ramp the upstream solar wind flow is decelerated by a few tens of km/s in the foreshock region where the diffuse ions have non-negligible pressures, which are proved to be balanced with the changes of the solar wind ram pressure. I will address the question of the origin of the diffuse ions based on the above observations. It is noted that (4), being the follow-up of the classical observations by IMP and ISEE, provides the clearest evidence that the diffuse ions are actively interacting with the incoming solar wind.

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