Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh52b..06s&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH52B-06
Physics
2116 Energetic Particles, Planetary, 2154 Planetary Bow Shocks
Scientific paper
Kinetic processes within the foreshock greatly perturb solar wind plasma and magnetic field parameters shortly prior to their interaction with the bow shock and magnetopause. Although few in number, Fermi accelerated ions exert pressures comparable to those of the ambient interplanetary magnetic field (IMF) and solar wind thermal plasma. The ions excavate cavities of depressed magnetic field strength and density on bundles of magnetic field lines connected to the bow shock. We use observations from Wind?s perigee passes to quantify the magnitude of these perturbations as functions of radial distance, local time, and ion flux levels outside the Earth?s bow shock. The perturbations first become noticeable some 60 RE upstream from Earth, while their effects are pronounced (factor of 2-3 variations) immediately outside the bow shock. As ion fluxes are bounded, the resulting density and magnetic field strength perturbations are most pronounced during intervals of low solar wind density and magnetic field strength, corresponding to high solar wind velocities. The foreshock cavities are an important (perhaps the most important) source of transient events in the outer dayside magnetosphere and high-latitude ionosphere.
Lepping Ronald P.
Phan Tai-Duc
Sibeck David G.
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