Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm51a1337r&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SM51A-1337
Physics
[2784] Magnetospheric Physics / Solar Wind/Magnetosphere Interactions, [2794] Magnetospheric Physics / Instruments And Techniques, [7974] Space Weather / Solar Effects, [7984] Space Weather / Space Radiation Environment
Scientific paper
Solar energetic protons have direct and rapid access to geostationary orbit (L = 6.6) and often to lower L shells, thereby presenting a severe space weather hazard throughout the magnetosphere. Starting with GOES 13, the GOES system has a new operational capability of co-located and simultaneous westward and eastward observations of 0.7-900 MeV solar proton fluxes. Due to the ~1 Re gyroradii of MeV protons at geostationary orbit, the guiding centers of the fluxes observed looking westward (eastward) lie well outside (inside) geostationary orbit. During solar energetic particle (SEP) events, eastward geostationary observations of 0.7-82 MeV protons exhibit time-varying differences with respect to their westward equivalents due to this "east-west effect." At times of high solar wind dynamic pressure (>10 nPa) following the arrival of an interplanetary shock, the "inside" and "outside" fluxes are approximately equal. As the pressure decreases to ~1 nPa, the "inside" fluxes decrease as much as an order of magnitude with respect to the "outside" fluxes. Under such low pressure conditions, the "inside" fluxes exhibit short-lived (1-3 hr) increases, sometimes to the levels of the "outside" fluxes, during periods of enhanced auroral electrojet index activity.
Mazur J. E.
Onsager T. G.
Rodriguez Juan V.
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