Magnetopause shadowing effects for radiation belt models during high-speed solar wind streams

Details Magnetopause shadowing effects for radiation belt models during high-speed solar wind streams Magnetopause shadowing effects for radiation belt models during high-speed solar wind streams

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm13a1787k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM13A-1787

Physics

[2720] Magnetospheric Physics / Energetic Particles: Trapped, [2730] Magnetospheric Physics / Magnetosphere: Inner

Scientific paper

Radiation belt models are driven, to a large degree, by boundary conditions: As the magnetosphere reacts to the dynamics of the solar wind, the trapping region of radiation belt particles changes with the magnetopause acting as a natural boundary defining a last closed drift shell (LCDS). Outside of the last closed drift shell, radiation belt processes cannot be described by the typical diffusive equations but could be numerically approximated with a strong loss term on the order of a drift period. We present a study comparing the loss of radiation belt fluxes at the outer boundary due to high-speed solar wind streams impinging on geospace. Our study includes the calculation of the LCDS for a variety of magnetic field models. These calculated LCDSs are applied to idealized numerical experiments driven by the mean solar wind conditions from a superposed-epoch study of radiation belt losses. The results are benchmarked and compared to data from the GPS constellation and LANL geosynchronous particle data. In addition, we find an empirical relation that can describe the LCDS as a second order polynomial of the geomagnetic index Dst. This empirical model can be easily implemented in radiation belt models by providing a numerical value for the outer boundary as a function of Dst.

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