Radiation belt energy and pitch angle distributions resulting from shock-drift injections

Details Radiation belt energy and pitch angle distributions resulting from shock-drift injections Radiation belt energy and pitch angle distributions resulting from shock-drift injections

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm41c..05k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM41C-05

Physics

2720 Energetic Particles: Trapped, 2753 Numerical Modeling, 2774 Radiation Belts, 2788 Magnetic Storms And Substorms (7954)

Scientific paper

In comparison with the Earth's outer zone radiation belts, sudden large variations in inner zone energetic particle fluxes are rare, occurring only during very large geomagnetic storms, usually initiated by coronal mass ejection (CME) driven interplanetary shocks. The violent geomagnetic storms of Oct-Nov 2003 mark the beginning of strong activity characterizing the declining phase of solar cycle No. 23. During the 29 Oct 2003 storm, ultra-relativistic (>10 MeV) electrons were injected below L = 3 producing a stably trapped radiation belt population that persisted for months following this event. We present results from a numerical study of shock-induced transport and heating of electrons in the 1-7 MeV range resulting in a newly formed 10-20 MeV belt; where test-particle trajectories are followed in time-dependent fields from an MHD magnetospheric model simulation of the 29 Oct 2003 Storm Sudden Commencement (SSC), driven by solar wind parameters measured at ACE. Both outer zone and solar energetic electron (SEE) sources for the new belt are considered. Energy and pitch angle distributions resulting from these two different possible sources are compared.

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