OpenGGCM Modeling of Proton Aurora Near Substorm Onset

Details OpenGGCM Modeling of Proton Aurora Near Substorm Onset OpenGGCM Modeling of Proton Aurora Near Substorm Onset

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsm54b..03g&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SM54B-03

Physics

[2455] Ionosphere / Particle Precipitation, [2790] Magnetospheric Physics / Substorms

Scientific paper

Proton Aurora is primarily caused by pitch angle scattering of particles gyrating about highly stretched field lines. Because only highly stretched fields efficiently scatter particles into the loss cone, the equatorward boundary of the proton aurora is often assumed to mark the transition from dipolar to tail-like field lines. We use the Open Geospace General Circulation Model (OpenGGCM) to compare the onset time and location of proton aurora with discrete electron aurora and magnetic reconnection in the near earth magnetotail for substorms that occurred on February 27, 2001, March 23, 2007 and February 27, 2009. During the events, we see the peak of the proton precipitation split. After splitting one peak travels eastward and the other westward. We compare these modeling results with IMAGE observations where these are available.

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