High Energy Precipitation and Consequences During the April 2002 Storms

Details High Energy Precipitation and Consequences During the April 2002 Storms High Energy Precipitation and Consequences During the April 2002 Storms

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsm32b1158f&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SM32B-1158

Physics

2407 Auroral Ionosphere (2704), 2455 Particle Precipitation, 2704 Auroral Phenomena (2407), 2736 Magnetosphere/Ionosphere Interactions, 7843 Numerical Simulation Studies

Scientific paper

Hemispheric maps of high energy proton and electron precipitation were created to characterize more accurately the energy inputs to the ionosphere-atmosphere system by interpolating NOAA-POES observations over 3-hour intervals during the April 2002 geomagnetic storms. The 3-hour cadence needed to achieve the required coverage is assumed to provide useful information, because of the relatively longer growth and development time scales for the ring current and the slow variation in long-duration solar particle events. These two populations probably account for most of the precipitation in the energy range >30 keV covered by the maps. The maps reveal interesting changes in the precipitation pattern with solar wind conditions and also a more isotropic in local time input during the intervals of sawtooth oscillations. Ring current ion precipitation is thought to be mainly a result of ion scattering in stretched geomagnetic fields as their gyroradii and the scale length of the field curvature become comparable near the equatorial plane. During the sawtooth activity, GOES observed tail-like fields to extend into the geosynchronous orbit region from midnight to dayside local times. Numerical results of our 3D Monte Carlo model will be presented for representative locations in the global particle precipitation. The transverse particle beam spreading effect is considered to be the result of the charge exchange and electron stripping collisions with the Earth's atmosphere. Initial comparisons between our model calculations and data will be provided as well.

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