The Relative Atmospheric Impacts and Energy Inputs of Precipitating Solar and Magnetospheric Ion and Electron Populations during the 17-24 April 2002 Events

Details The Relative Atmospheric Impacts and Energy Inputs of Precipitating Solar and Magnetospheric Ion and Electron Populations during the 17-24 April 2002 Events The Relative Atmospheric Impacts and Energy Inputs of Precipitating Solar and Magnetospheric Ion and Electron Populations during the 17-24 April 2002 Events

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsa12a..07k&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SA12A-07

Physics

2455 Particle Precipitation, 2479 Solar Radiation And Cosmic Ray Effects, 2716 Energetic Particles, Precipitating, 2736 Magnetosphere/Ionosphere Interactions, 2788 Storms And Substorms

Scientific paper

A rich variety of solar and magnetospheric particles precipitated into the upper atmosphere during a series of 3 magnetic storms and a solar particle event that occurred in rapid succession linked to active region 9906. These populations include: large-scale periodic (every 2-3 hours) activations of the auroral oval precipitation, a significant auroral high energy tail, ring current precipitation, a series of solar protons and solar relativistic electron populations entering the expanded storm-time polar cap, and one of the larger solar energetic particle events of this solar cycle including enhanced >10 MeV/nucleon particles, near-relativistic electrons and high energy protons. The relatively soft energy spectrum of the solar proton event has interesting implications for the depth of penetration and ultimate impacts on the upper atmosphere. The combination of these solar and magnetospheric particles produced dramatic and long-lasting changes to the structure, chemistry and composition of the upper atmosphere. We focus on the relative energy input from each of these populations versus time and estimate their contributions to heating, ionization and the production of chemically-active minor species in the upper atmosphere. We use this information to identify solar drivers that produced particularly geoeffective particle inputs to the upper atmosphere both in terms of energy input and the altitude where they produce their maximum impacts.

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