Poynting Flux Response to Strong Solar Wind Pressure Enhancements

Details Poynting Flux Response to Strong Solar Wind Pressure Enhancements Poynting Flux Response to Strong Solar Wind Pressure Enhancements

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsa21b1549k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SA21B-1549

Statistics

Computation

0355 Thermosphere: Composition And Chemistry, 0368 Troposphere: Constituent Transport And Chemistry, 2721 Field-Aligned Currents And Current Systems (2409), 2788 Magnetic Storms And Substorms (7954)

Scientific paper

Strong solar wind dynamic pressure changes cause dramatic variations in the ionospheric transpolar potential and coupling efficiency between the solar wind and the terrestrial magnetosphere. Magnetospheric particle precipitation into the high latitude ionosphere also shows strong responses to solar wind pressure pulses. Neutral density data from low Earth orbiting satellites suggest that these pulses are a source of unmodeled error in satellite drag computations. Improved data processing for measurements from DMSP satellites allows us to investigate the Poynting flux response to strong solar wind pulses that precede some magnetic storms. Including these and other data in the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure provides perspective on the temporal and spatial variations of energy available to fuel thermospheric upheavals associated with enhanced satellite drag. We compare the Poynting flux and corresponding ionospheric and thermospheric perturbations from storms that were preceded by large solar wind dynamic pressure increases during May 15-17, 2005 and Aug 24-26, 2005 with those of a storm without such pre-conditioning.

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