Ion Outflow Response to the ICME on 29 October-03 November 2004 and the ICME on 07-13 November 2004

Details Ion Outflow Response to the ICME on 29 October-03 November 2004 and the ICME on 07-13 November 2004 Ion Outflow Response to the ICME on 29 October-03 November 2004 and the ICME on 07-13 November 2004

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsa13a..09e&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SA13A-09

Physics

2164 Solar Wind Plasma, 2776 Polar Cap Phenomena, 2784 Solar Wind/Magnetosphere Interactions, 2788 Storms And Substorms

Scientific paper

We examine the flux of ions outflowing from the polar ionosphere into the magnetosphere in response to two different Interplanetary Coronal Mass Ejections (ICMEs). We discuss differences in the solar wind conditions and then compare and contrast different outflow responses. We examine the outflowing thermal ions that flow away from the Earth along magnetic field lines. Previous simulation studies indicate that such outflowing ions can travel to the plasma sheet and ring current. Most of the field-aligned outward moving ions we observe during these storms appears to be O+. The flux of O+ outflowing ions has been shown to increase linearly with increasing solar wind pressure. However, much of the previous work was done over a limited range of solar wind dynamic pressures. We look at these ICMEs, which have large solar wind pressures, to determine if the outflow response is linear at higher pressures. We use ion measurements from the Thermal Ion Dynamics Experiment (TIDE) on the Polar spacecraft and solar wind measurements from the Solar Wind Electron Proton Alpha Monitor (SWEPAM) on the ACE spacecraft.

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