The geoeffective scale sizes of solar wind events

Details The geoeffective scale sizes of solar wind events The geoeffective scale sizes of solar wind events

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh31a0705j&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH31A-0705

Physics

2102 Corotating Streams, 2134 Interplanetary Magnetic Fields, 2139 Interplanetary Shocks, 2169 Sources Of The Solar Wind

Scientific paper

It was shown earlier that the correlations for both plasma and IMF (interplanetary magnetic field) parameters measured at two spacecraft degrade substantially with their separation. Especially, for IMF perpendicular (to the Sun-Earth line) separations of about 100 RE yielded poor correlations during geomagnetically quiet periods. In contrast, during the magnetic storms these correlations improve substantially, suggesting larger scale sizes for geoeffective events. We take the advantage of large perpendicular separations between Wind and Ace in 1999 and 2000 and examine the time integral of Bs (southward IMF) during geoeffective periods. We find that this parameter, representing the geoeffective scale size, is well preserved over distances much larger than 100 RE. We calculate the front normal directions for the shock fronts preceding magnetic storms. Front normals are then used to estimate relevant scale sizes for different shock drivers, particularly CMEs and Complex ejecta consisting of multiple CMEs. We also show that the shock front normal direction can be used as an useful tool to differentiate individual CMEs in Complex ejectas.

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