Examination of geoeffective structures in the solar wind using ACE and WIND data from 1998-2000.

Details Examination of geoeffective structures in the solar wind using ACE and WIND data from 1998-2000. Examination of geoeffective structures in the solar wind using ACE and WIND data from 1998-2000.

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22c09b&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22C-09

Physics

7513 Coronal Mass Ejections

Scientific paper

Previous correlation studies of solar wind conditions with geomagnetic activity have shown that long periods (hours) of strong southward magnetic fields and high solar wind velocities combine to produce major geomagnetic storms. Magnetic field data from the Advanced Composition Explorer (ACE) and the WIND satellites confirm the presence of strong southward components of the interplanetary magnetic field during all periods of major activity, Ap > 50, between January 1998 and September 2000. An examination of solar wind data for seven severe geomagnetic storms in this period reveals that while the interplanetary signatures of a coronal mass ejection (CME) were present in every event, the location of the strong southward magnetic field varied. In 6 of the 7 severe storms, strong southward fields were present in the swept up wind immediately following the shock as well as in the interplanetary CME. In one of these events, the strong southward magnetic fields were present only in the wind immediately following the shock and not in CME itself. In addition to needing information about the magnetic topology of individual CMEs, improved 3-D models of the interactions of CMEs and shocks with the ambient solar wind coupled with more accurate information regarding the CME size, location and trajectory are required to produce reliable, long term forecasts of geomagnetic activity.

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