Photospheric Magnetic field boundary conditions for CMEs: Two case studies

Details Photospheric Magnetic field boundary conditions for CMEs: Two case studies Photospheric Magnetic field boundary conditions for CMEs: Two case studies

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22a04l&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22A-04

Other

7509 Corona, 7511 Coronal Holes, 7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7529 Photosphere

Scientific paper

We select two distinctively different cases of isolated CMEs during the cycle 22-23 minimum for close scrutiny of the global photospheric magnetic field behaviour. The well known January 6, 1997 case occurred with only an apparent filament disruption in a decaying active region near the central meridian just south of the equator. There were few other active regions on the visible hemisphere at the time, except for two small bipolar features. However, from the previous solar rotation, it was clear that several strong active regions were on the invisible hemisphere at the time, but underwent large changes before reappearing over the limb. We investigate the possibility that their significant evolution on the farside produced coronal disturbances on the nearside. For this purpose we use various observed and constructed time-dependent synoptic maps to examine coronal field and coronal hole reactions to the possible changing global photospheric field. We also examine a contrasting case on 12 May 1997 when activity clearly occurred on the visible disk in a small but strong active region. As a whole, these studies may lead to better defined solar boundary conditions for CME modeling using numerical simulations.

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