The Evolution of Photospheric Source Regions of CMEs

Details The Evolution of Photospheric Source Regions of CMEs The Evolution of Photospheric Source Regions of CMEs

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.3808m&link_type=abstract

American Astronomical Society Meeting 204, #38.08; Bulletin of the American Astronomical Society, Vol. 36, p.713

Astronomy and Astrophysics

Astronomy

Scientific paper

In this presentation we determine the source regions of CMEs that were observed with SOHO/LASCO during times of solar activity maximum (Feb./Mar. 2000) and during the declining phase of the solar cycle (Nov./Dec. 2002). The CMEs were traced back onto the disk and EIT EUV images were used for identifying the sources. With the help of MDI synoptic and high cadence magnetograms we follow the evolution of the photospheric magnetic flux about 12 h before and after the event. We find that 80% of the identified CMEs (29 out of a total of 36 events) show small--scale flux changes before the event, usually flux emergence or flux disappearance. In 20% of the cases we find no signature of photospheric flux changes.

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