Magnetic Reconnection and Mass Acceleration in Solar Eruptions

Details Magnetic Reconnection and Mass Acceleration in Solar Eruptions Magnetic Reconnection and Mass Acceleration in Solar Eruptions

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp23a..07q&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP23A-07

Other

7513 Coronal Mass Ejections, 7519 Flares, 7531 Prominence Eruptions, 7835 Magnetic Reconnection

Scientific paper

We study the relationship between magnetic reconnection and mass acceleration in solar eruptive events of different magnetic configurations. The preliminary results of the case studies confirm the temporal correlation and magnitude scaling between reconnection rate and acceleration. We find that such observationally determined reconnection-acceleration relationship is independent of magnetic configurations of source regions, such as weak bipolar magnetic fields or multi-polar active regions, and regardless of whether CMEs are accompanied by filament eruption or not, or whether reconnection may take place above or below the flux rope. Other properties of coronal magnetic reconnection, including the reconnection height and the total magnetic flux transferred by reconnection, are also studied in these events in view of the role of magnetic reconnection in solar eruptions.

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