Magnetic reconnection in solar eruptive events of varying magnetic configurations

Details Magnetic reconnection in solar eruptive events of varying magnetic configurations Magnetic reconnection in solar eruptive events of varying magnetic configurations

Feb 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jastp..69..129q&link_type=abstract

Journal of Atmospheric and Solar-Terrestrial Physics, Volume 69, Issue 1-2, p. 129-134.

Physics

Scientific paper

We study the relationship between magnetic reconnection and acceleration of filaments and coronal mass ejections (CMEs) in different magnetic configurations. They occur in either quiet-Sun or active regions of either bipolar or multi-polar magnetic fields, and are either or not accompanied by filament eruptions. The preliminary results of the case studies confirm the temporal correlation and magnitude scaling relationship between reconnection rate and acceleration in the early phase of eruptions. The results suggest no clear difference between events of different magnetic configurations. It is shown that the total reconnection flux, which is calculated to be 10Mx, is proportional to the average velocities of CMEs, suggesting the important role of magnetic reconnection in the early stage of solar eruptions.

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