A Method for Determining Coronal Reconnection Rates in Eruptive Events

Details A Method for Determining Coronal Reconnection Rates in Eruptive Events A Method for Determining Coronal Reconnection Rates in Eruptive Events

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000spd....31.0280f&link_type=abstract

American Astronomical Society, SPD Meeting #31, #02.80; Bulletin of the American Astronomical Society, Vol. 32, p.825

Astronomy and Astrophysics

Astronomy

Scientific paper

By measuring the rate at which the magnetic flux opened by a coronal mass ejection, or an eruptive flare, disappears, one can determine the global rate of reconnection in Webers per second (or Maxwells per second in CGS units) as a function of time. No specific model of the coronal magnetic field is needed using this approach. All that is required is the line-of-sight component of the field as obtained from a standard magnetogram and measurements of the surface area on the Sun corresponding to newly closed field lines. The latter can be determined by observing the motion of the chromospheric ribbons which lie at the feet of the X-ray loops formed in the aftermath of an eruptive event.

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