Statistical Study of the Reconnection Rate in Solar Flares

Details Statistical Study of the Reconnection Rate in Solar Flares Statistical Study of the Reconnection Rate in Solar Flares

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..171i&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Physics

1

Scientific paper

The soft X-ray telescope (SXT) aboard Yohkoh has established that the driving mechanism of solar flares is magnetic reconnection. However, the physics of reconnection has not been clarified. One of the current puzzles is: what determines the reconnection rateNULL The reconnection rate is defined as reconnected magnetic flux per unit time or equivalently the ratio of inflow speed into reconnection point to Alfven velocity in non-dimension, and is one of the most important physical quantities in reconnection physics. However, observations have not yet succeeded to statistically determine the reconnection rate because direct observation of reconnection inflow and coronal magnetic field is difficult. In this poster we present a method to determine the reconnection rate from observational data, which use the following relations: H = frac B2 4pi vinL2 vinB = vfootBfoot. Here H, L, vfoot and Bfoot are respectively the flare heating rate, size of the flare arcade, separation velocity of the two ribbon, and magnetic field strength of the foot points. Since these four quantities can be obtained from observational data, the relations above give the inflow velocity vin and coronal magnetic field B, and thus the reconnection rate can be determined. Appling this method to many flare observations, we will determine the reconnection rate in solar flares statistically. A preliminary result is presented.

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