Volume 441, Number 1, October I 2005
|Page(s)||353 - 360|
|Published online||13 September 2005|
Indirect calculation of the magnetic reconnection rate from flare loops
Centre for Astrophysics, University of Central Lancashire, Preston, PR2 2HE, UK e-mail: email@example.com
2 L-3 Communications Government Services Inc, NASA GSFC, Greenbelt, Maryland 20771, USA
Accepted: 23 June 2005
High time resolution Transition Region And Coronal Explorer (TRACE) 171 and 195 Å observations of the evolution of flare loops on 1999 March 18 have been investigated. Given the location of the magnetic loops on the northeast solar limb and the cadence of the TRACE observations (~50 s), an estimation of the footpoint velocity due to ongoing reconnection was undertaken. This was achieved by calculating the velocity at which successive loops brighten in the emission lines during the postflare phase. A typical footpoint velocity of 1.5 km s km s-1 is obtained and a reconnection rate of ~0.001-0.03 is determined using the method outlined in Isobe et al. (2002, ApJ, 566, 528). This value for the reconnection rate is consistent with the regime outlined by Petschek's model for magnetic reconnection.
Key words: Sun: UV radiation / Sun: magnetic fields / Sun: corona
© ESO, 2005
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