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Magnetic reconnection: from ``open'' EUV loops to closed post-flare ones observed by SDO View all abstracts by submitter

Jun Zhang   Submitted: 2013-11-07 00:39

Employing the emph{Solar Dynamics Observatory} observations, we select three well observed events including two flares and one extreme-ultraviolet (EUV) brightening. During the three events, the EUV loops evidently changed. One event was related to a major solar flare which took place on 2012 July 12 in active region NOAA AR 11520. ``Open'' EUV loops rooted in a facula of the AR deflected to the post-flare loops and then merged with them while the flare ribbon approached the facula. Meanwhile, ``open'' EUV loops rooted in a pore disappeared from top to bottom as the flare ribbon swept the pore. From the low temperature channels (e.g., 171 {AA}) to the high temperature channels (e.g., 94 {AA}), the loop evolution was similar. The coronal magnetic fields extrapolated from the photospheric vector magnetograms also show that the fields apparently ``open'' prior to the flare become closed after it. The other two events were associated with a B1.1 flare on 2010 May 24 and an EUV brightening on 2013 January 03, respectively. During both of these two events, some ``open'' loops either disappeared or darkened before the formation of new closed loops. We suggest that the observations reproduce the image predicted by the standard magnetic reconnection model: ``open'' magnetic fields become closed due to reconnection, manifesting as a transformation from ``open'' EUV loops to closed post-flare ones.

Authors: Jun Zhang, Shuhong Yang, Ting Li, Yuzong Zhang, Leping Li and Chaowei Jiang
Projects: SDO-AIA

Publication Status: 2013, ApJ, 776, 57
Last Modified: 2013-11-07 10:19
Go to main E-Print page  Twist Accumulation and Topology Structure of a Solar Magnetic Flux Rope  Dynamics of coronal rain and descending plasma blobs in solar prominences: I. Fully ionised case  Edit Entry  Download Preprint  Delete Entry 

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