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Reconnection in Three Dimensions: The Role of Spines in Three Eruptive Flares View all abstracts by submitter

Angela Des Jardins   Submitted: 2008-11-26 10:42

In order to better understand magnetic reconnection and particle acceleration in solar flares, we compare the RHESSI hard X-ray (HXR) footpoint motions of three flares with a detailed study of the corresponding topology given by a Magnetic Charge Topology (MCT) model. We analyze the relationship between the footpoint motions and topological spine lines and find that the examined footpoint sources move along spine lines. We present a 3D topological model in which that movement can be understood. As reconnection proceeds, flux is transferred between the reconnecting domains, causing the separator to move. The movement of the separator?s chromospheric ends, identified with the HXR footpoints, is along those spine lines on which the separator ends.

Authors: Angela Des Jardins, Richard Canfield, Dana Longcope, Crystal Fordyce, and Scott Waitukaitis
Projects: RHESSI

Publication Status: In press
Last Modified: 2008-11-26 11:50
Go to main E-Print page  SUMER observations of the inverse Evershed effect in the transition region above a sunspot  Magnetic Changes in the course of the X7.1 Solar Flare on 2005 January 20  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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