Ultra-violet footpoints as tracers of coronal magnetic connectivity and restructuring during a solar flare

Fletcher, L. (2009) Ultra-violet footpoints as tracers of coronal magnetic connectivity and restructuring during a solar flare. Astronomy and Astrophysics, 493(1), pp. 241-250. (doi:10.1051/0004-6361:20077972)

Fletcher, L. (2009) Ultra-violet footpoints as tracers of coronal magnetic connectivity and restructuring during a solar flare. Astronomy and Astrophysics, 493(1), pp. 241-250. (doi:10.1051/0004-6361:20077972)

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Publisher's URL: http://dx.doi.org/10.1051/0004-6361:20077972

Abstract

<p><b>Context:</b> The bright, compact ultraviolet sources that appear in flare ribbons are interpreted as sites of energisation of the chromosphere, most likely by electron beams from the corona. Previously we have developed an algorithm to track these compact sources in observations by the Transition Region and Coronal Explorer (TRACE), recording position and intensity. We now exploit this further.</p> <p><b>Aims:</b> We aim at identifying conjugate footpoint pairs by cross-correlating the TRACE 1600 Å lightcurves in one particular event – the 2002-July-17 M 8.5 flare. We also seek the spatial relationship between the magnetic flux transfer (reconnection) rate, well-connected locations, and energy input by electrons.</p> <p><b>Methods:</b> We performed wavelet à trous filtering on the UV light curves, followed by a linear cross-correlation, to identify well-correlated pairs. We used RHESSI data to determine the locations of strong electron beam input.</p> <p><b>Results:</b> Maps of footpoint pairs were produced in which we can identify well-separated locations that have well-correlated 1600 Å light curves. The time lag between credible conjugate footpoint brightenings can be a few seconds. The flare magnetic connectivity is found to evolve with time. RHESSI hard X-ray sources are found where the flux transfer rate is highest.</p> <p><b>Conclusions:</b> We propose that the correlated footpoints are in fact conjugate pairs that are magnetically linked. In some instances, this linkage may be via a coronal null. The time lag in many cases is consistent with excitation by relativistic particles, but correlations with a longer time lag may suggest excitation by waves.</p>

Item Type:Articles
Status:Published
Refereed:Yes
Glasgow Author(s) Enlighten ID:Fletcher, Professor Lyndsay
Authors: Fletcher, L.
College/School:College of Science and Engineering > School of Physics and Astronomy
Journal Name:Astronomy and Astrophysics
Publisher:EDP Sciences
ISSN:0004-6361
ISSN (Online):1432-0746
Copyright Holders:Copyright © 2009 EDP Sciences
First Published:First published in Astronomy and Astrophysics 493(1):241-250
Publisher Policy:Reproduced in accordance with the copyright policy of the publisher

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Project CodeAward NoProject NamePrincipal InvestigatorFunder's NameFunder RefLead Dept
465931Solar, stellar and cosmological plasmas: a synthesis of data, modelling and theory.Declan DiverScience & Technologies Facilities Council (STFC)ST/F002149/1Physics and Astronomy