French, RJ; Matthews, SA; van Driel-Gesztelyi, L; Long, DM; Judge, PG; (2020) Dynamics of Late-stage Reconnection in the 2017 September 10 Solar Flare. The Astrophysical Journal , 900 (2) , Article 192. 10.3847/1538-4357/aba94b.

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Abstract

The American Astronomical Society, find out more The Institute of Physics, find out more Dynamics of Late-stage Reconnection in the 2017 September 10 Solar Flare Ryan J. French1, Sarah A. Matthews1, Lidia van Driel-Gesztelyi1,2,3, David M. Long1, and Philip G. Judge4 Published 2020 September 15 • © 2020. The American Astronomical Society. All rights reserved. The Astrophysical Journal, Volume 900, Number 2 74 Total downloads Turn on MathJax Get permission to re-use this article Share this article Share this content via email Share on Facebook Share on Twitter Share on Google+ Share on Mendeley Hide article information Author affiliations 1 Mullard Space Science Laboratory, University College London, Dorking RH5 6NT, UK 2 LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université Paris Diderot, 5 place Jules Janssen, F-92190 Meudon, France 3 Konkoly Observatory of the Hungarian Academy of Sciences, Budapest, Hungary 4 HAO, National Center for Atmospheric Research, P.O. Box 3000, Boulder, CO 80307-3000, USA ORCID iDs Ryan J. French https://orcid.org/0000-0001-9726-0738 Sarah A. Matthews https://orcid.org/0000-0001-9346-8179 Lidia van Driel-Gesztelyi https://orcid.org/0000-0002-2943-5978 David M. Long https://orcid.org/0000-0003-3137-0277 Philip G. Judge https://orcid.org/0000-0001-5174-0568 Dates Received 2020 June 24 Accepted 2020 July 24 Published 2020 September 15 Check for updates using Crossmark Citation Ryan J. French et al 2020 ApJ 900 192 Create citation alert DOI https://doi.org/10.3847/1538-4357/aba94b Keywords Solar flares ; Solar flare spectra ; Solar magnetic reconnection ; Spectropolarimetry ; Spectroscopy Journal RSS feed Create or edit your corridor alerts What are corridors? This link opens in a new tab. Abstract In this multi-instrument paper, we search for evidence of sustained magnetic reconnection far beyond the impulsive phase of the X8.2-class solar flare on 2017 September 10. Using Hinode/EIS, CoMP, SDO/AIA, K-Cor, Hinode/XRT, RHESSI, and IRIS, we study the late-stage evolution of the flare dynamics and topology, comparing signatures of reconnection with those expected from the standard solar flare model. Examining previously unpublished EIS data, we present the evolution of nonthermal velocity and temperature within the famous plasma sheet structure, for the first four hours of the flare's duration. On even longer timescales, we use differential emission measures and polarization data to study the longevity of the flare's plasma sheet and cusp structure, discovering that the plasma sheet is still visible in observations of CoMP linear polarization on 2017 September 11, long after its last appearance in EUV. We deduce that magnetic reconnection of some form is still ongoing at this time—27 hr after flare onset.

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