A topological approach to understand a multiple-loop solar flare

We analyze the UV and X-ray data obtained by the SMM satellite for the flare starting at 02:36 UT on November 12, 1980 in AR 2779. From a detailed revision of the O v emission, we find that the observations are compatible with energy being released in a zone above the magnetic inversion line of the...

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Publicado: 1995
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v161_n1_p103_Bagala
http://hdl.handle.net/20.500.12110/paper_00380938_v161_n1_p103_Bagala
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paper:paper_00380938_v161_n1_p103_Bagala2023-06-08T15:02:33Z A topological approach to understand a multiple-loop solar flare We analyze the UV and X-ray data obtained by the SMM satellite for the flare starting at 02:36 UT on November 12, 1980 in AR 2779. From a detailed revision of the O v emission, we find that the observations are compatible with energy being released in a zone above the magnetic inversion line of the AR intermediate bipole. This energy is then transported mainly by conduction towards the two distant kernels located in the AR main bipole. One of these kernels is first identified in this paper. Accelerated particles contribute to the energy transport only during the impulsive phase. We model the observed longitudinal magnetic field by means of a discrete number of subphotospheric magnetic poles, and derive the magnetic field overall topology. As in previous studies of chromospheric flares, the O v kernels are located along the intersection of the computed separatrices with the photosphere. Especially where the field-line linkage changes 'discontinuously', these kernels can be linked in pairs by lines that extend along separatrices. Our results agree with the hypothesis of magnetic energy released by magnetic reconnection occurring on separatrices. © 1995 Kluwer Academic Publishers. 1995 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v161_n1_p103_Bagala http://hdl.handle.net/20.500.12110/paper_00380938_v161_n1_p103_Bagala
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
description We analyze the UV and X-ray data obtained by the SMM satellite for the flare starting at 02:36 UT on November 12, 1980 in AR 2779. From a detailed revision of the O v emission, we find that the observations are compatible with energy being released in a zone above the magnetic inversion line of the AR intermediate bipole. This energy is then transported mainly by conduction towards the two distant kernels located in the AR main bipole. One of these kernels is first identified in this paper. Accelerated particles contribute to the energy transport only during the impulsive phase. We model the observed longitudinal magnetic field by means of a discrete number of subphotospheric magnetic poles, and derive the magnetic field overall topology. As in previous studies of chromospheric flares, the O v kernels are located along the intersection of the computed separatrices with the photosphere. Especially where the field-line linkage changes 'discontinuously', these kernels can be linked in pairs by lines that extend along separatrices. Our results agree with the hypothesis of magnetic energy released by magnetic reconnection occurring on separatrices. © 1995 Kluwer Academic Publishers.
title A topological approach to understand a multiple-loop solar flare
spellingShingle A topological approach to understand a multiple-loop solar flare
title_short A topological approach to understand a multiple-loop solar flare
title_full A topological approach to understand a multiple-loop solar flare
title_fullStr A topological approach to understand a multiple-loop solar flare
title_full_unstemmed A topological approach to understand a multiple-loop solar flare
title_sort topological approach to understand a multiple-loop solar flare
publishDate 1995
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v161_n1_p103_Bagala
http://hdl.handle.net/20.500.12110/paper_00380938_v161_n1_p103_Bagala
_version_ 1768543459355918336

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