A topological approach to understand a multiple-loop solar flare

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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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Autor principal: Bagalá, Liria Gabriela
Otros Autores: Mandrini, C.H, Rovira, M.G, Démoulin, Pascal, Hénoux, J.C
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: Kluwer Academic Publishers 1995
Acceso en línea:Registro en Scopus
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100 1 |a Bagalá, Liria Gabriela 
245 1 2 |a A topological approach to understand a multiple-loop solar flare 
260 |b Kluwer Academic Publishers  |c 1995 
270 1 0 |m Bagalá, L.G.; Instituto de Astronomía y Física del Espacio, IAFE-CONICET, CC.67, Suc.28, Buenos Aires, 1428, Argentina 
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504 |a Mandrini, C.H., Machado, M.E., (1992) Solar Phys., 141, p. 147 
504 |a Mandrini, C.H., Démoulin, P., Hénoux, J.C., Machado, M.E., (1991) Astron. Astrophys., 250, p. 541 
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504 |a Rust, D.M., Simnett, G.M., Smith, D.F., Observational evidence for thermal wave fronts in solar flares (1985) The Astrophysical Journal, 288, p. 401 
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504 |a Schmieder, B., van Driel-Gesztelyi, L., Hénoux, J-C., Simnett, G.M., (1991) Astron. Astrophys., 244, p. 533 
504 |a Schmieder, B., Hagyard, M.J., Guoxiang, A., Hongqi, Z., Kalmán, B., Györi, L., (1994) Solar Phys., 150, p. 199 
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506 |2 openaire  |e Política editorial 
520 3 |a 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.  |l eng 
593 |a Instituto de Astronomía y Física del Espacio, IAFE-CONICET, CC.67, Suc.28, Buenos Aires, 1428, Argentina 
593 |a Observatoire de Paris, DASOP, URA 326 (CNRS), Meudon Cédex, 92195, France 
700 1 |a Mandrini, C.H. 
700 1 |a Rovira, M.G. 
700 1 |a Démoulin, Pascal 
700 1 |a Hénoux, J.C. 
773 0 |d Kluwer Academic Publishers, 1995  |g v. 161  |h pp. 103-121  |k n. 1  |p Sol Phys  |x 00380938  |w (AR-BaUEN)CENRE-2238  |t Solar Physics 
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