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...
Guardado en:
| Publicado: |
1995
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| 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 |
| Aporte de: |
| Sumario: | 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. |
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