Evidence of magnetic reconnection from Hα, soft X-ray and photospheric magnetic field observations

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A conventional view of magnetic reconnection is mainly based on the 2-D picture of an X-type neutral point, or on the extension of it to 3-D, and it is thought to be accompanied by flux transport across separatrices (places where the field-line mapping is discontinuous). This view is too restrictive...

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Detalles Bibliográficos
Autor principal: Mandrini, C.H
Otros Autores: Démoulin, Pascal, Bagalá, Liria Gabriela, Van Driel-Gesztelyi, L., Hénoux, J.C, Schmieder, B., Rovira, M.G
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 1997
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Mandrini, C.H. 
245 1 0 |a Evidence of magnetic reconnection from Hα, soft X-ray and photospheric magnetic field observations 
260 |c 1997 
270 1 0 |m Mandrini, C.H.; Inst. Astronomia y Fis. del Espacio, IAFE, CC.67, Suc.28, 1428 Buenos Aires, Argentina 
504 |a Alissandrakis, C.E., (1981) Astron. Astrophys., 100, p. 197 
504 |a Bagalá, L.G., Mandrini, C.H., Rovira, M.G., Démoulin, P., Hénoux, J.C., (1995) Solar Phys., 161, p. 103 
504 |a Baum, P., Bratenahl, A., (1980) Solar Phys., 67, p. 245 
504 |a Démoulin, P., Hénoux, J.C., Mandrini, C.H., (1992) Solar Phys., 139, p. 105 
504 |a Démoulin, P., Hénoux, J.C., Mandrini, C.H., (1994) Astron. Astrophys., 285, p. 1023 
504 |a Démoulin, P., Priest, E.R., Lonie, D.P., (1996) J. Geophys. Res., 101 (A4), p. 7631 
504 |a Démoulin, P., Van Driel-Gesztelyi, L., Schmieder, B., Hénoux, J.C., Csepura, G., Hagyard, M.J., (1993) Astron. Astrophys., 271, p. 292 
504 |a Démoulin, P., Mandrini, C.H., Rovira, M.G., Hénoux, J.C., Machado, M.E., (1994) Solar Phys., 150, p. 221 
504 |a Démoulin, P., Hénoux, J.C., Priest, E.R., Mandrini, C.H., (1996) Astron. Astrophys., 308, p. 643 
504 |a Démoulin, P., Bagalá, L.G., Mandrini, C.H., Hénoux, J.C., Rovira, M.G., (1996) Astron. Astrophys., , submitted 
504 |a Gary, G.A., Hagyard, M.J., (1990) Solar Phys., 126, p. 21 
504 |a Gorbachev, V.S., Somov, B.V., (1988) Solar Phys., 117, p. 77 
504 |a Gorbachev, V.S., Somov, B.V., (1989) Soviet Astron., 33 (1), p. 57 
504 |a Mandrini, C.H., Démoulin, P., Hénoux, J.C., Machado, M.E., (1991) Astron. Astrophys., 250, p. 541 
504 |a Mandrini, C.H., Rovira, M.G., Démoulin, P., Hénoux, J.C., Machado, M.E., Wilkinson, L.K., (1993) Astron. Astrophys., 272, p. 609 
504 |a Mandrini, C.H., Démoulin, P., Rovira, M.G., De La Beaujardière, J.F., Hénoux, J.C., (1995) Astron. Astrophys., 303, p. 927 
504 |a Mandrini, C.H., Démoulin, P., Van Driel-Gesztelyi, L., Schmieder, B., Cauzzi, G., Hofmann, A., (1996) Solar Phys., 168, p. 115 
504 |a Parnell, C.E., Priest, E.R., Golub, L., (1994) Solar Phys., 151, p. 57 
504 |a Priest, E.R., Démoulin, P., (1995) J. Geophys. Res., 100 (A12), p. 23443 
504 |a Van Driel-Gesztelyi, L., Hofmann, A., Démoulin, P., Schmieder, B., Csepura, G., (1994) Solar Phys., 149, p. 309 
504 |a Van Driel-Gesztelyi, L., Schmieder, B., Cauzzi, G., Mein, N., Hofmann, A., Nitta, N., Kurokawa, H., Staiger, J., (1996) Solar Phys., 163, p. 145 
506 |2 openaire  |e Política editorial 
520 3 |a A conventional view of magnetic reconnection is mainly based on the 2-D picture of an X-type neutral point, or on the extension of it to 3-D, and it is thought to be accompanied by flux transport across separatrices (places where the field-line mapping is discontinuous). This view is too restrictive when we realize the variety of configurations that are seen flaring. We designed an algorithm, called Source Method (SM), to determine the magnetic topology of active regions (ARs). The observed photospheric field was extrapolated to the corona using subphotospheric sources and the topology was defined by the link between these sources. Hα flare brightenings were found to be located at the intersection with the chromosphere of the separatrices so defined. These results and the knowledge we gained on the properties of magnetic field-line linkage, led us to generalize the concept of separatrices to 'quasi-separatrix layers' (QSLs) and to design a new method ('quasi-separatrix layers method', QSLM) to determine the magnetic topology of ARs. QSLs are regions where the magnetic field-line linkage changes drastically (discontinuously when they behave like separatrices) and the QSLM can be applied to ARs where the photospheric field has been extrapolated using any kind of technique. In this paper we apply the QSLM to observed flaring regions presenting very different configurations and also to a decaying AR where a minor phenomenon, like an X-ray bright point (XBP), is observed. We find that the locations of flare and XBP brightenings are related to the properties of the field-line linkage of the underlying magnetic region, as expected from recent developments of 3-D magnetic reconnection. The extrapolated coronal field lines representing the structures involved in the analyzed events have their photospheric footpoints located at both sides of QSLs. Our results strongly support the hypothesis that magnetic reconnection is at work in various coronal phenomena, ranging from the less energetic ones to large-scale eruptions.  |l eng 
593 |a Inst. Astronomia y Fis. del Espacio, IAFE, CC.67, Suc.28, 1428 Buenos Aires, Argentina 
593 |a Observatoire de Paris, Section de Meudon, URA 2080 (CNRS), F-92195 Meudon Cedex, France 
593 |a Konkoly Observatory, Pf. 67, Budapest, H-1525, Hungary 
700 1 |a Démoulin, Pascal 
700 1 |a Bagalá, Liria Gabriela 
700 1 |a Van Driel-Gesztelyi, L. 
700 1 |a Hénoux, J.C. 
700 1 |a Schmieder, B. 
700 1 |a Rovira, M.G. 
773 0 |d 1997  |g v. 174  |h pp. 229-240  |k n. 1-2  |p Sol. Phys.  |x 00380938  |w (AR-BaUEN)CENRE-2238  |t Solar Physics 
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856 4 0 |u https://hdl.handle.net/20.500.12110/paper_00380938_v174_n1-2_p229_Mandrini  |x handle  |y Handle 
856 4 0 |u https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00380938_v174_n1-2_p229_Mandrini  |x registro  |y Registro en la Biblioteca Digital 
961 |a paper_00380938_v174_n1-2_p229_Mandrini  |b paper  |c PE 
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963 |a VARI 

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