Interpretation of multiwavelength observations of November 5, 1980 solar flares by the magnetic topology of AR 2766
We present a detailed analysis of the magnetic topology of AR 2776 together with H α UV, X-rays, and radio observations of the November 5, 1980 flares in order to understand the role of the active region large-scale topology on the flare process. As at present the coronal magnetic field is modeled b...
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| Otros Autores: | , , , |
| Formato: | Capítulo de libro |
| Lenguaje: | Inglés |
| Publicado: |
Kluwer Academic Publishers
1994
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| Acceso en línea: | Registro en Scopus DOI Handle Registro en la Biblioteca Digital |
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| LEADER | 06887caa a22006137a 4500 | ||
|---|---|---|---|
| 001 | PAPER-19079 | ||
| 003 | AR-BaUEN | ||
| 005 | 20250306084458.0 | ||
| 008 | 190411s1994 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-51649141528 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Démoulin, Pascal | |
| 245 | 1 | 0 | |a Interpretation of multiwavelength observations of November 5, 1980 solar flares by the magnetic topology of AR 2766 |
| 260 | |b Kluwer Academic Publishers |c 1994 | ||
| 270 | 1 | 0 | |m Démoulin, P.; Observatoire de Paris, DASOP, URA326 (CNRS), Meudon Cédex, 92195, France |
| 504 | |a Déemoulin, P., Priest, E.R., (1992) Astron. Astrophys., 258, p. 535 | ||
| 504 | |a Démoulin, P., Hénoux, J.C., Mandrini, C.H., (1992) Solar Phys., 139, p. 105 | ||
| 504 | |a Démoulin, P., Hénoux, J. C., and Mandrini, C. H.: 1993, Astron. Astrophys., submitted; Démoulin, P., van Driel-Gesztelyi, L., Schmieder, B., Hénoux, J. C., Csepura, G., and Hagyard, M. J.: 1993, Astron. Astrophys., in press; Duijveman, A., Hoyng, P., Machado, M.E., (1982) Solar Phys., 81, p. 137 | ||
| 504 | |a Duijveman, A., Somov, B.V., Spektor, A.R., (1983) Solar Phys., 88, p. 257 | ||
| 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 Hesse, M., Schindler, K., A theoretical foundation of general magnetic reconnection (1988) Journal of Geophysical Research, 93 (6 A), p. 5559 | ||
| 504 | |a Hénoux, J.C., Somov, B.V., (1987) Astron. Astrophys., 185, p. 306 | ||
| 504 | |a Hénoux, J. C., Démoulin, P., Mandrini, C. H., and Rovira, M. G.: 1993, ‘Publications of the Astron; Hoyng, P., Marsh, K. A., Zirin, H., and Dennis, B.R.: 1983, Astrophysical Journal268865; Low, B.C., (1992) Astron. Astrophys., 253, p. 311 | ||
| 504 | |a Machado, M.E., Rovira, M.G., Sneibrun, C.V., (1985) Solar Phys., 99, p. 189 | ||
| 504 | |a Machado, M.E., Moore, R.L., Hernandez, A.M., Rovira, M.G., Hagyard, M.J., Smith, J.B., Jr., The observed characteristics of flare energy release. I - Magnetic structure at the energy release site (1988) The Astrophysical Journal, 326, p. 425 | ||
| 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 Martens, P.C.H., Van den Oord, G.H.J., Hoyng, P., (1985) Solar Phys., 96, p. 253 | ||
| 504 | |a Neidig, D., Smith, J.B., Jr., Hagyard, M.J., Machado, M.E., (1986) Adv. Space Res., 6 (6), p. 25 | ||
| 504 | |a Nordlung, A., Stein, R.F., Solar Photosphere: Structure, Convection and Magnetic Fields (1990) Proceedings of the IAU Colloq., 138, p. 191 | ||
| 504 | |a Priest, E.R., Forbes, T., Does fast magnetic reconnection exist? (1992) Journal of Geophysical Research, 97, p. 16757 | ||
| 504 | |a Somov, B.V., (1986) Astron. Astrophys., 163, p. 210 | ||
| 504 | |a Van Driel-Gesztelyi, L., Hofmann, A., Démoulin, P., Schmieder, B., Csepura, G., (1994) Solar Phys., 149, p. 309 | ||
| 504 | |a Vekstein, G.E., Priest, E.R., (1992) Astrophys. J., 384, p. 333 | ||
| 504 | |a Wilkinson, L.K., Elie, A.G., Gary, G.A., (1992) Astrophys. J., 392, p. L39 | ||
| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a We present a detailed analysis of the magnetic topology of AR 2776 together with H α UV, X-rays, and radio observations of the November 5, 1980 flares in order to understand the role of the active region large-scale topology on the flare process. As at present the coronal magnetic field is modeled by an ensemble of sub-photospheric sources whose positions and intensities are deduced from a least-square fit between the computed and observed longitudinal magnetic fields. Charges and dipole representations are shown to lead to similar modeling of the magnetic topology provided that the number of sources is great enough. However, for AR 2776, departure from a potential field has to be taken into account, therefore a linear force-free field extrapolation is used. The locations of the four bright off-band H α kernels in quadrupolar active regions have been studied previously. In this new study the active region is bipolar and shows a two-ribbon structure. We show that these two ribbons are a consequence of the bipolar photospheric field (the four kernels of quadrupolar regions merge into two bipolar regions). The two ribbons are found to be located at the intersection of the separatrices with the chromosphere when the shear, deduced from the fibril direction, is taken into account. This study supports the hypothesis that magnetic energy is stored in field-aligned currents and released by magnetic reconnection at the location of the separator, before being transported along field lines to the chromospheric level. It is also possible that part of the magnetic energy could be stored and released on the separatrices. Our study shows that meeting just one of two conditions- the presence of intense coronal currents or of a separator in a magnetic field configuration - is not sufficient for flaring. In order to release the stored energy, the coronal currents need either to be formed along the separatrices or to be transported towards the separator or separatrices. The location of the observed photospheric current concentrations on the computed separatrices supports this view. © 1994 Kluwer Academic Publishers. |l eng | |
| 593 | |a Observatoire de Paris, DASOP, URA326 (CNRS), Meudon Cédex, 92195, France | ||
| 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, URA326 (CNRS), Meudon Cédex, 92195, France | ||
| 593 | |a Department of Physics, The University of Alabama in Huntsville, 35899, AL, United States | ||
| 700 | 1 | |a Mandrini, C.H. | |
| 700 | 1 | |a Rovira, M.G. | |
| 700 | 1 | |a Hénoux, J.C. | |
| 700 | 1 | |a Machado, M.E. | |
| 773 | 0 | |d Kluwer Academic Publishers, 1994 |g v. 150 |h pp. 221-243 |k n. 1-2 |p Sol Phys |x 00380938 |w (AR-BaUEN)CENRE-2238 |t Solar Physics | |
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