Development of a topological model for solar flares
The main theoretical studies of the process involved in solar flares have been made in the two-dimensional approximation. However, the preliminary studies made with three field components suggest that reconnection could take place in the separatrices, the separator (intersection of separatrices) bei...
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Kluwer Academic Publishers
1992
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| Acceso en línea: | Registro en Scopus DOI Handle Registro en la Biblioteca Digital |
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| LEADER | 07031caa a22006137a 4500 | ||
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| 001 | PAPER-19242 | ||
| 003 | AR-BaUEN | ||
| 005 | 20250306084517.0 | ||
| 008 | 190411s1992 xx ||||fo|||| 00| 0 eng|d | ||
| 024 | 7 | |2 scopus |a 2-s2.0-0003130986 | |
| 040 | |a Scopus |b spa |c AR-BaUEN |d AR-BaUEN | ||
| 100 | 1 | |a Démoulin, Pascal | |
| 245 | 1 | 0 | |a Development of a topological model for solar flares |
| 260 | |b Kluwer Academic Publishers |c 1992 | ||
| 270 | 1 | 0 | |m Démoulin, P.; Observatoire de Paris, DASOP, URA 326, Meudon Principal Cedex, 92195, France |
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| 504 | |a Démoulin, P. and Priest, E. R.: 1992a, Astron. Astrophys. (in press); Démoulin, P. and Priest, E. R.: 1992b, Solar Phys. (in press); Gaizauskas, V. and Harvey, K. L.: 1991, in B. Schmieder and E. R. Priest (eds.), Proceedings of the Chantilly Meeting on Solar Flares, Paris Observatory, p. 25; Gorbachev, V.S., Somov, B.V., (1988) Solar Phys., 117, p. 77 | ||
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| 504 | |a Heyvaerts, J. and Hagyard, M. J.: 1991, in B. Schmieder and E. R. Priest (eds.), Proceedings of the Chantilly Meeting on Solar Flares, Paris Observatory, p. 1; Heyvaerts, J., Priest, E.R., Rust, D.M., An emerging flux model for the solar flare phenomenon (1977) The Astrophysical Journal, 216, p. 123 | ||
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| 504 | |a Mandrini, C., Démoulin, P., Hénoux, J.C., Machado, M., (1991) Astron. Astrophys., 250, p. 541 | ||
| 504 | |a Martin, S. F.: 1990, in V. Ruždjak and E. Tandberg-Hanssen (eds.), ‘Conditions for the Formation of Prominences as Inferred from Optical Observations’, IAU Colloq.117, 1; Martres, M.J., Michard, R., Soru-Escaut, I., Tsap, T.T., (1968) Solar Phys., 5, p. 187 | ||
| 504 | |a Priest, E.R., (1981) Solar Flare Magneto-Hydrodynamics, , Gordon and Breach, New York | ||
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| 504 | |a Schmieder, B., Priest, E.R., (1991) Proceedings of the Chantilly Meeting on Solar Flares, , Paris Observatory, Paris | ||
| 504 | |a Schmieder, B., Van Driel-Gesztelyi, L., Hénoux, J.C., Simnett, G.M., (1991) Astron. Astrophys., 244, p. 533 | ||
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| 506 | |2 openaire |e Política editorial | ||
| 520 | 3 | |a The main theoretical studies of the process involved in solar flares have been made in the two-dimensional approximation. However, the preliminary studies made with three field components suggest that reconnection could take place in the separatrices, the separator (intersection of separatrices) being a privileged location for this process. As a consequence the sites of flare kernels must be located on the intersections of the separatrices with the photosphere. Therefore, in order to understand the role of interacting large-scale structures in solar flares, we have analysed the topology of three-dimensional potential and linear force-free fields. The magnetic field has been modelled by a distribution of charges or dipoles located below the photosphere. This modelling permits us to define the field connectivity by the charges or the dipoles at both ends of every field line. We found that the appearance of a separator above the photosphere is more likely when a parasitic bipole emerges outside the axis that joins the main polarities and when the field lines are characteristic of a field created by dipoles. The separatrices derived in the potential and force-free hypothesis have different shapes. However, in the strong field regions where flares usually occur, the separatrices of the potential and force-free field models become closer. This property makes possible the use of the potential field, as a first estimate, for computing the location in the photosphere of the separatrices and for comparing this location with the position of observed H α kernels. Displacements of the separatrices of a force-free field result from modifications of the free energy of the field. Then force-free fields have the further capability of predicting the kernel displacement. In all cases a configuration suitable for prominence support is found above the separator. © 1992 Kluwer Academic Publishers. |l eng | |
| 593 | |a Observatoire de Paris, DASOP, URA 326, Meudon Principal Cedex, 92195, France | ||
| 593 | |a Instituto de Astronomía y Física del Espacio, IAFE-CONICET, CC.67, Suc.28, Buenos Aires, 1428, Argentina | ||
| 700 | 1 | |a Hénoux, J.C. | |
| 700 | 1 | |a Mandrini, C.H. | |
| 773 | 0 | |d Kluwer Academic Publishers, 1992 |g v. 139 |h pp. 105-123 |k n. 1 |p Sol Phys |x 00380938 |w (AR-BaUEN)CENRE-2238 |t Solar Physics | |
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