Abstract
A model based on a self-similar magnetohydrodynamic (MHD) solution is presented which accounts for the dynamic behavior of the birth of an active region due to the emergence of magnetic flux. The constraints of this model are deduced from observations. Specifically, this self-similar MHD solution explains the observation that plasma flow ascends in one leg and descends in the other leg of an arch filament system (AFS). Furthermore, the solution accounts for the formation of a current sheet in which a slow reconnection may occur that may explain the appearance of bright plages in the neighborhood of an AFS.
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References
Bachmann, G.: 1978, Bull. Astron. Inst. Czech. 29, 180.
Bruzek, A.: 1967, Solar Phys. 2, 451.
Bruzek, A.: 1968, in K. O. Kiepenheuer (ed.), ‘Structure and Development of Solar Active Regions’, IAU Symp. 35, 293.
Bruzek, A.: 1969, Solar Phys. 8, 29.
Chou, D. and Fisher, G. H.: 1989, Astrophys. J. 341, 533.
Coppi, B. and Friedland, A. B.: 1971, Astrophys. J. 169, 379.
Forbes, T. G. and Priest, E. R.: 1984, Solar Phys. 94, 315.
Gopasyuk, S. I.: 1967, Izv. Krymsk. Astrofiz. Obs. 37, 29.
Gopasyuk, S. I.: 1969, Izv. Krymsk. Astrofiz. Obs. 40, 111.
Heyvaerts, J., Priest, E. N., and Rust, D. M.: 1977, Astrophys. J. 216, 123.
Howard, R.: 1971, Solar Phys. 16, 21.
Kawaguchi, I. and Kitai, R.: 1976, Solar Phys. 46, 125.
Low, B. C.: 1982, Astrophys. J. 254, 796.
Meyer, F. et al.: 1979, Astron. Astrophys. 76, 35.
Nakagawa, Y., Steinolfson, R. S., and Wu, S. T.: 1976, Solar Phys. 47, 193.
Petschek, H. E.: 1967, Proc. AAS-NASA Symp. ‘On the Physics of Solar Flares’, NASA SP-50, p. 425.
Parker, E. N.: 1963, Astrophys. J. Suppl. Ser. 8, 177.
Shibata, K., Tajima, T., Steinolfson, R. S., and Matsumoto, R.: 1989, Astrophys. J. 354, 584.
Song, M. T. and Wu, S. T.: 1992, Proc. of Magnetic Field and Velocity Field Conference held on June 1992, Wutai-Mountain.
Song, M. T., Wu, S. T., and Dryer, M.: 1993, in AIAA Paper No. 93-3177, 24th Plasmadynamics and Laser Conference, July 6–9, 1993, Orlando, Florida.
Sonnerup, B. U. O.: 1970, J. Plasma Phys. 4, 161.
Sonnerup, B. U. O.: 1970, High Energy Phenomena on the Sun, p. 357.
Van Dyke, Milton: 1975, Perturbation Methods in Fluid Mechanics, The Parabolic Press, Stanford, California.
Zhang, H. Q. and Song, M. T.: 1992, Solar Phys. 138, 69.
Zirin, H.: 1974, in R. G. Athay (ed.), ‘Chromospheric Fine Structure’, IAU Symp. 56, 161.
Zirin, H.: 1987, Solar Phys. 114, 239.
Zwaan, C.: 1985, Solar Phys. 100, 397.
Zwaan, C.: 1987, Ann. Rev. Astron. Astrophys. 25, 83.
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Song, M.T., Wu, S.T. & Zhang, H.Q. Self-similar magnetohydrodynamic solution for the dynamics of magnetic flux emergence. Sol Phys 167, 57–77 (1996). https://doi.org/10.1007/BF00146328
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DOI: https://doi.org/10.1007/BF00146328