Abstract
Simple models for the MHD eruption of a solar prominence are presented, in which the prominence is treated as a twisted magnetic flux tube that is being repelled from the solar surface by magnetic pressure forces. The effects of different physical assumptions to deal with this magneto-hydrodynamically complex phenomenon are evaluated, such as holding constant the prominence current, radius, flux or twist or modelling the prominence as a current sheet. Including a background magnetic field allows the prominence to be in equilibrium initially with an Inverse Polarity and then to erupt due to magnetic non-equilibrium when the background magnetic field is too small or the prominence twist is too great. The electric field at the neutral point below the prominence rapidly increases to a maximum value and then declines. Including the effect of gravity also allows an equilibrium with Normal Polarity to exist. Finally, an ideal MHD solution is found which incorporates self-consistently a current sheet below the prominence and which implies that a prominence will still erupt and form a current sheet even if no reconnection occurs. When reconnection is allowed it is, therefore, driven by the eruption.
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References
Amari, T. and Aly, J. J.: 1989, Astron. Astrophys. 208, 261.
Anzer, U.: 1989, in E. R. Priest (ed.), Dynamics and Structure of Quiescent Solar Prominences, Kluwer Academic Publishers, Dordrecht, The Netherlands, Ch. 6.
Biskamp, D. and Welter, H.: 1989, Solar Phys. 120, 49.
Browning, P. K. and Priest, E. R.: 1986, Solar Phys. 106, 335.
Demoulin, P. K. and Priest, E. R.: 1988, Astron. Astrophys. 206, 336.
Demoulin, P. K. and Priest, E. R.: 1990, to be submitted.
Forbes, T. G.: 1986, Astrophys. J. 305, 553.
Forbes, T. G.: 1990, to be submitted.
Forbes, T. G. and Priest, E. R.: 1983, Solar Phys. 88, 211.
Hood, A. W. and Priest, E. R.: 1980, Solar Phys. 66, 113.
Kaastra, J. S.: 1985, Ph.D. Thesis, Univ. Utrecht.
Kuin, N. and Martens, P.: 1986, in A. Poland (ed.), Coronal and Prominence Plasmas, NASA CP-2442, p. 241.
Kuperus, M. and Raadu, M. A.: 1974, Astron. Astrophys. 31, 189.
Martens, P.: 1986, in A. Poland (ed.), Coronal and Prominence Plasmas, NASA CP-2442, p. 431.
Mikic, Z., Barnes, D. C., and Schnack, D. D.: 1988, Astrophys. J. 328, 830.
Poletto, G. and Kopp, R. A.: 1986, in D. F. Neidig (ed.), The Lower Atmosphere of Solar Flares, NSO, Sacramento Peak, NM, p. 453.
Priest, E. R.: 1981, Solar Flare MHD, Gordon and Breach, London.
Priest, E. R.: 1982, Solar MHD, D. Reidel Publ. Co., Dordrecht, Holland.
Priest, E. R.: 1985, Rep. Prog. Phys. 48, 955.
Priest, E. R.: 1986, in P. Gondhalekar (ed.), Proc. RAL Workshop on Solar and Stellar Flares, p. 140.
Priest, E. R.: 1989, Dynamics and Structure of Quiescent Solar Prominences, Kluwer Academic Press, The Netherlands.
Robertson, J. A. and Priest, E. R.: 1987, Solar Phys. 114, 311.
Steele, C. D. and Priest, E. R.: 1989, Solar Phys. 119, 157.
Sturrock, P.: 1980, Solar Flares, Colo. Ass. Univ. Press.
Van Tend, W. and Kuperus, M.: 1978, Solar Phys. 59, 115.
Zwingmann, W.: 1985, Ph.D. Thesis, Bochum University.
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Priest, E.R., Forbes, T.G. Magnetic field evolution during prominence eruptions and two-ribbon flares. Sol Phys 126, 319–350 (1990). https://doi.org/10.1007/BF00153054
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DOI: https://doi.org/10.1007/BF00153054