Magnetic Reconnection Models of Flares

  • T. G. Forbes
Part of the Astrophysics and Space Science Library book series (ASSL, volume 143)


The most feasible energy source for solar and stellar flares is the energy stored in coronal magnetic fields. To convert a significant fraction of this energy into heat and kinetic energy in a short time requires rapid change in the topology of the magnetic fields, and hence, rapid reconnection of field lines. Recent numerical and analytical models of solar flares suggest that the magnetic energy released by reconnection drives chromospheric ablation in the flare ribbons. Simple theoretical arguments based on compressible reconnection theory predict that the temperature of the ablated plasma should be about 1.03 × 106 B0.62 oK where B is the coronal magnetic field strength in Gauss.


Field Line Current Sheet Solar Flare Magnetic Reconnection Coronal Magnetic Field 
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  1. Dungey, J.W. 1953, Phil. Mag., 44, 725.Google Scholar
  2. Forbes, T.G. 1986, Astrophys. J., 305, 553.ADSCrossRefGoogle Scholar
  3. Forbes, T.G. and Malherbe, J.M. 1986a, Astrophys. J. (Lett.), 302, L67.ADSCrossRefGoogle Scholar
  4. Forbes, T.G. and Malherbe, J.M. 1986b, in The Lower Atmosphere of Solar Flares, ed. D.F. Neidig, NSO, Sacramento Peak, NM, p. 443.Google Scholar
  5. Forbes, T.G. and Priest, E.R. 1983, Solar Phys., 88, 211.ADSCrossRefGoogle Scholar
  6. Forbes, T.G. and Priest, E.R. 1984, Solar Phys., 94, 315.ADSCrossRefGoogle Scholar
  7. Furth, H.P., Killeen, J., and Rosenbluth, M.N. 1963, Phys. Fluids, 6, 459.ADSCrossRefGoogle Scholar
  8. Jakimiec, J., Sylwester, B., Sylwester, J., Lemen, J.R., Mewe, R., Bentley, R.D., Peres, G., Serio, S. and Schrijver, J. 1987, in Solar Maximum Analysis, eds. V.E. Stepanov and V.N. Obridko, VNU Science, Utrecht, The Netherlands, p. 91.Google Scholar
  9. Kopp, R.A. and Pneuman, G.W. 1976, Solar Phys., 99, 263.Google Scholar
  10. Lee, M.A. 1982, J., Geophys. Res., 87, 5063.ADSCrossRefGoogle Scholar
  11. Lin, H.-A., Lin, R.P., and Kane, S.R. 1985, Solar Phys., 50, 85.Google Scholar
  12. Malherbe, J.M., Forbes T.G., and Priest, E.R. 1984, in The Hydromagnetic of the Sun, ESA SP-220, p. 119.ADSGoogle Scholar
  13. Martin, S.F., Livi, S.H.B., and Wang, J. 1985, Australian J. Phys., 30, 929.ADSGoogle Scholar
  14. McCabe, M. 1973, Solar Phys., 30, 439.ADSCrossRefGoogle Scholar
  15. Parker, E.N. 1963, Astrophys. J., Suppl.Ser., 8, 177.ADSCrossRefGoogle Scholar
  16. Petschek, H.E. 1964, in AAS-NASA Symposium on the Physics of Solar Flares, ed. W.N. Hess, NASA SP-50, p. 425.Google Scholar
  17. Podgorny, A.I. and Syrovatsky, S.I. 1981, Sov. J. Plasma Phys., 7, 580.Google Scholar
  18. Priest, E.R. and Forbes, T.G. 1986, J. Geophys. Res., 91, 5579.ADSCrossRefGoogle Scholar
  19. Schindler, K. 1984, in Magnetic Reconnection in Space and Laboratory Plasmas, ed. E.W. Hones, Jr., Monograph 30, AGU Washington, DC, p.9.CrossRefGoogle Scholar
  20. Schmieder, B., Forbes, T.G., and Malherbe, J.M. 1987, Astrophys. J., 317, 956.ADSCrossRefGoogle Scholar
  21. Scholer, M. 1987, ‘Earthward plasma flow during near-Earth magnetotail reconnection: numerical simulations’, J. Geophys. Res., submitted.Google Scholar
  22. Sonnerup, B.U.Ö. 1970, J. Plasma Phys., 4, 161.ADSCrossRefGoogle Scholar
  23. Soward, A.M. and Priest, E.R. 1982, J. Plasma Phys., 28, 335.ADSCrossRefGoogle Scholar
  24. Sturrock, P. 1966, Nature, 211, 695.ADSCrossRefGoogle Scholar
  25. Svestka, Z. 1976, Solar Flares, Reidel, Dordrecht, The Netherlands, p. 310.Google Scholar
  26. Sweet, P.A. 1958, in Electromagnetic Phenomenon in Cosmical Physics, ed. B. Lehnert, Cambridge Univ., London, p. 123.Google Scholar
  27. Tandberg-Hanssen, E. 1974, Solar Prominences, Reidel, Dordrecht, The Netherlands, p. 78.Google Scholar
  28. Ugai, M. 1987, Geophys. Res. Lett., 14, 103.ADSCrossRefGoogle Scholar
  29. Van Hoven, G. 1981, in Solar Flare Magnetohydrodynamics, ed. E.R. Priest, Gordon and Breach, London, p. 217.Google Scholar
  30. Vasyliunas, V.M. 1975, Rev. Geophys. and Space Phys., 13, 303.ADSCrossRefGoogle Scholar
  31. Withbroe, G.L. 1978, Astrophys. J., 225, 641.ADSCrossRefGoogle Scholar
  32. Xu, A-.A. 1987, in Solar Maximum Analysis, eds. V.E. Stepanov and V.N. Obridko, VNU Science, Utrecht, The Netherlands, p. 147.Google Scholar
  33. Zirin, H. 1986, in The Lower Atmosphere of Solar Flares, ed. D.F. Neidig, NSO, Sacramento Peak, NM, p. 78.Google Scholar

Copyright information

© Kluwer Academic Publishers 1988

Authors and Affiliations

  • T. G. Forbes
    • 1
  1. 1.Institute for the Study of Earth, Oceans and SpaceUniversity of New HampshireDurhamUSA

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