Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-26T03:27:36.512Z Has data issue: false hasContentIssue false
  • English
  • Français

Current Sheets in Solar Flares

Published online by Cambridge University Press:  04 August 2017

E. R. Priest
E. R. Priest*
Affiliation:
Applied Maths Dept., St. Andrews University Scotland

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Until recently magnetic reconnection in solar flares was discussed simplistically in terms of either a spontaneous tearing mode instability or a driven Petschek mode. Now the subtle relationship between these two extremes is much better understood. Current sheets may form and reconnection may be initiated in many different ways. There are also a variety of nonlinear pathways from a reconnection instability and several types of driven reconnection.

In solar flares current sheets may be important as new flux emerges from below the photosphere and also as a magnetic arcade closes down after being blown open by an eruptive instability. Numerical simulations of these sheets will be described, including new features such as the presence of a fast shock in Petschek's mechanism and impulsive bursty reconnection due to secondary tearing and coalescence.

Type
Session IV
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 233 - 244
Copyright
Copyright © Reidel 1985 

References

Browning, P. and Priest, E.R.: 1983, submitted.Google Scholar
Cargill, P.J. and Priest, E.R.: 1982, Solar Phys. 76, 357.Google Scholar
Dungey, J.W.: 1953, Phil. Mag. 44, 725.Google Scholar
Finn, J.M. and Kaw, P.K.: 1977, Phys. Fluids 20, 72.CrossRefGoogle Scholar
Forbes, T.G. and Priest, E.R.: 1982a, Solar Phys. 81, 303.CrossRefGoogle Scholar
Forbes, T.G. and Priest, E.R.: 1982b, Planet. Space Sci. 30, 1983.Google Scholar
Forbes, T.G. and Priest, E.R.: 1983, Solar Phys. 84, 169.CrossRefGoogle Scholar
Furth, H.P., Killeen, J. and Rosenbluth, M.N.: 1963, Phys. Fl. 6, 459.Google Scholar
Heyvaerts, J., Priest, E.R. and Rust, D.M.: 1977, Astrophys. J. 216, 123.Google Scholar
Hood, A.W. and Priest, E.R.: 1979, Solar Phys. 64, 303.Google Scholar
Hood, A.W. and Priest, E.R.: 1980, Solar Phys. 66, 113.CrossRefGoogle Scholar
Hood, A.W.: 1983, submitted.Google Scholar
Kopp, R. and Pneuman, G.W.: 1976, Solar Phys. 50, 85.Google Scholar
Migliulo, S. and Cargill, P.: 1983, submitted.Google Scholar
Milne, A.M. and Priest, E.R.: 1981, Solar Phys. 73, 157.Google Scholar
Mok, Y. and Van Hoven, G.: 1982, Phys. Fluids 25, 636.Google Scholar
Parker, E.N.: 1972, Astrophys. J. 174, 499.CrossRefGoogle Scholar
Parker, E.N.: 1983, Astrophys. J. 264, 635.Google Scholar
Pneuman, G.W.: 1983, Astrophys. J. 265, 468.Google Scholar
Priest, E.R.: 1984, Rep. Prog. Phys.Google Scholar
Pritchett, P.L. and Wu, C.C.: 1979, Phys. Fluids 22, 2140 Google Scholar
Raadu, M.A.: 1972, Solar Phys. 22, 425.Google Scholar
Rosner, R. and Knobloch, E.: 1982, Astrophys. J. 262, 349.Google Scholar
Sakurai, T.: 1976, Pub. Astron. Soc. Japan 28, 177.Google Scholar
Sato, T. and Hayashi, T.: 1979, Phys, Fluids 22, 1189.Google Scholar
Steinolfson, R.S. and Van Hoven, G.: 1983, Phys. Fluids 26, 117.Google Scholar
Steinolfson, R.S. and Van Hoven, G.: 1984, Astrophys. J. Google Scholar
Syrovatsky, S.I.: 1966, Soviet Astron. 10, 270.Google Scholar
Syrovatsky, S.I.: 1978, Solar Phys. 58, 89.Google Scholar
Tsinganos, K.C.: 1982, Astrophys. J. 259, 832.Google Scholar
Tur, T.J. and Priest, E.R.: 1978, Solar Phys. 58, 181.Google Scholar
Ugai, M. and Tsuda, T.: 1977, J. Plasma Phys. 17, 337.Google Scholar
Van Hoven, G., Ma, S.S. and Einaudi, G.: 1981, Astron. Astrophys. 99, 232.Google Scholar
Van Hoven, G., Steinolfson, R.S. and Tachi, T.: 1983, Ap. J. Letts.Google Scholar
Yang, C.K. and Sonnerup, B.U.O.: 1976, Astrophys. J. 206, 570.Google Scholar