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Magnetic Shear and Flares

Published online by Cambridge University Press:  19 July 2016

P. Venkatakrishnan
P. Venkatakrishnan*
Affiliation:
Indian Institute of Astrophysics Bangalore 560034 India

Abstract

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Magnetic tension posseses low values at regions of large magnetic “shear” on the polarity inversion line. The low tension allows for a non-force-free field that depends on the density of the medium. Instabilities which can modify the density may then possibly evolve into solar flares. Heuristic arguments are given to favour instability driven flare scenarios.

Type
VII. Magnetic Reconnection and Coronal Evolution
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 319 - 322
Copyright
Copyright © Kluwer 1990 

References

Colgate, S.A.: 1978, Astrophys. J. , 221, 1068.Google Scholar
Hagyard, M.J., Smith, J.B. Jr., Teuber, D., and West, E. A.: 1984, Solar Phys. , 91, 115.CrossRefGoogle Scholar
Hagyard, M.J., Venkatakrishnan, P. and Smith, J.B. Jr.: 1989, Astrophys. J. Supp. Series (in press).Google Scholar
Kahler, S.W., Moore, R.L., Kane, S.R., and Zirin, H.: 1988, Astrophys. J. , 328, 824.CrossRefGoogle Scholar
Low, B.C.: 1982, Solar Phys. , 77, 43.CrossRefGoogle Scholar
Venkatakrishnan, P.: 1984a Ph.D. Thesis, Bangalore University.Google Scholar
Venkatakrishnan, P.: 1984b, Kodaikanal Obs. Bull. 4, 19.Google Scholar
Venkatakrishnan, P.: 1990, Solar Phys. ,accepted Google Scholar
Wu, S. T., Song, M.T., and Dryer, M.: 1990, IAU Symp. 142.Google Scholar
Zwingmann, W.: 1987, Solar Phys. , 111, 309.CrossRefGoogle Scholar