Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-29T18:42:40.243Z Has data issue: false hasContentIssue false
  • English
  • Français

A Unified Treatment of the Filament and Flare Instabilities

Published online by Cambridge University Press:  04 August 2017

Gerard van Hoven
Gerard van Hoven*
Affiliation:
Department of Physics, University of California, Irvine, California 92717 (U.S.A.)

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.

Filaments and flares occur in sheared magnetic structures as a result of radiative cooling and resistive reconnection, respectively. A new integrated theory of these two unstable processes is described, which includes the relevant effects of magnetohydrodynamics and energy transport. The normally dissociated thermal and tearing phenomena are coupled together by a temperature–dependent Coulomb resistivity. As a result, the filamentation and flaring instabilities of a sheared field may coexist, as is familiar from the solar example.

The growth rates and spatial structures of these two modes are detailed here. The much faster radiative instability is shown to provide significant magnetic reconnection, particularly at shorter wavelengths. The long–wavelength reconnection mode is found to be abetted by the resistivity increase caused by the dominance of cooling at the X point, in contrast to its nonradiative behavior. Implications of these results for the development of coronal activity are described.

Type
Session IV
Information
Symposium - International Astronomical Union , Volume 107: Unstable Current Systems and Plasma Instabilities , 1985 , pp. 263 - 271
Copyright
Copyright © Reidel 1985 

References

Chiuderi, C. and Van Hoven, G.: 1979, Astrophys. J. (Letters) 232, L69.CrossRefGoogle Scholar
Field, G.B.: 1965, Astrophys. J. 142, 531.CrossRefGoogle Scholar
Furth, H.P., Killeen, J., and Rosenbluth, M.N.: 1963, Phys. Fluids 6, 459.CrossRefGoogle Scholar
Hildner, E.: 1974, Solar Phys. 35, 123.CrossRefGoogle Scholar
Killeen, J.: 1970, in Physics of Hot Plasmas, eds. Rye, B.J. and Taylor, J.C. (New York: Plenum), pp. 212–219.Google Scholar
Spitzer, L.: 1962, in Physics of Fully Ionized Gases (New York: Wiley Interscience), pp. 136–145.Google Scholar
Steinolfson, R.S.: 1983, Phys. Fluids 26.CrossRefGoogle Scholar
Steinolfson, R.S. and Van Hoven, G.: 1983, Phys. Fluids 26, 117.CrossRefGoogle Scholar
Steinolfson, R.S. and Van Hoven, G.: 1984, Astrophys. J., to appear.Google Scholar
Tachi, T., Steinolfson, R.S., and Van Hoven, G.: 1983, Phys. Fluids 26.CrossRefGoogle Scholar
Van Hoven, G.: 1979, Astrophys. J. 232, 572.CrossRefGoogle Scholar
Van Hoven, G., Steinolfson, R.S., and Tachi, T.: 1983, Astrophys. J. 268, 860.CrossRefGoogle Scholar
Van Hoven, G., Tachi, T., and Steinolfson, R.S.: 1983, UCI Phys. Rept. No. 83-25, submitted to Astrophys. J. Google Scholar