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Thermal Instability in a Hot Plasma

Published online by Cambridge University Press:  12 April 2016

Steve A. Balbus  and
Noam Soker
Steve A. Balbus
Affiliation:
Department of AstronomyUniversity of VirginiaP. O. Box 3818 University Station Charlottesville, VA 22903U.S.A.
Noam Soker
Affiliation:
Department of AstronomyUniversity of VirginiaP. O. Box 3818 University Station Charlottesville, VA 22903U.S.A.

Abstract

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The nature of local thermal instability in static and dynamic radiating plasmas described by an equilibrium cooling function has been reexamined. Several new results have been found. In a plasma in both thermal and hydrostatic equilibrium, if the cooling function is not an explicit function of position, and does not display isentropic thermal instability (i.e. sound waves are thermally stable), then isobaric thermal instability by the Field criterion is present if and only if convective instability is present by the Schwarzschild criterion. In this case, thermal overstability does not occur. For the case of a dynamical plasma we present a very general Lagrangian equation for the development of nonradial thermal instability. In the limit of large cooling time to free-fall time ratio, the equation is solved analytically by WKBJ techniques. Results are directly applicable to cluster X-ray cooling flows. Such flows are surprisingly stable except for perturbation wavenumbers that are very nearly radial. We believe that the origin of cooling flow optical filaments is not to be found in linear thermal instability.

Type
1. X-rays from a Hot Plasma
Information
International Astronomical Union Colloquium , Volume 115: High Resolution X-ray Spectroscopy of Cosmic Plasmas , 1990 , pp. 44 - 48
Copyright
Copyright © Cambridge University Press 1990

References

Balbus, S.A., and Soker, N. 1988, Ap.J., in press.Google Scholar
Begelman, M.C., McKee, C.F., and Shields, G.A. 1983, Ap. J., 271, 70.Google Scholar
Canizares, C.R., Markert, T.H., and Donahue, M. 1987, in Cooling Flows in Clusters and Galaxies, ed. Fabian, A.C., (Kluwer: Dordrecht), p. 73.Google Scholar
Field, G.B. 1965, Ap. J., 142, 531.CrossRefGoogle Scholar
Hu, E.M., Cowie, L.L., and Wang, Z. 1985, Ap. J. Suppl., 59, 447.Google Scholar
Lazareff, B., Castets, A., Kim, D.-W., and Jura, M. 1988, preprint.Google Scholar
Mathews, W.G., and Bregman, J.N. 1978, Ap. J., 224, 308.Google Scholar
Nulsen, P.E.J. 1986, M.N.R.A.S., 221, 337.Google Scholar
Raymond, J.C., Cox, D.P., and Smith, B.W. 1976, Ap. J., 204, 290.CrossRefGoogle Scholar
Sarazin, C.L. 1986, REv. Mod. Phys., 58, 1.CrossRefGoogle Scholar
Thomas, P.A. 1987, in Cooling Flows in Clusters and Galaxies, ed. Fabian, A.C., (Kluwer: Dordrech), p. 361.Google Scholar
White, R.E. III, and Sarazin, C.L. 1987, Ap. J., 318, 612.CrossRefGoogle Scholar