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MHD Thermal Instabilities in Inhomogeneous Atmospheres

  • G. Bodo (a1), A. Ferrari (a2) (a3), S. Massaglia (a3) and R. Rosner (a4)

Extract

The Einstein Observatory survey of stellar coronae (Vaiana et al. 1981) and, specifically, the results on cool, low luminosity stars has suggested a correlation between stellar X-ray luminosity and stellar rotational velocity (Pallavicini et al. 1982, Walter 1981, Vaiana et al. 1981). In addition the Skylab observations of the solar corona have demonstrated a tight correlation between photospheric surface magnetic structures, which emerge from the interior in the form of “loops” above the photosphere by, viz., buoyancy instabilities, (Parker 1979; see also Acheson 1979, Schmitt & Rosner 1982, and references therein), and coronal X-ray emission (Golub et al. 1980). It therefore becomes important to ask how a coronal state (i.e. low density and high temperature plasma) of a stellar atmosphere is formed , presumably from a pure radiative equilibrium configuration.

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Copyright

References

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Acheson, D.J. 1979 Solar Physics, 62, p.23
Ferrari, A., Rosner, R., and Vaiana, G. S. 1982, Ap. J. in press
Golub, L., et al. 1980, Ap. J., 238, p. 343
Heyvaerts, J. 1974, Astron. Astrphys. 37, p. 65
Pallavicini, R., et al. 1982, in 2nd Cambridge Cool Stars Workshop, ed. Golub, L. and Giampapa, M.
Parker, E. N. 1979, Cosmical Magnetic Fields (Oxford, Clarendon Press)
Schmitt, J. and Rosner, R. 1982, Ap. J. in press
Vaiana, G. S. et al. 1981, Ap. J. 244, p. 163
Walter, F. G.. 1981, Ap. J. 245, p. 677

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