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MHD Thermal Instabilities in Inhomogeneous Atmospheres

Published online by Cambridge University Press:  12 April 2016

G. Bodo ,
A. Ferrari ,
S. Massaglia  and
R. Rosner
G. Bodo
Affiliation:
Osservatorio Astronomico di Torino
A. Ferrari
Affiliation:
Istituto di Cosmo-geofisica del C.N.R., Torino Istituto di Fisica Generale, Universita' di Torino
S. Massaglia
Affiliation:
Istituto di Fisica Generale, Universita' di Torino
R. Rosner
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA

Extract

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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.

Type
Session IV: Theoretical Aspects
Information
International Astronomical Union Colloquium , Volume 71: Activity in Red-Dwarf Stars , 1983 , pp. 621 - 623
Copyright
Copyright © Reidel 1983

References

REFERENCES

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