Relaxation oscillations and double temperature structures in stellar coronae

Details Relaxation oscillations and double temperature structures in stellar coronae Relaxation oscillations and double temperature structures in stellar coronae

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...125...69h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 125, no. 1, Aug. 1983, p. 69-74. Research supported by the Nederlandse Organis

Astronomy and Astrophysics

Astrophysics

8

Early Stars, Stellar Coronas, Stellar Oscillations, Stellar Temperature, Photosphere, Stellar Mass Ejection, Stellar Winds, Temperature Distribution

Scientific paper

Further work using the iterative method of Hearn and Vardavas (1981) for calculating stationary models for stellar coronae has shown that the coronae of small extent obtained with large fluxes of mechanical energy are not stable. It is suggested that the corona undergoes a relaxation oscillation in which a single extended corona collapses to a double corona which in turn builds up to a single extended corona again. Such a coronal relaxation oscillation may be an explanation for the observed variations of mass loss from late B and early A type supergiants and perhaps from Be stars. The inclusion of radiative forces resulting from the absorption of photospheric radiation by resonance lines should increase the period of the oscillation. If these radiative forces are sufficiently strong they should stabilize the oscillation giving a double corona structure. Such a model could in principle explain the observed soft X-ray emission of OB supergiants and the discrepancy between mass loss rates deduced from the ultraviolet and radio measurements.

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