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Stellar mass loss and atmospheric Instability

Published online by Cambridge University Press:  12 April 2016

Cornelis de Jager  and
Hans Nieuwenhuijzen
Cornelis de Jager
Affiliation:
Astronomical Observatory and Laboratory for Space Research Beneluxlaan 21, 3527 HS UTRECHT, the Netherlands
Hans Nieuwenhuijzen
Affiliation:
Astronomical Observatory and Laboratory for Space Research Beneluxlaan 21, 3527 HS UTRECHT, the Netherlands

Abstract

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A review is given of rate of mass-loss values in the upper part of the Hertzsprung-Russell diagram. Near the luminosity limit of stellar existance = −10−4 M⊙ yr−1. Episodical mass loss in bright variable super- and hypergiants does not significantly increase this value. For Wolf-Rayet stars the rate of mass loss is larger by a factor 140 than for non-evolved stars with the same Teff and L; for C stars this factor is ten. This can be explained qualitatively. Rotation appears hardly to influence the rate of mass loss except for vrot-values close to the break-up velocity. This is in accordance with theory. We suggest the existence of a Red Supergiant Branch; along that branch mass loss is virtually independent of luminosity. Stellar winds along the upper limit of stellar existence are mainly due: to radiation pressure for hot supergiants (≳ 10 000 K); to turbulent pressure for cool supergiants (3000-10 000 K), and to dust-driven and pulsation-driven winds for cooler stars. The turbulent pressure may originate in largescale stochastic motions as observed in Alpha Cyg. Episodical mass loss, as observed in P Cyg, HR 8752 and other Very Luminous Variables may be due to occasional violent stochastic motions, resulting in a shock-driven episodical mass-loss component.

Type
Part II. Mass-Losing Stars in Different Stages of Evolution
Information
International Astronomical Union Colloquium , Volume 108: Atmospherics Diagnostics of Stellar Evolution: Chemical Peculiarity, Mass Loss, and Explosion , 1988 , pp. 102 - 113
Copyright
Copyright © Springer-Verlag 1988

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