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Mass Loss from Eruptive Stars

Published online by Cambridge University Press:  14 August 2015

A. A. Boyarchuk
A. A. Boyarchuk*
Affiliation:
Krymskaya Astrofizicheskaya Observatoriya, U.S.S.R.

Extract

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The previous reports by Lüst and by Pottasch concerned quasi-stationary mass loss. The loss is called quasi-stationary because the basic characteristics of a star, its temperature and its radius, do not change significantly during the time that a particle needs to flow from the stellar surface out to a point where the stellar influence is negligible. However there are many stars which show significant changes of temperature and radius within a short time. Very often these changes are accompanied by instantaneous ejection of a great amount of material. For example, during the outburst of a nova the ejected mass can reach 10−4M⊙. Such effects are very appreciable in the so-called ‘eruptive variables’, in which the brightness changes spasmodically. It is very likely that the rate and the mechanism of mass loss of eruptive variables are different from that of normal stars.

Type
Part II: Interaction of Stars and Interstellar Medium
Information
Symposium - International Astronomical Union , Volume 39: Interstellar Gas Dynamics , 1970 , pp. 281 - 290
Copyright
Copyright © Reidel 1970 

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