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The formation of shells in the wind from P Cygni
Published online by Cambridge University Press: 12 April 2016
Abstract
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A mechanism is proposed for the formation of shells around P Cygni. These shells seem to arise at approximately two monthly intervals and each appears to undergo a steady acceleration of some 0.6 cm s-2 during the six months that it is present. In the process to be described the formation of the shells takes place in a stellar wind that moves outwards ballistically from the photosphere. Small fluctuations in wind speed are introduced there and eventually lead to the condensation of shells at a radial distance of the order of 1014 cm. The density in the shells is large enough to account for their acceleration by the Lyman continuum emitted by the star. It is also proposed here that the observed time scale of two months is set by the dynamics of the flow field in interaction with the random fluctuations imposed on it at the photosphere.
- Type
- Section I: Main Papers, General Discussions, and Two Panel Discussions
- Information
- International Astronomical Union Colloquium , Volume 113: Physics of Luminous Blue Variables , 1989 , pp. 177 - 184
- Copyright
- Copyright © Kluwer 1989
References
Lamers, H. J. G. L.M.: 1987 in Instabilities in Luminous Early Type Stars, eds. Lamers, H. G. J. L. M. and de Loore, C. W. H., Reidel, Dordrecht, p.99.Google Scholar
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