Abstract
It is well known that stellar winds are an ubiquitous feature of young, massive, very luminous stars at the upper end of the main sequence with masses in the range 20–200 M and that the evolution of these objects is strongly affected by severe mass-loss connected with the stellar winds. The most promising attempt to explain these winds quantitatively is the theory of radiation driven winds, which has been established in its original form by Lucy and Solomon (1970) and Castor, Abbott and Klein (1975, “CAK”). Most of the basic observational properties of the hot massive star stellar winds can be explained by this self-consistent theory, if the substantial improvements, which have been worked out very recently (Pauldrach, Puls, Kudritzki (1986), “PPK”; Kudritzki, Pauldrach, Puls (1987); Pauldrach (1987), Puls (1987)) are taken into account.
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© 1988 Kluwer Academic Publishers
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Pauldrach, A., Kudritzki, R.P., Gabler, R., Wagner, A. (1988). Radiation Driven Winds of Central Stars of Planetary Nebulae. In: Bianchi, L., Gilmozzi, R. (eds) Mass Outflows from Stars and Galactic Nuclei. Astrophysics and Space Science Library, vol 142. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-2941-8_5
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DOI: https://doi.org/10.1007/978-94-009-2941-8_5
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