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Radiative wind acceleration in early type stars

Published online by Cambridge University Press:  12 April 2016

N. Panagia  and
F. Macchetto
N. Panagia
Affiliation:
Istituto di Radioastronomia CNR, Bologna, Italy
F. Macchetto
Affiliation:
ESA Space Science Department, Noordwijk, Netherlands

Abstract

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The processes of radiative acceleration of stellar winds in OB stars by single and multiple photon scattering are considered. Single scattering can be the dominant accelerating process for stars later than B2 (Teff < 2 x 104 K) and can account for terminal velocities up to 500 – 1000 km s-1 . Multiple scattering of photons in the approximate range 200 – 500 A provides additional wind acceleration for stars earlier than B2 to reach terminal velocities of up to 2000 – 4000 km s-1 A systematic increase of the terminal velocity as a function of the effective temperature is predicted. Observational data confirm this expectation quite well.

Type
Session III - Winds From Early Type Stars: Theory
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 173 - 178
Copyright
Copyright © Reidel 1981

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