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Astron. Astrophys. 362, 295-309 (2000)

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New theoretical mass-loss rates of O and B stars

J.S. Vink 1, A. de Koter 2 and H.J.G.L.M. Lamers 1,3

1 Astronomical Institute, Utrecht University, P.O. Box 80000, 3508 TA Utrecht, The Netherlands
2 Astronomical Institute "Anton Pannekoek", University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
3 SRON Laboratory for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands

Received 14 February 2000 / Accepted 7 August 2000


We have calculated mass-loss rates for a grid of wind models covering a wide range of stellar parameters and have derived a mass-loss recipe for two ranges of effective temperature at either side of the bi-stability jump around spectral type B1.

For a large sample of O stars, it is shown that there is now good agreement between these new theoretical mass-loss rates that take multiple scattering into account and observations.

Agreement between the observed and new theoretical wind momenta increases confidence in the possibility to derive distances to luminous stars in distant stellar systems using the Wind momentum Luminosity Relation.

For the winds of the B stars there is an inconsistency in the literature between various mass-loss rate determinations from observations by different methods. One group of [FORMULA] determinations of B stars does follow the new theoretical relation, while another group does not. The lack of agreement between the observed mass-loss rates derived by different methods may point to systematic errors in mass-loss determinations from observations for B stars.

We show that our theoretical mass-loss recipe is reliable and recommend it be used in evolutionary calculations.

Key words: stars: early-type – stars: mass-loss – stars: supergiants – stars: winds, outflows – stars: evolution

Send offprint requests to: J.S. Vink (j.s.vink@astro.uu.nl)

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© European Southern Observatory (ESO) 2000

Online publication: October 30, 19100