EDP Sciences
Free access
Volume 418, Number 2, May I 2004
Page(s) 639 - 648
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20040090

A&A 418, 639-648 (2004)
DOI: 10.1051/0004-6361:20040090

Maximum mass-loss rates of line-driven winds of massive stars: The effect of rotation and an application to $\eta\,$Carinae

C. Aerts1, H. J. G. L. M. Lamers2, 3 and G. Molenberghs4

1  Institute of Astronomy, Catholic University of Leuven, Celestijnenlaan 200 B, 3001 Leuven, Belgium
2  Astronomical Institute, Utrecht University, PO Box 80000, 3508 TA Utrecht, The Netherlands
3  SRON Laboratory, for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
4  Center for Statistics, Limburgs Universitair Centrum, Universitaire Campus, Building D, 3590 Diepenbeek, Belgium

(Received 31 March 2003 / Accepted 10 January 2004)

We investigate the effect of rotation on the maximum mass-loss rate due to an optically-thin radiatively-driven wind according to a formalism which takes into account the possible presence of any instability at the base of the wind that might increase the mass-loss rate. We include the Von Zeipel effect and the oblateness of the star in our calculations. We determine the maximum surface-integrated mass that can be lost from a star by line driving as a function of rotation for a number of relevant stellar models of massive OB stars with luminosities in the range of $5.0< \log\,(L/L_{\odot})<6.0$. We also determine the corresponding maximum loss of angular momentum. We find that rotation increases the maximum mass-loss rate by a moderate factor for stars far from the Eddington limit as long as the ratio of equatorial to critical velocity remains below 0.7. For higher ratios, however, the temperature, flux and Eddington factor distributions change considerably over the stellar surface such that extreme mass loss is induced. Stars close to the Eddington-Gamma limit suffer extreme mass loss already for a low equatorial rotation velocity. We compare the maximum mass-loss rates as a function of rotation velocity with other predicted relations available in the literature which do not take into account possible instabilities at the stellar surface and we find that the inclusion thereof leads to extreme mass loss at much lower rotation rates. We present a scaling law to predict maximum mass-loss rates. Finally, we provide a mass-loss model for the LBV $\eta\,$Carinae that is able to explain the large observed current mass-loss rate of ~ $10^{-3}\,M_\odot\,$yr -1 but that leads to too low wind velocities compared to those derived from observations.

Key words: stars: early-type -- stars: mass-loss -- stars: winds, outflows -- stars: evolution -- methods: statistical -- stars: individual: $\eta\,$Car

Offprint request: C. Aerts, conny@ster.kuleuven.ac.be

SIMBAD Objects

© ESO 2004

What is OpenURL?

The OpenURL standard is a protocol for transmission of metadata describing the resource that you wish to access.

An OpenURL link contains article metadata and directs it to the OpenURL server of your choice. The OpenURL server can provide access to the resource and also offer complementary services (specific search engine, export of references...). The OpenURL link can be generated by different means.

  • If your librarian has set up your subscription with an OpenURL resolver, OpenURL links appear automatically on the abstract pages.
  • You can define your own OpenURL resolver with your EDPS Account.
    In this case your choice will be given priority over that of your library.
  • You can use an add-on for your browser (Firefox or I.E.) to display OpenURL links on a page (see http://www.openly.com/openurlref/). You should disable this module if you wish to use the OpenURL server that you or your library have defined.