Maximum massloss rates of linedriven winds of massive stars: The effect of rotation and an application to η Carinae
Abstract
We investigate the effect of rotation on the maximum massloss rate due to an opticallythin radiativelydriven 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 massloss rate. We include the Von Zeipel effect and the oblateness of the star in our calculations. We determine the maximum surfaceintegrated 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_{☉})<6.0. We also determine the corresponding maximum loss of angular momentum. We find that rotation increases the maximum massloss 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 EddingtonGamma limit suffer extreme mass loss already for a low equatorial rotation velocity. We compare the maximum massloss 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 massloss rates. Finally, we provide a massloss model for the LBV η Carinae that is able to explain the large observed current massloss rate of ∼10^{3} M_{☉} yr^{1} but that leads to too low wind velocities compared to those derived from observations.
 Publication:

Astronomy and Astrophysics
 Pub Date:
 May 2004
 DOI:
 10.1051/00046361:20040090
 Bibcode:
 2004A&A...418..639A
 Keywords:

 stars: earlytype;
 stars: massloss;
 stars: winds;
 outflows;
 stars: