Upper Limit for the Mass Loss Rate of Rapidly Rotating Single Main-Sequence O9-B4 Stars.
Astronomical Observatory, Ural State University, Yekaterinburg, Russia
An upper limit for the mass loss rate of rapidly rotating main-sequence O9-B4 stars has been determined. The maximum mass loss rate of a rotating star is determined by the ability of radiation pressure in lines to remove matter from the gravitational potential well of the star. The maximum mass loss rate in the case of extremely rapid stellar rotation is a factor of 3-7 higher than that in the case of nonrotating star. A simple formula for determining the ratio of the maximum mass loss rate of a rotating star to the maximum mass loss rate of a nonrotating star with the same mass, luminosity, and volume is suggested.
Reference: Astronomy Letters, 2010, Vol.36
Status: Manuscript has been accepted