The influence of rotation in radiation driven wind from hot stars: New solutions and disk formation in Be stars

Abstract

The theory of radiation driven wind including stellar rotation is re-examined. After a suitable change of variables, a new equation for the mass loss rate is derived analytically. The solution of this equation remains within 1% confidence when compared with numerical solutions. Also, a non-linear equation for the position of the critical (singular) point is obtained. This equation shows the existence of an additional critical point, besides the standard m--CAK critical point. For a stellar rotation velocity larger than aprox. 0.7 - 0.8 V_{breakup}, there exists only one critical point, located away from the star's surface. Numerical solutions crossing through this new critical point, are attained. In these cases, the wind has a very low terminal velocity and therefore a higher density wind. Disk formation in Be stars is discussed in the frame of this new line driven stellar wind solution.

arXiv comment40 pages, 15 figures, Accepted for publication in ApJ

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