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The theory of radiation driven wind including stellar rotation isre-examined. After a suitable change of variables, a new equation for the massloss rate is derived analytically. The solution of this equation remains within1% confidence when compared with numerical solutions. Also, a non-linearequation for the position of the critical (singular) point is obtained. Thisequation shows the existence of an additional critical point, besides thestandard m--CAK critical point. For a stellar rotation velocity larger thanaprox. 0.7 - 0.8 V_{breakup}, there exists only one critical point, locatedaway from the star's surface. Numerical solutions crossing through this newcritical point, are attained. In these cases, the wind has a very low terminalvelocity and therefore a higher density wind. Disk formation in Be stars isdiscussed in the frame of this new line driven stellar wind solution.Comment: 40 pages, 15 figures, Accepted for publication in Ap

The Influence of Rotation in Radiation‐driven Wind from Hot Stars: New Solutions and Disk Formation in Be Stars