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 \sim 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 .