The disk wind , which is powered by the radiation force due to spectral lines ( line force ) , is studied for broad absorption line ( BAL ) quasars .
We investigate the structure of the disk wind based on the non-hydrodynamic method and compare with wind properties inferred from X-ray observations of BAL quasars .
In this paper , we apply the stellar wind theory to the initial condition ( the mass outflow rate at the base of the wind ) .
We found the funnel-shaped winds with a half opening angle of \sim 50 ^ { \circ } for the case of \epsilon = 0.3 - 0.9 and M _ { BH } = 10 ^ { 7 - 8.5 } M _ { \odot } , where \epsilon is the Eddington ratio and M _ { BH } is the black hole mass .
Thus , the absorption features are observed for an observer of which a viewing angle is around 50 ^ { \circ } .
A probability of BAL quasars is \sim 7 - 11 \% , which is roughly consistent the abundance ratio of BAL quasars , \sim 10 - 15 \% .
Here , the probability is estimated by the solid angle , that the absorbing features would be detected , divided by 4 \pi .
In contrast , if the Eddington ratio is smaller than 0.01 or if the black hole is very massive , M _ { BH } \gtrsim 10 ^ { 9 } M _ { \odot } , the disk wind is not launched due to the less effective line force .
Then , the quasars are identified as non-BAL quasars independently of the observer ’ s viewing angle .