Fluctuating moment (see eq.(1)) can be estimated as:
So for D we can write the equation which differs from eq.(6) (Lipunov & Popov 1995):
where -turbulent velocity, -characteristic scale of the turbulence. This scale is of order of radius of gravitational capture, :
where
The turbulent velocity is less or equal to the sound speed, (in opposite case a great bulk of energy will dissipate in the form of shock waves), that's why we can write:
where and .
From eq. (12) we can get:
here 
As we see there is a strong dependence of D on v. So we can evaluate v(in this case it is the stellar wind velocity, ):
Values of are shown in table 3.