RADIATIVE DISK WINDS UNDER RADIATION DRAG II

Radiatively accelerated accretion-disk winds, which consist of ionized gas particles and are accelerated in disk radiation fields, were exam ined, taking into account radiation drag. For the present purpose, we quantitatively calculate the full components of radiation fields produ ced by a standard accretion disk around a black hole, considering the Doppler enhancement to the first order of vie. As a result, there appe ar to be two major effects, which are dropped in the traditional radia tive winds. First, a radiation-drag force appears, which is proportion al to the particle velocity in this order and suppresses the motion of wind particles. Second, we emphasize that an azimuthal component of r adiative flux appears, since the disk radiation field has angular mome ntum. Using the components of radiation fields, we examined the radiat ive disk winds without imposing a near-disk approximation. Compared wi th the non-dragged winds, where the radiation-drag force is dropped, t he acceleration in the vertical direction is suppressed due to the eff ect of radiation drag. That is, the radiation-drag force makes winds h arder to blow than winds without the drag force. We obtained the escap e condition of the radiative disk winds. In the present case, the disk wind blows from the inner disk when the disk luminosity exceeds 80% o f the Eddington luminosity (in the case without the drag force it blow s when the disk luminosity exceeds 60% of the Eddington luminosity). M oreover, these values become much smaller than the values obtained in a previous study, when the near-disk approximation was used, since the spatial variations of the disk radiation fields were fully taken into account in the present case.