Radiative Disk Winds from a Self-Similar Slim Disk

Ken-ya Watarai, Jun Fukue
1999 Nippon Tenmon Gakkai obun kenkyu hokoku  
We investigated the radiation fields of a self-similar slim disk and the behavior of wind particles, which are driven by the radiation pressure of a self-similar slim disk. When the accretion rate is of the order of a critical rate, the accretion disk must puff up in the vertical direction to form a so-called slim disk. In contrast to a standard alpha disk, this slim disk has two major features: i) the disk is geometrically (mildly) thick, and ii) the radial motion is comparable to the
more » ... ble to the rotational motion (advection). These effects make the opening angle of the disk less than 180°, and the disk radiation fields are expected to enhance towards the center. However, we found that trajectories of wind particles are accelerated along the disk surface. This indicates that the shape of the disk strongly influence the motion of plasma particles. Furthermore, particles lose angular momentum by radiation drag, while gaining angular momentum from rotating radiation fields. Taking into consideration the Compton drag, the income and expenditure of angular momentum of wind particles is positive, and they tend to spread out in a radial direction. The parameter / is the viscous-dissipated energy which is stored in the accreting gas as entropy, 1 -/ radiative cooling. We assume that / is independent of r. This as-
doi:10.1093/pasj/51.5.725 fatcat:bnqdlbmo3bdozjncacj6qlffpi