Super-Eddington Black-Hole Models for SS 433

Abstract

Abstract We examine highly super-Eddington black-hole models for SS 433, based on two-dimensional hydrodynamical calculations coupled with radiation transport. The super-Eddington accretion flow with a small viscosity parameter, $ \alpha = 10^{-3}$, results in a geometrically–and optically-thick disk with a large opening angle of $ \sim 60^{\circ}$ to the equatorial plane and a very rarefied, hot, and optically-thin high-velocity jets region around the disk. The thick accretion flow consists of two different zones: an inner advection-dominated zone and an outer convection-dominated zone. The high-velocity region around the disk is divided into two characteristic regions, a very rarefied funnel region along the rotational axis and a moderately rarefied high-velocity region outside of the disk. The temperatures of $ \sim 10^7 \,\mathrm{K}$ and the densities of $ \sim 10^{-7} \,\mathrm{g} \,\mathrm{cm}^{-3}$ in the upper disk vary sharply to $ \sim 10^8 \,\mathrm{K}$ and $ 10^{-8}\,\mathrm{g} \,\mathrm{cm}^{-3}$, respectively, across the disk boundary between the disk and the high-velocity region. The X-ray emission of iron lines would be generated only in a confined region between the funnel wall and the photospheric disk boundary, where flows are accelerated to relativistic velocities of $ \sim 0.2 \,c$ due to the dominant radiation-pressure force. The results are discussed regarding the collimation angle of the jets, the large mass-outflow rate observed in SS 433, and the ADAFs and the CDAFs models.