Super-Eddington Black-Hole Models for SS 433

We examine highly super-Eddington black-hole models for SS 433, based ontwo-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 witha large opening angle of $\sim 60^{\circ}$ to the equatorial plane and a veryrarefied, hot, and optically thin high-velocity jets region around the disk. The thick accretion flow consists of two different zones: an inneradvection-dominated zone and an outer convection-dominated zone. Thehigh-velocity region around the disk is divided into two characteristicregions, a very rarefied funnel region along the rotational axis and amoderately rarefied high-velocity region outside of the disk. The temperaturesof $\sim 10^7$ K and the densities of $\sim 10^{-7}$ g cm$^{-3}$ in the upperdisk vary sharply to $\sim 10^8$ K and $10^{-8}$ g cm$^{-3}$, respectively,across the disk boundary between the disk and the high-velocity region. TheX-ray emission of iron lines would be generated only in a confined regionbetween the funnel wall and the photospheric disk boundary, where flows areaccelerated to relativistic velocities of $\sim$ 0.2 $c$ due to the dominantradiation-pressure force. The results are discussed regarding the collimationangle of the jets, the large mass-outflow rate obserevd in SS 433, and theADAFs and the CDAFs models.Comment: 19 pages, 11 figures, to be published in Publ. Astron. Soc. Japan, 200