Abstract
Abstract We examine highly super-Eddington accretion disk models onto a neutron star for SS 433, based on two-dimensional hydrodynamical calculations. The super-Eddington accretion flows form a kind of standing shock elongated along the rotational axis of the disk. This results in a very rarefied, hot, optically thin region between the shock and the axis. The anisotropic radiation fields in this region accelerate the flows to relativistic jets of ∼ 0.2 c with a collimation angle of ∼ 10°–25°. The accretion disk is highly convective or turbulent near to the equatorial plane, and is very geometrically thick. Most of the input accreting matter is blown off from the system through the jets and the disk wind. The super-Eddington accretion disk models are promising to explain SS 433.
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