We examine the jets and the disc of SS 433 at super-Eddington luminosities with \dot { M } \sim 600 \dot { M } _ { c } by time-dependent two-dimensional radiation hydrodynamical calculations , assuming \alpha -model for the viscosity .
One-dimensional supercritical accretion disc models with mass loss or advection are used as the initial configurations of the disc .
As a result , from the initial advective disc models with \alpha =0.001 and 0.1 , we obtain the total luminosities \sim 2.5 \times 10 ^ { 40 } and 2.0 \times 10 ^ { 40 } erg s ^ { -1 } .
The total mass-outflow rates are \sim 4 \times 10 ^ { -5 } and 10 ^ { -4 } { M _ { \odot } } yr ^ { -1 } and the rates of the relativistic axial outflows in a small half opening angle of \sim 1 ^ { \circ } are about 10 ^ { -6 } { M _ { \odot } } yr ^ { -1 } : the values generally consistent with the corresponding observed rates of the wind and the jets , respectively .
From the initial models with mass loss but without advection , we obtain the total mass-outflow and axial outflow rates smaller than or comparable to the observed rates of the wind and the jets respectively , depending on \alpha .
In the advective disc model with \alpha = 0.1 , the initially radiation-pressure dominant , optically thick disc evolves to the gas-pressure dominated , optically thin state in the inner region of the disc , and the inner disc is unstable .
Consequently , we find remarkable modulations of the disc luminosity and the accretion rate through the inner edge .
These modulations manifest themselves as the recurrent hot blobs with high temperatures and low densities at the disc plane , which develop outward and upward and produce the QPOs-like variability of the total luminosity with an amplitude of a factor of \sim 2 and quasi-periods of \sim 10 – 25 s. This may explain the massive jet ejection and the QPOs phenomena observed in SS 433 .