We apply our two-dimensional ( 2D ) , radially self-similar steady-state accretion flow model to the analysis of hydrodynamic simulation results of supercritical accretion flows .
Self-similarity is checked and the input parameters for the model calculation , such as advective factor and heat capacity ratio , are obtained from time-averaged simulation data .
Solutions of the model are then calculated and compared with the simulation results .
We find that in the converged region of the simulation , excluding the part too close to the black hole , the radial distribution of azimuthal velocity v _ { \phi } , density \rho and pressure p basically follows the self-similar assumptions , i.e .
they are roughly proportional to r ^ { -0.5 } , r ^ { - n } , and r ^ { - ( n + 1 ) } , respectively , where n \sim 0.85 for the mass injection rate of 1000 L _ { \mathrm { E } } / c ^ { 2 } , and n \sim 0.74 for 3000 L _ { \mathrm { E } } / c ^ { 2 } .
The distribution of v _ { r } and v _ { \theta } agrees less with self-similarity , possibly due to convective motions in the r \theta plane .
The distribution of velocity , density and pressure in \theta direction obtained by the steady model agrees well with the simulation results within the calculation boundary of the steady model .
Outward mass flux in the simulations is overall directed toward polar angle of 0.8382 rad ( \sim 48.0 ^ { \circ } ) for 1000 L _ { \mathrm { E } } / c ^ { 2 } , and 0.7852 rad ( \sim 43.4 ^ { \circ } ) for 3000 L _ { \mathrm { E } } / c ^ { 2 } , and \sim 94 % of the mass inflow are driven away as outflow , while outward momentum and energy fluxes are focused around the polar axis .
Part of these fluxes lie in the region that are not calculated by the steady model , and special attention should be paid when the model is applied .