  We examine radiative standing shocks in advective accretion flows around
stellar-mass black holes by 2D radiation hydrodynamic simulations, focusing on
the super-Eddington accreting flow. Under a set of input flow parameters
responsible for the standing shock, the shock location on the equator decreases
toward the event horizon with an increasing accretion rate. The optically thin
and hot gas in the narrow funnel region along the rotational axis changes
gradually into a dense and optically thick state with the increasingly dense
gas transported from the base of the radiative shock near the equator. As a
result, the luminosity becomes as high as ~ $10^{40}$ erg $s^{-1}$, and the
radiation shows a strongly anisotropic distribution around the rotational axis
and then very low edge-on luminosity as ~ $10^{36}$ erg $s^{-1}$. The mass
outflow rate from the outer boundary is high as ~ $10^{-5}$ and $10^{-4}$
$M_{\odot} yr^{-1}$ but most of the outflow is originated through the radial
outer boundary and may be observed over a wide wind region. The models show
approximately black body spectra with a temperature of $5 \times 10^{6} - 3
\times 10^{7}$ K at the vertical outer boundary surface. The radiative shock
models with the super-Eddington luminosities show a possible model for the
superaccretor SS 433 and Ultraluminous X-ray sources with stellar-mass black
holes.
