  To what extent can the one-dimensional slim disk model reproduce the
multi-dimensional results of global radiation-hydrodynamic simulations of
super-Eddington accretion? With this question in mind, we perform systematic
simulation study of accretion flow onto a non-spinning black hole for a variety
of black hole masses of $(10 - 10^7) M_{\odot}$ and mass accretion rates of
$(1.4 \times 10^2 - 5.6 \times 10^3)L_{\rm Edd}/c^2$ (with $L_{\rm Edd}$ and
$c$ being the Eddington luminosity and speed of light). In order to adequately
resolve large-scale outflow structure, we extensively expand a simulation box
to cover the space of $3000 r_{\rm S}$ (with $r_{\rm S}$ being the
Schwarzschild radius), larger than those in most previous studies, so that we
can put relatively large angular momentum to the gas injected from the outer
simulation boundary. The adopted Keplerian radius, at which the centrifugal
force balances with the gravitational force, is $r_{\rm K}=300 r_{\rm S}$. The
injected mass first falls and is accumulated at around this radius and then
slowly accretes towards the central black hole via viscosity. We simulate such
accretion processes, taking inverse and bulk Compton scattering into account.
The simulated accretion flow is in a quasi-steady state inside $r_{\rm qss}\sim
200 r_{\rm S}$. Within this radius the flow properties are, as a whole, in good
agreement with those described by the slim disk model except that the radial
density profile of the underlying disk is much flatter, $\rho\propto r^{-0.73}$
(cf. $\rho\propto r^{-3/2}$ in the slim disk model), due probably to efficient
convection. We find very weak outflow from inside $r\sim 200 r_{\rm S}$ unlike
the past studies.
