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To what extent can the one-dimensional slim disk model reproduce themulti-dimensional results of global radiation-hydrodynamic simulations ofsuper-Eddington accretion? With this question in mind, we perform systematicsimulation study of accretion flow onto a non-spinning black hole for a varietyof 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 adequatelyresolve large-scale outflow structure, we extensively expand a simulation boxto cover the space of $3000 r_{\rm S}$ (with $r_{\rm S}$ being theSchwarzschild radius), larger than those in most previous studies, so that wecan put relatively large angular momentum to the gas injected from the outersimulation boundary. The adopted Keplerian radius, at which the centrifugalforce balances with the gravitational force, is $r_{\rm K}=300 r_{\rm S}$. Theinjected mass first falls and is accumulated at around this radius and thenslowly accretes towards the central black hole via viscosity. We simulate suchaccretion processes, taking inverse and bulk Compton scattering into account.The simulated accretion flow is in a quasi-steady state inside $r_{\rm qss}\sim200 r_{\rm S}$. Within this radius the flow properties are, as a whole, in goodagreement with those described by the slim disk model except that the radialdensity 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 efficientconvection. We find very weak outflow from inside $r\sim 200 r_{\rm S}$ unlikethe past studies.

Systematic two-dimensional radiation hydrodynamic simulations of super-Eddington accretion flow and outflow: Comparison with the slim disk model