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Abstract We perform axisymmetric two-dimensional radiation-hydrodynamic simulations of super-Eddington accretion flow and outflow around black holes to examine the properties of radiation and outflow as functions of the black hole mass and the accretion rate on to the black hole (Ṁ ₁₇). We find that the ṁ ₁₇ (Ṁ ₁₇c² /L ₄₃₃) dependence of L ₑ₀₃/L ₄₃₃ and L ₌₄₂₇/L ₄₃₃ found for a stellar-mass black hole can apply to the high-mass cases, where L ₑ₀₃ is the radiation luminosity, L ₌₄₂₇ is the mechanical luminosity, c is the speed of light, and L ₄₃₃ is the Eddington luminosity. Such universalities can appear in the regime in which electron scattering opacity dominates over absorption opacity. Further, the normalized isotropic mechanical luminosity L ₌₄₂₇^ ISO/L ₄₃₃ (evaluated by normalized density and velocity at =10^) exhibits a broken power-law relationship with ṁ ₁₇; L ₌₄₂₇^ ISO/ L ₄₃₃ ṁ ₁₇^2. 7 (or ṁ ₁₇^0. 7) below (above) ṁ ₁₇ 400. This is because the radial velocity stays nearly constant (or even decreases) below (above) the break with increase of ṁ ₁₇. We also find that the luminosity ratio is L ₌₄₂₇/L ₑ₀₃^ ISO 0. 05 at ṁ ₁₇ 100, which is roughly consistent with the observations of NLS1, 1H 0323+103.
Yoshioka et al. (Fri,) studied this question.