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By performing two-dimensional axisymmetric general relativistic radiationmagnetohydrodynamics simulations with spin parameter $a^*$ varying from -0.9 to0.9, we investigate the dependence on the black hole spin of the energy flowfrom supercritical accretion disk around stellar mass black hole. It is foundthat optically and geometrically thick disks form near the equatorial plane,and a part of the disk matter is launched from the disk surface in all models.The gas ejection is mainly driven by the radiative force, but magnetic forcecannot be neglected, when $|a^*|$ is large. The energy outflow efficiency(total luminosity normalized by $\dot{M}_{\rm in} c^2 $; $\dot{M}_{\rm in}$ and$c$ are the mass accretion rate at the event horizon and the light speed) islarger for rotating black holes than for non-rotating black holes. This is$0.7\%$ for $a^*=-0.7$, $0.3\%$ for $a^*=0$, and $5\%$ for $a^*=0.7$ for$\dot{M}_{\rm in} \sim 100L_{\rm Edd}/c^2$ ($L_{\rm Edd}$ is Eddingtonluminosity). Also, although the energy is mainly released by radiation when$a^* \sim 0$, the Poynting power increases with $|a^*|$ and exceeds theradiative luminosity for models with $a^* \geq 0.5$ and $a^* \leq -0.7$. Themore the black hole rotates, the larger the power ratio of the kineticluminosity to the isotropic luminosity tends to be. This implies that objectswith large (small) power ratio may have rapidly (slowly) rotating black holes.Among ultraluminous X-ray sources, IC342 X-1, is a candidate with a rapidlyrotating black hole.

Component of energy flow from supercritical accretion disks around rotating stellar mass black holes