By performing two-dimensional axisymmetric general relativistic radiation magnetohydrodynamics simulations with spin parameter
varying from -0.9 to
0.9, we investigate the dependence on the black hole spin of the energy flow
from supercritical accretion disk around stellar mass black hole. It is found
that 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 force
cannot be neglected, when is large. The energy outflow efficiency
(total luminosity normalized by ; and
are the mass accretion rate at the event horizon and the light speed) is
larger for rotating black holes than for non-rotating black holes. This is
for , for , and for for
( is Eddington
luminosity). Also, although the energy is mainly released by radiation when
, the Poynting power increases with and exceeds the
radiative luminosity for models with and . The
more the black hole rotates, the larger the power ratio of the kinetic
luminosity to the isotropic luminosity tends to be. This implies that objects
with large (small) power ratio may have rapidly (slowly) rotating black holes.
Among ultraluminous X-ray sources, IC342 X-1, is a candidate with a rapidly
rotating black hole.