Modeling Super-Eddington Accretion Flow

Super-Eddington (or supercritical) accretion flow seems to be realized in many astrophysical situations, such as ultra-luminous X-ray Sources, We first discuss several noteworthy observable features of the supercritical accretion flow based on the framework of ( I) one-dimensional, slim disk model. We expect flatter temperature profile, if the accretion rate exceeds the critical rate. and we find such a signature in the X-ray data of some ULXs. We then examine the data of (2) multi-dimensional, global radiation-hydrodynamic (RHD) simulations of disk accretion. Effects of relativistic beaming and gas outflow are particularly stressed there. Finally, we present our most recent results of (3) global, radiation-magnetohydrodynamic (RMHD) simulations of accretion flow. This model could for the first time reproduce the three different regimes of accretion (supercritical, standard-type, and radiatively inefficient accretion flow) with the same code by varying the density normalization.