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 (1) 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.