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We present the detailed global structure of black hole accretion flows andoutflows through newly performed two-dimensional radiation-magnetohydrodynamicsimulations. By starting from a torus threaded with weak toroidal magneticfields and by controlling the central density of the initial torus, rho_0, wecan reproduce three distinct modes of accretion flow. In model A with thehighest central density, an optically and geometrically thick supercriticalaccretion disk is created. The radiation force greatly exceeds the gravityabove the disk surface, thereby driving a strong outflow (or jet). Because ofthe mild beaming, the apparent (isotropic) photon luminosity is ~22L_E (whereL_E is the Eddington luminosity) in the face-on view. Even higher apparentluminosity is feasible if we increase the flow density. In model B with amoderate density, radiative cooling of the accretion flow is so efficient thata standard-type, cold, and geometrically thin disk is formed at radii greaterthan ~7R_S (where R_S is the Schwarzschild radius), while the flow isradiatively inefficient otherwise. The magnetic-pressure-driven disk windappears in this model. In model C the density is too low for the flow to beradiatively efficient. The flow thus becomes radiatively inefficient accretionflow, which is geometrically thick and optically thin. The magnetic-pressureforce, in cooperation with the gas-pressure force, drives outflows from thedisk surface, and the flow releases its energy via jets rather than viaradiation. Observational implications are briefly discussed.

Global Structure of Three Distinct Accretion Flows and Outflows around Black Holes through Two-Dimensional Radiation-Magnetohydrodynamic Simulations