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By performing 2.5-dimensional special relativistic radiationmagnetohydrodynamics simulations, we study the super-critical accretion disksand the outflows launched via the radiation force. We find that the outflow isaccelerated by the radiation flux force, but the radiation drag force preventsthe outflow velocity from increasing. The outflow velocity saturates around30-40% of the light speed around the rotation axis, since then the flux forcebalances with the drag force. Our simulations show that the outflow velocity iskept nearly constant in the regime of \dot{M}_{BH} ~ 100-1000 L_{Edd}/c^2,where \dot{M}_{BH} is the mass accretion rate, L_{Edd} is the Eddingtonluminosity, and c is the light speed. Such a faster outflow is surrounded by aslower outflow of ~ 0.1c. This velocity is also determined by force balancebetween the radiation flux force and the radiation drag. The radiation dragworks to collimate the slower outflow in cooperation with the Lorentz force,although the faster outflow is mainly collimated by the Lorentz force. Thekinetic energy is carried by the slower outflow rather than by the fasteroutflow. The total kinetic luminosity of the outflow as well as the photonluminosity is ~ L_{Edd}, almost independent of the mass accretion rate.

publications of the astronomical society of japan

Radiation Drag Effects in Black Hole Outflows from Super-critical  Accretion Disks via Special Relativistic Radiation Magnetohydrodynamics  Simulations