輻射圧優勢降着流の輻射磁気流体シミュレーション(宇宙流体(2),一般講演)

概要

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Three dimensional radiation magnetohydrodynamics (MHD) simulation is used to explorer radiation-dominated MHD accretion flows around black holes. The local shearing box approximation is employed to simulate a radial slice of geometrically thin and optically thick accretion disk. Magnetorotational instability due to the velocity shear drives MHD turbulence, which dissipates to produce thermal energy. A dynamical and thermal equilibrium state that lasts for at least dozens of thermal times is established in the simulation box. In the dynamical equilibrium, the gravity is compensated by the gradient of radiation pressure near the midplane and by that of magnetic pressure in the upper region. On the other hand, not only radiative diffusion but also radiative advection associated with magnetic buoyancy transport the dissipated thermal energy to the disk surface to achieve the thermal equilibrium.
日本流体力学会の論文
2007-08-06