D332 光学的に薄いブラックホール降着円盤の3次元MHD数値実験 : 輻射冷却の効果(D-33 宇宙流体(3),一般講演)

概要

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We present the results of three-dimensional global resistive magnetohydrodynamic (MHD) simulations of optically thin black hole accretion flows. Radiative cooling term is included in the energy equation. General relativistic effects are simulated by using the pseudo-Newtonian potential. The initial state is a rotating torus threaded by weak toroidal magnetic fields. As the magneto-rotational instability (MRI) grows in the torus, mass accreting from the torus forms an optically thin, hot accretion disk. When the surface density of the disk exceeds a threshold, the disk makes transition toward an optically thick, cool disk. We found that during this transition, the disk becomes dominated by magnetic pressure because magnetic pressure increases as the disk shrinks in the vertical direction conserving the toroidal magnetic flux.
日本流体力学会の論文
2004-08-09