AM05-08-004 ブラックホール降着流の輻射磁気流体力学シミュレーション(宇宙流体1,一般講演)

概要

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We calculate the vertical structure of a local patch of an accretion disk in which heating by dissipation of MRI-driven MHD turbulence is balanced by radiative cooling. Heating, radiative transport, and cooling are computed self-consistently with the structure by solving the equations of radiation MHD in the searing-box approximation. In a statistically steady state, the disk atmosphere stretches upward, with the photosphere rising to 〜7H (H is the scale height), in contrast to the 〜3H predicted by conventional analytic models. This extended structure is supported by the pressure of the magnetic field, which has escaped from the inside of the disk by magnetic buoyancy. Dissipation is distributed across the region within 〜3H of the midplane, and the dissipated energy is mainly transported to the disk surface by radiation diffusion. The dynamic and thermodynamic balance is stable over 5 thermodynamical time (50 dynamical time).
日本流体力学会の論文
2005-09-05