Hydrodynamic Simulations of Tilted Thick-Disk Accretion onto a Kerr Black Hole

Details Hydrodynamic Simulations of Tilted Thick-Disk Accretion onto a Kerr Black Hole Hydrodynamic Simulations of Tilted Thick-Disk Accretion onto a Kerr Black Hole

2004-03-15

arxiv.org/abs/astro-ph/0403356v2

Astronomy and Astrophysics

Astrophysics

51 pages, 34 figures (color figures reduced for this archive), this version accepted to ApJ

Scientific paper

10.1086/428433

We present results from fully general relativistic three-dimensional numerical studies of thick-disk accretion onto a rapidly-rotating (Kerr) black hole with a spin axis that is tilted (not aligned) with the angular momentum vector of the disk. We initialize the problem with the solution for an aligned, constant angular momentum, accreting thick disk, which is then allowed to respond to the Lense-Thirring precession of the tilted black hole. The precession causes the disk to warp, beginning at the inner edge and moving out on roughly the Lense-Thirring precession timescale. The propagation of the warp stops at a radius in the disk at which other dynamical timescales, primarily the azimuthal sound-crossing time, become shorter than the precession time. At this point, the warp effectively freezes into the disk and the evolution becomes quasi-static, except in cases where the sound-crossing time in the bulk of the disk is shorter than the local precession timescale. We see evidence that such disks undergo near solid-body precession after the initial warping has frozen in. Simultaneous to the warping of the disk, there is also a tendency for the midplane to align with the symmetry plane of the black hole due to the preferential accretion of the most tilted disk gas. This alignment is not as pronounced, however, as it would be if more efficient angular momentum transport (e.g. from viscosity or magneto-rotational instability) were considered.

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