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

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

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..apr.k1024f&link_type=abstract

American Physical Society, April Meeting, 2004, May 1-4, 2004, Denver, Colorado April 2004, MEETING ID: APR04, abstract #K1.024

Statistics

Computation

Scientific paper

We present detailed results from three-dimensional, general relativistic numerical studies of tilted thick-disk accretion onto a rapidly-rotating (Kerr) black hole. These results may be relevant to X-ray binaries, active-galactic nuclei, core-collapse supernovas, and gamma-ray burst progenitors. In this work, we explore two different values of the black-hole spin parameter: a/M=+0.9 (prograde disk) and a/M=-0.9 (retrograde disk); and three different values for the initial tilt of the disk: 0, 15, and 30 degrees. Similar to previous work, we initialize each model with the solution for an aligned, constant angular momentum, accreting thick disk. The black hole is then instantaneously tilted using a transformation of the metric. The disk is allowed to respond to the Lense-Thirring precession of the tilted black hole. As expected, the tilted disks gradually reach a quasi-static twisted, warped configuration. We also find that the mass accretion rate depends strongly on the initial tilt angle. We attempt this problem with three different computational grid geometries: Cartesian, spherical, and spherical with a logarithmic radial coordinate. Although the Cartesian grid has the advantages of being free of any coordinate singularities and not favoring any particular symmetry, we find that it does not adequately maintain the angular momentum of the disk. The spherical grid does much better in this regard. The logarithmic radial coordinate dramatically improves resolution near the black-hole horizon and noticeably improves the accuracy of the mass accretion rate.

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