Bending Waves and Standing Shocks in Numerically Simulated Tilted Black-Hole Accretion Disks

Details Bending Waves and Standing Shocks in Numerically Simulated Tilted Black-Hole Accretion Disks Bending Waves and Standing Shocks in Numerically Simulated Tilted Black-Hole Accretion Disks

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.4808f&link_type=abstract

American Astronomical Society, AAS Meeting #211, #48.08; Bulletin of the American Astronomical Society, Vol. 39, p.810

Astronomy and Astrophysics

Astronomy

Scientific paper

This work presents a detailed analysis of the overall flow structure and unique features of the inner region of the tilted disk simulations described in Fragile et al. (2007, ApJ, 668, 417). We identify a quasi-stationary bending wave that drives large-scale circulation through the disk. We also find an extended quasi-stationary shock associated with the previously identified plunging streams. The shock occurs where material not associated with the plunging streams intersects the streams while orbiting the black hole. The plunging stream and associated shock are roughly aligned with the line of nodes between the disk and black-hole midplanes. As the disk precesses (on a timescale much longer than the orbital timescale) the plunging stream and shock also precess. This precessing structure could present a very strong low frequency QPO signal due to the changing viewing angle and aspect ratio. For the disk in this simulation, the precession has a frequency of 3(M&sun;/M) Hz. However, this value is strongly dependent on the size of the disk. The standing shock could also serve as a potential site for particle acceleration.

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