Quasi-spherical, Time-dependent Viscous Accretion Flow With High Viscosity

Details Quasi-spherical, Time-dependent Viscous Accretion Flow With High Viscosity Quasi-spherical, Time-dependent Viscous Accretion Flow With High Viscosity

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21822902l&link_type=abstract

American Astronomical Society, AAS Meeting #218, #229.02; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We reported the results of the time-dependent simulations of large amplitude oscillations of advective, viscous, sub-Keplerian disks with a proper trement of angular momentum transfer in one-dimensional, quasi-spherical transonic accretion flow around a non-rotating black hole using the Lagrangian Total Variation Diminising (TVD) and a remap routine.Our code has a shock-capturing capability better than both standard Eulerian code and Lagrangian SPH code. It could well follow the angular momentum transfer of the viscous, subsonic, analytical solution. Hence, we present a simulation of a rotating, viscous, transonic fluid with shocks. Oscillation of the accretion shock was produced due to the different rates of angular momentum transfer across the shock and the heat dissipated due to the presence of high viscosity parameter. Moreover, as the shock drifts to larger distances, a secondary inner shock develops. We showed that the inner shock is the direct consequence of expansion of the outer shock, as well as creation of regions with dl / dr < 0 due to more efficient angular momentum transfer near the inner sonic point. The oscillatory motion of the shock induced oscillation in all the disk parameters such as emission, rate of matter consumed by the black hole, and the rate of angular momentum consumed by the black hole. Our simulation may have implication for low and high frequency QPOs.

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