Numerical simulation of the formation of shock waves in thin accretion disks and the resulting angular momentum transport

Details Numerical simulation of the formation of shock waves in thin accretion disks and the resulting angular momentum transport Numerical simulation of the formation of shock waves in thin accretion disks and the resulting angular momentum transport

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...218..102k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 218, no. 1-2, July 1989, p. 102-110.

Astronomy and Astrophysics

Astrophysics

15

Accretion Disks, Angular Momentum, Astronomical Models, Shock Wave Propagation, Active Galactic Nuclei, Binary Stars, Corotation, Quasars, Simulation

Scientific paper

Two-dimensional numerical simulations of the formation and propagation of shocks inside a Keplerian disk and their effects on the transport of angular momentum have been performed in order to explore dissipation in shock waves as a possible mechanism for the apparent high viscosity in thin accretion disks. It is found that nonaxisymmetric perturbations produce spiral shaped waves inside the disk, and that the radial behavior of the wave amplitudes can be determined by the position of the corotation radius and the dissipation. Waves moving away from the corotation radius show a strong steepening, along with the formation of shock fronts. Perturbations from the outside are shown to be more efficient for the formation of shock waves in a disk than disturbances initiated from the inside.

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