Standing shocks in isothermal rotating winds and accretion. II - Effects of viscous dissipation

Details Standing shocks in isothermal rotating winds and accretion. II - Effects of viscous dissipation Standing shocks in isothermal rotating winds and accretion. II - Effects of viscous dissipation

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.243..610c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 243, April 15, 1990, p. 610-619.

Statistics

Computation

38

Astrophysics, Isothermal Flow, Rotating Fluids, Shock Waves, Standing Waves, Viscous Flow, Angular Momentum, Black Holes (Astronomy), Computational Astrophysics, Energy Dissipation, Stellar Winds

Scientific paper

Previous work on the standing shock formation is extended to include the effects of the viscous dissipation in the rotating flows. In this case neither the angular momentum nor the energy of the flow remains conserved. In the nondissipative flow, for a given set of the initial parameters, there are two final locations where a shock could form in a black hole accretion. Shocks at these locations are otherwise identical. This ambiguity is removed in the presence of dissipation. This is shown using both the Shakura-Suniaev viscosity and an effective turbulent viscosity. In the presence of a small dissipation, the shocks no longer remain identical; they dissipate different amounts of energy, and they also vary in strength. Furthermore, when the dissipation is larger, one of the shocks disappears completely. A unique description of the thin rotating isothermal flow around compact objects with or without shocks is obtained.

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