On dynamics of nonmagnetic accretion disks

Abstract

Axisymmetric accretion disks in vicinity of a central compact body are studied. In the case of non-viscous disk it is proven that all solutions for the midplane circular velocity are unstable. Hence, the pure hydrodynamic turbulence in accretion disks is possible. It is disproved the well-known arguments that an inviscid accretion disk must be sub-Keplerian. It is also demonstrated that the regular asymptotic solutions, often used in astrophysics, can lead to erroneous conclusions. It is proven that a laminar viscous disk can be approximated with a great precision by the vortex motion. Assuming that a turbulent gas tends to flow with minimal losses, we have shown that a turbulent disk tends to be Keplerian.

38 pages

References in corpus (7)

• The turbulent destruction of clouds - I. A k-epsilon treatment of turbulence in 2D models of adiabatic shock-cloud interactions
• On the possible turbulence mechanism in accretion disks in non-magnetic binary stars
• A study of transient dynamics of perturbations in Keplerian discs using a variational approach
• A viscous instability in axially symmetric laminar shear flows
• Perturbations dynamics in Keplerian flow under external stochastic forcing
• Hydrodynamical activity in thin accretion disks
• Accretion disks around black holes with account of magnetic fields