Thermal conduction and selfsimilar accretion flows
Abstract
Generalizing Gilham's (1981) weakly viscous model to include a weak shear viscosity and a simple thermal conduction law, it is shown that a series of selfsimilar rotating accretion flows can be constructed. Solutions with both inflow and outflow along the polar axis are easily generated, forming a continuous sequence linking Gilham's models to a family of nonrotating spherical infall models. No physically acceptable disklike solutions are found to exist corresponding to these quasispherical solutions. The solutions with thermal conduction remain subject to the convective instability at moderate to high latitudes that besets both Gilham's models and Begelman and Meier's (1982) disks.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 August 1987
 DOI:
 10.1093/mnras/227.3.623
 Bibcode:
 1987MNRAS.227..623A
 Keywords:

 Accretion Disks;
 Computational Astrophysics;
 Rotating Fluids;
 Thermal Conductivity;
 Flow Stability;
 NavierStokes Equation;
 Viscosity;
 Astrophysics