Thermal conduction and self-similar accretion flows

Details Thermal conduction and self-similar accretion flows Thermal conduction and self-similar accretion flows

Aug 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.227..623a&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 227, Aug. 1, 1987, p. 623-638.

Statistics

Computation

3

Accretion Disks, Computational Astrophysics, Rotating Fluids, Thermal Conductivity, Flow Stability, Navier-Stokes Equation, Viscosity

Scientific paper

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 self-similar 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 quasi-spherical 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.

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