Hydrodynamical calculations towards steady state structures in boundary layers in accretion disks. 2: 2-D models

Details Hydrodynamical calculations towards steady state structures in boundary layers in accretion disks. 2: 2-D models Hydrodynamical calculations towards steady state structures in boundary layers in accretion disks. 2: 2-D models

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...295..268h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 295, no. 1, p. 268-288

Astronomy and Astrophysics

Astrophysics

14

Accretion Disks, Boundary Layers, Hydrodynamic Equations, Steady State, Two Dimensional Models, White Dwarf Stars, Angular Momentum, Angular Velocity, Navier-Stokes Equation, Time Dependence, Viscosity

Scientific paper

The efficient hydrodynamical solver developed by Hujeirat & Rannacher (1994) is applied to search for steady state solution for the set of time-dependent Navier-Stokes equations describing a 2-D boundary layer around a non-magnetic white dwarf. We present the results of four model calculations carried out on the viscous time scale. The results indicate (1) the accreted matter loses most of its angular momentum via a shock in the boundary layer and forms a dense, quasi-spherical and pressure supported shell in some cases and belts in others, (2) the viscosity in the disk is too large, modifying the viscosity prescription is necessary to prevent dissolution of the disk, (3) formation of circulations is observed in the shock-near regions whenever the angular velocity undergoes strong vertical variations near the equator or in the absence of cooling via thermal diffusion, (4) at least under optically thick conditions, the angular velocity and the temperature achieve a relatively braod maxima in the equatorial region, and (5) to resolve the thermal structure of BL-AD consistently, it is necessary to consider the vertical variation of angular velocity.

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