On the influence of the viscosity on the structure of the boundary layer of accretion disks

Details On the influence of the viscosity on the structure of the boundary layer of accretion disks On the influence of the viscosity on the structure of the boundary layer of accretion disks

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...247...95k&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 247, no. 1, July 1991, p. 95-107.

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49

Accretion Disks, Cataclysmic Variables, Stellar Structure, Boundary Layers, Computational Astrophysics, Hydrodynamics, Protostars, Viscosity

Scientific paper

Two-dimensional hydrodynamical calculations are presented of the structure of the boundary layer (BL) in cataclysmic variables using different values for the viscosity and varying some of the system parameters. The results are found to depend strongly on the viscosity magnitude. For high and constant values of the kinematic viscosity, the flow in the BL is smooth and quasi-stationary. In this case the radial infall velocity of the gas near the star is supersonic. If a more realistic description of the turbulent viscosity is used, where the viscosity is proportional to the local sound velocity times the pressure scale height, the flow is strongly time-dependent and unstable. In the case when the flow becomes supersonic, radial shocks are formed so that the flow remains mainly subsonic. The boundary layer luminosity oscillates with an amplitude of about 1.5 mag on timescales of the Keplerian period at the stellar surface. It is suggested that this accounts for some of the variability on short time scales observed in cataclysmic variables.

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