Hydrodynamical calculations of accretion disks in close binary systems. I - Method. II - Models

Details Hydrodynamical calculations of accretion disks in close binary systems. I - Method. II - Models Hydrodynamical calculations of accretion disks in close binary systems. I - Method. II - Models

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...114..309h&link_type=abstract

Astronomy and Astrophysics, vol. 114, no. 2, Oct. 1982, p. 309-327.

Astronomy and Astrophysics

Astrophysics

24

Accretion Disks, Binary Stars, Hydrodynamics, Stellar Mass Accretion, Stellar Models, Angular Momentum, Energy Dissipation, Gas Flow, Gas Pressure, Laminar Flow, Mass Transfer, Particle Trajectories, Pressure Gradients, Radiative Transfer, Spatial Resolution, Stellar Structure, Viscosity

Scientific paper

The present investigation is concerned with a pseudoparticle method which represents an extension of the numerical method reported by Lin and Pringle (1976). Differences between the method discussed in the investigation and similar previously developed procedures are related to the consideration of a pressure gradient, the treatment of the viscosity, and the additional consideration of a horizontal energy transport, which is important in the innermost disk region. The basic equations are considered, taking into account the momentum equation, the energy equation, and the viscosity. In connection with the calculations, the gas is divided into individual particles. Two different approaches are employed in the calculations. The particle variables are calculated by making use of the Lagrangian formalism, while the fluid variables are computed locally in a grid. The particle variables include location, velocity, internal energy, and radiation. Fluid variables are density pressure, pressure gradient, viscosity, and heat transport.

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