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Numerical Calculations for Accretion Disks in Close Binary Systems

Published online by Cambridge University Press:  12 April 2016

G. Hensler
G. Hensler*
Affiliation:
Universitäts-Sternwarte, Geismarlandstr. 11, D-3400 Göttingen

Abstract

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A numerical method for 3D magnetohydrodynamical investigations of accretion disks in close binary systems is presented, which allows for good spatial resolution of structures (hot spot, accretion column). The gas is treated as individual gas cells (pseudo-particles) whose motion is calculated within a grid consisting of one spherical inner part for 3D MHD and two plane outer parts. Viscous interactions of the gas cells are taken into account by a special treatment connected with the grid geometry.

We present one result of 2D hydrodynamical calculations for a binary applying the following parameters which are representative for Cataclysmic Variables: M1 = 1 Mʘ, r1 = 10-2 Rʘ, M2 = 0.5 Mʘ, p = 0.2 d, M = 10-9 Mʘ y-1.

Column density and radiative flux distributions over the disk are shown and briefly discussed by comparison with the theoretical understanding of these Dwarf Novae drawn from observations.

Type
Part III: Evolutionary Processes in Close Binary Systems
Information
International Astronomical Union Colloquium , Volume 69: Binary and Multiple Stars as Tracers of Stellar Evolution , 1982 , pp. 219 - 230
Copyright
Copyright © Reidel 1982

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