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A 3-D hydrodynamical simulation of wind accretion

Published online by Cambridge University Press:  07 August 2017

Henri M.J. Boffin
Henri M.J. Boffin*
Affiliation:
Institut d'Astronomie et d'Astrophysique C.P. 165, Université Libre de Bruxelles 50, av. F.D. Roosevelt B-1050 BRUSSELS

Abstract

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Using a 3-dimensional hydrodynamical code, based on the Smooth Particle Hydrodynamics (SPH) method, we have simulated the case of wind accretion. Several configurations were studied:

  • - homogeneous mass flow

  • - wind with a density gradient

  • - wind with a velocity gradient

In each case, the accretion rate as well as the accreted angular momentum has been calculated. Comparisons were done with other simulations published in the literature and especially with the two currently existing 3-D simulations. According to one of these group (Matsuda et al., 1990) resolution is very critical in determining the accretion rate as well as to determine if the flow is stationary or not. We have done simulation at various resolutions and we confirm its importance for the deduced accretion rate. However, our simulations do not seem to show any non- stationary behaviour.

Type
Oral and Contributed Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 453 - 456
Copyright
Copyright © Kluwer 1992 

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