Wind accretion in binary stars - I. Mass accretion ratio

Details Wind accretion in binary stars - I. Mass accretion ratio Wind accretion in binary stars - I. Mass accretion ratio

2004-03-15

arxiv.org/abs/astro-ph/0403329v1

Astron.Astrophys. 419 (2004) 335-343

Astronomy and Astrophysics

Astrophysics

8 pages, accepted for publication in Astronomy and Astrophysics

Scientific paper

10.1051/0004-6361:20040070

Three-dimensional hydrodynamic calculations are performed in order to investigate mass transfer in a close binary system, in which one component undergoes mass loss through a wind. The mass ratio is assumed to be unity. The radius of the mass-losing star is taken to be about a quarter of the separation between the two stars. Calculations are performed for gases with a ratio of specific heats gamma=1.01 and 5/3. Mass loss is assumed to be thermally driven so that the other parameter is the sound speed of the gas on the mass-losing star. Here, we focus our attention on two features: flow patterns and mass accretion ratio, which we define as the ratio of the mass accretion rate onto the companion to the mass loss rate from the mass-losing primary star. We characterize the flow by the mean normal velocity of wind on the critical Roche surface of the mass-losing star, Vr. When Vr<0.4 A Omega, where A and Omega are the separation between the two stars and the angular orbital frequency of the binary, respectively, we obtain Roche-lobe over-flow (RLOF), while for Vr>0.7 A Omega we observe wind accretion. We find very complex flow patterns in between these two extreme cases. We derive an empirical formula of the mass accretion ratio in the low and in the high velocity regime.

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