WIND ACCRETION IN BINARY STARS .2. ACCRETION RATES

Citation
T. Theuns et al., WIND ACCRETION IN BINARY STARS .2. ACCRETION RATES, Monthly Notices of the Royal Astronomical Society, 280(4), 1996, pp. 1264-1276
Citations number
46
Categorie Soggetti
Astronomy & Astrophysics
ISSN journal
00358711
Volume
280
Issue
4
Year of publication
1996
Pages
1264 - 1276
Database
ISI
SICI code
0035-8711(1996)280:4<1264:WAIBS.>2.0.ZU;2-L
Abstract
Smoothed particle hydrodynamics (SPH) is used to estimate accretion ra tes of mass, linear and angular momentum in a binary system where one component undergoes mass loss through a wind. Physical parameters are chosen such as to model the alleged binary precursors of barium stars, whose chemical peculiarities are believed to result from the accretio n of the wind from a companion that was formerly on the asymptotic gia nt branch (AGB). The binary system modelled consists of a 3-M(.) AGB s tar (losing mass at a rate 10(-6) M(.) yr(-1)) and a 1.5-M(.) star on the main sequence, in a 3-au circular orbit. Three-dimensional simulat ions are performed for gases with polytropic indices gamma=1, 1.1 and 1.5, to bracket more realistic situations that would include radiative cooling. Mass accretion rates are found to; depend on resolution, and we estimate typical values of 1-2 per cent for the gamma=1.5 case and 8 per cent for the other models. The highest resolution obtained (wit h 400 000 particles) corresponds to an accretor of linear size approxi mate to 16 R(.). Despite being (in the gamma = 1.5 case) about 10 time s smaller than theoretical estimates based on the Bondi-Hoyle prescrip tion, the SPM accretion rates remain large enough to explain the pollu tion of barium stars. Uncertainties in the current SPH rates remain, h owever, owing to the simplified treatment of the wind acceleration mec hanism, as well as to the absence of any cooling prescription and to t he limited numerical resolution. Angular momentum transfer leads to si gnificant spin-up of the accretor and can account for the rapid rotati on of HD 165141, a barium star with a young white dwarf companion and a rotation rate unusually large among K giants. In the circular orbit modelled in this paper, hydrodynamic thrust and gravitational drag alm ost exactly compensate and so the net transfer of linear momentum is n early zero. For small but finite eccentricities and the chosen set of parameters, the eccentricity tends to decrease.