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.