  Binary stars often move through an ambient medium from which they accrete
material and angular momentum, as in triple-star systems, star-forming clouds,
young globular clusters and in the centres of galaxies. A binary form of
Bondi-Hoyle-Lyttleton accretion results whereby the accretion rate depends on
the binary properties: the stellar masses and separation, and the relative wind
speed. We present the results of simulations performed with the hydrodynamic
code GANDALF, to determine the mass accretion rates over a range of binary
separations, inclinations and mass ratios. When the binary separation is short,
the binary system accretes like a single star, while accretion onto stars in
wide binaries is barely affected by their companion. We investigate
intermediate-separation systems in some detail, finding that as the binary
separation is increased, accretion rates smoothly decrease from the rate equal
to that of a single star to the rate expected from two isolated stars. The form
of this decrease depends on the relative centre-of-mass velocity of the binary
and the gas, with faster-moving binaries showing a shallower decrease.
Accretion rates vary little with orbital inclination, except when the orbit is
side-on and the stars pass through each others' wakes. The specific angular
momentum accretion rate also depends on the inclination but is never sufficient
to prevent the binary orbit from contracting. Our results may be applied to
accretion onto protostars, pollution of stars in globular and nuclear clusters,
and wind mass-transfer in multiple stellar systems.
