  We present numerical simulations of stellar wind dynamics in the central
parsec of the Galactic centre, studying in particular the accretion of gas on
to Sgr A*, the super-massive black hole. Unlike our previous work, here we use
state-of-the-art observational data on orbits and wind properties of individual
wind-producing stars. Since wind velocities were revised upwards and non-zero
eccentricities were considered, our new simulations show fewer clumps of cold
gas and no conspicuous disc-like structure. The accretion rate is dominated by
a few close `slow wind stars' v_w < 750 km/s, and is consistent with the Bondi
estimate, but variable on time-scales of tens to hundreds of years. This
variability is due to the stochastic in-fall of cold clumps of gas, as in
earlier simulations, and to the eccentric orbits of stars. The present models
fail to explain the high luminosity of Sgr A* a few hundred years ago implied
by Integral observations, but we argue that the accretion of a cold clump with
a small impact parameter could have caused it. Finally, we show the possibility
of constraining the total mass-loss rate of the `slow wind stars' using near
infra-red observations of gas in the central few arcseconds.
