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 } \leq 750 km s ^ { -1 } ) , 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 .