  The Galactic center provides a unique laboratory to study the interaction of
a supermassive black hole (SMBH) with its gaseous and stellar environment.
Simulations to determine the accretion of stellar winds from the surrounding
O-stars onto the black hole have been performed earlier, but in those the
presence of the S-star system was ignored. The S-stars are a group of young
massive B-stars in relatively close orbits around the black hole. Here we
simulate those stars in order to study their contribution to the accretion
rate, without taking the more distant and massive O-stars into account. We use
the Astrophysical Multi-purpose Software Environment (AMUSE) to combine
gravitational physics, stellar evolution and hydrodynamics in a single
simulation of the S-stars orbiting the supermassive black hole, and use this
framework to determine the amount of gas that is accreted onto the black hole.
We find that the accretion rate is sensitive to the wind properties of the
S-stars (rate of mass-loss and terminal velocity). Our simulations are
consistent with the observed accretion rate of the black hole only if the stars
exhibit high wind massloss rates that are comparable with those of evolved 7-10
Myr old stars with masses of M=19-25 M_SUN. This is in contrast with
observations that have shown that these stars are rather young, main-sequence
B-stars. We therefore conclude that the S-stars cannot account for the
accretion rate alone.
