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 _ { \odot } . 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 can not account for the accretion rate alone .