Abstrakt
The central supermassive black hole of the Milky Way, Sgr A*, accretes at a very low rate making it a very underluminous galactic nucleus. Despite the tens of Wolf-Rayet stars present within the inner parsec supplying TILDE OPERATOR+D9110^-3 M_e yr^-1 in stellar winds, only a negligible fraction of this material (3000 yr) the material accumulates close to the black hole in the form of a disk.
Considering the duration of the Wolf-Rayet phase (TILDE OPERATOR+D91105 yr), we conclude that this scenario has likely already happened, and could be responsible for the more active past of Sgr A*, and/or its current outflow. We argue that the hypothesis of the mass-losing stars being the main regulator of the activity of the black hole deserves further consideration.