ON THE ORIGIN OF THE CENTRAL 1″ HOLE IN THE STELLAR DISK OF SGR A* AND THE FERMI GAMMA-RAY BUBBLES

Abstract

The supermassive black hole Sgr A* at the center of the Galaxy is surrounded by two misaligned disks of young, massive stars extending from ~0.04 to 0.4 pc. The stellar surface density increases as ~ r^-2 towards Sgr A* but is truncated within 1" (0.04pc). We explore the origin of this annulus using a model in which star formation occurs in a disk of gas created through the partial capture of a gas cloud as it sweeps through the inner few parsecs of the galaxy and temporarily engulfs Sgr A*. We identify the locations within which star formation and/or accretion onto Sgr A* take place. Within 0.04 pc the disk is magnetically active and the associated heating and enhanced pressure prevents the disk from becoming self gravitating. Instead, it forms a magneto-turbulent disk that drains onto Sgr A* within 3 Myr. Meanwhile, fragmentation of the gas beyond the central 0.04 pc hole creates the observed young stellar disk. The two large scale bubbles of gamma-ray emission extending perpendicular to the Galactic plane may be created by a burst of accretion of ~10^5 Msun of gas lying between 0.01 and 0.03 pc. The observed stellar ages imply that this capture event occurred ~10^6.5 yr ago, thus such events occurring over the life time of the Galaxy could have significantly contributed to the current mass of Sgr A* and to the inner few parsec of the nuclear star cluster. We suggest that these events also occur in extragalactic systems.