Massive stars in sub-parsec rings around galactic centers

Abstract

We consider the structure of self-gravitating marginally stable accretion disks in galactic centers in which a small fraction of the disk mass has been converted into proto-stars. We find that proto-stars accrete gaseous disk matter at prodigious rates. Mainly due to the stellar accretion luminosity, the disk heats up and geometrically thickens, shutting off further disk fragmentation. The existing proto-stars however continue to gain mass by gas accretion. As a results, the initial mass function for disk-born stars at distances R ~ 0.03-3 parsec from the super-massive black hole should be top-heavy. The effect is most pronounced at around R ~ 0.1 parsec. We suggest that this result explains observations of rings of young massive stars in our Galaxy and in M31, and predict that more of such rings will be discovered.

Figure 1 replaced (the one supplied in the previous version was for a different SMBH mass than intended)

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