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Massive stars in subparsec rings around galactic centres
Article first published online: 7 SEP 2006
DOI: 10.1111/j.1365-2966.2006.10772.x
Issue
Monthly Notices of the Royal Astronomical Society
Volume 372, Issue 1, pages 143–150, October 2006
Additional Information
How to Cite
Nayakshin, S. (2006), Massive stars in subparsec rings around galactic centres. Monthly Notices of the Royal Astronomical Society, 372: 143–150. doi: 10.1111/j.1365-2966.2006.10772.x
Publication History
- Issue published online: 7 SEP 2006
- Article first published online: 7 SEP 2006
- Accepted 2006 July 4. Received 2006 June 23; in original form 2005 December 16
- Abstract
- Article
- References
- Cited By
Keywords:
- accretion, accretion discs;
- stars: formation;
- Galaxy: centre;
- galaxies: active
ABSTRACT
We consider the structure of self-gravitating marginally stable accretion discs in galactic centres in which a small fraction of the disc mass has been converted into protostars. We find that protostars accrete gaseous disc matter at prodigious rates. Mainly due to the stellar accretion luminosity, the disc heats up and thickens geometrically, shutting off further disc fragmentation. The existing protostars, however, continue to gain mass by gas accretion. As a result, the initial mass function for disc-born stars at distances R∼ 0.03–3 pc from the supermassive black hole should be top-heavy. The effect is most pronounced at around R∼ 0.1 pc. We suggest that this result explains observations of rings of young massive stars in our Galaxy and in M31, and we predict that more such rings will be discovered.