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Title: Star formation in the GC: observational constraints and theory
Authors: Nayakshin, Sergei
First Published: 1-Jan-2006
Presented at: Galactic Center Workshop From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei, Bad Honnef, GERMANY
Start Date: 18-Apr-2006
End Date: 22-Apr-2006
Publisher: IOP Publishing
Citation: Galactic Center Workshop 2006: From the Center of the Milky Way to Nearby Low-Luminosity Galactic Nuclei, 2006, 54, pp. 208-216 (9)
Abstract: We review some observational aspects and theoretical models for the formation of the young massive stars in the central parsec of our Galaxy. It is concluded that an in-situ star formation model provides the best description of the data. One possible guess for the initial gas confguration is one circular and another eccentric gas discs, not necessarily coeval during their short lifetimes. The circular disc probably resulted from a mass deposition event long compared with the local orbital time, whereas the eccentric disc should have formed more dynamically. Based on X-ray observations of the GC, we argue that the initial mass function (IMF) of stars formed in these discs is top-heavy. Such top-heavy IMF is most likely a result of inefficiency with which these optically thick discs fragment, and thus may be a generic result for star-forming AGN discs. We also present preliminary results of numerical simulations of star forming discs, showing that stars with a top-heavy IMF can be formed in both circular and eccentric discs. However, the inner arcsecond ''S-stars'', and the massive star cluster IRS13E, do not naturally form in these star-forming discs, and still lack explanation.
DOI Link: 10.1088/1742-6596/54/1/034
ISSN: 1742-6588
eISSN: 1742-6596
Version: Publisher Version
Status: Peer-reviewed
Type: Conference Paper
Rights: Archived with reference to SHERPA/RoMEO and publisher website. Creative Commons Attribution License 3.0
Appears in Collections:Conference Papers & Presentations, Dept. of Physics and Astronomy

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