In situ formation of the massive stars around SgrA*

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dc.creatorMapelli, M.
dc.creatorHayfield, T.
dc.creatorMayer, L.
dc.creatorWadsley, J.
dc.date2008-05-02
dc.date.accessioned2026-07-07T09:36:38Z
dc.date.available2026-07-07T09:36:38Z
dc.descriptionThe formation of the massive young stars surrounding SgrA* is still an open question. In this paper, we simulate the infall of an isothermal, turbulent molecular cloud towards the Galactic Centre (GC). As it spirals towards the GC, the molecular cloud forms a small and dense disc around SgrA*. Efficient star formation (SF) is expected to take place in such a dense disc. We model SF by means of sink particles. At ~6x10^5 yr, ~6000 solar masses of stars have formed, and are confined within a thin disc with inner and outer radius of 0.06 and 0.5 pc, respectively. Thus, this preliminary study shows that the infall of a molecular cloud is a viable scenario for the formation of massive stars around SgrA*. Further studies with more realistic radiation physics and SF will be required to better constrain this intriguing scenario.
dc.description6 pages, 4 figures, resubmitted to MNRAS Letters after addressing referee report
dc.identifierhttps://arxiv.org/abs/0805.0185
dc.identifierhttp://arxiv.org/abs/0805.0185
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/160186
dc.subjectAstrophysics
dc.titleIn situ formation of the massive stars around SgrA*
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