Second-generation star formation in globular clusters of different masses
| Autor: | A Yaghoobi, F Calura, J Rosdahl, H Haghi |
|---|---|
| Přispěvatelé: | Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL) |
| Rok vydání: | 2021 |
| Předmět: |
stars: formation
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph] [SDU]Sciences of the Universe [physics] Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) hydrodynamics Globular clusters: general FOS: Physical sciences Astrophysics::Solar and Stellar Astrophysics Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Astrophysics::Galaxy Astrophysics methods: numerical |
| Zdroj: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 2022, 510 (3), pp.4330-4346. ⟨10.1093/mnras/stab3682⟩ Monthly Notices of the Royal Astronomical Society, 2022, 510, pp.4330-4346. ⟨10.1093/mnras/stab3682⟩ |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | By means of three-dimensional hydrodynamical simulations, we investigate the formation of second generation (SG) stars in young globular clusters of different masses. We consider clusters with a first generation of asymptotic giant branch (AGB) stars with mass 10^5 and 10^6 Msun moving at constant velocity through a uniform gas with density 10^(-24) and 10^(-23) g cm^(-3). Our setup is designed to reproduce the encounter of a young cluster with a reservoir of dense gas, e. g. during its orbital motion in the host galaxy. In the low-density models, as a result of the cooling AGB ejecta which collect in the centre, weakly perturbed by the external ram pressure, a compact central He-rich SG stellar component is formed on a timescale which decreases with increasing initial cluster mass. Our high-density models are subject to stronger ram pressure, which prevents the accumulation of the most He-rich AGB ejecta in the cluster centre. As a result, the SG is more extended and less He-enhanced than in the low-density models. By combining our results with previous simulations, we are able to study relevant, cluster-related scaling relations across a dynamical range of two orders of magnitude in mass (from 10^5 Msun to 10^7 Msun). In agreement with current observationally-based estimates, we find positive correlations between the SG-to-total number ratio and maximum He enhancement in SG stars as a function of the initial cluster mass. 18 pages, 8 figures, MNRAS, accepted for publication |
| Databáze: | OpenAIRE |
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