Second-generation star formation in globular clusters of different masses. Issue 3 (22nd December 2021)

• Record Type: Journal Article
• Authors: Yaghoobi, A; Calura, F; Rosdahl, J; Haghi, H
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 510:Issue 3(2022)
• Page Start: 4330
• Page End: 4346
• Publication Date: 2021-12-22
• Subjects: hydrodynamics -- methods: numerical -- stars: formation -- Globular clusters: general; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab3682
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: 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 $10^6\, \mathrm{M}_{\odot }$ moving at constant velocity through a uniform gas with density 10 −24 and 10 −23 g cm −3 . Our set-up 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 time-scale 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 $ to $10^7 \, \mathrm{M}_{\odot }$ ). 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.