SCYON Abstract

Received on: 18 10 2022

Ionising Feedback Effects on Star Formation in Globular Clusters with Multiple Stellar Populations

Authors:A. Yaghoobi 1,2,3, J. Rosdahl 2, F. Calura 4, P. Khalaj 1, H. Haghi 1
Affiliations:(1) Department of Physics, Institute for Advanced Studies in Basic Sciences (IASBS), Zanjan, Iran; (2) Univ Lyon, Univ Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon, Saint-Genis-Laval, France; (3) Department of Physics, Faculty of Sciences, Ferdowsi University of Mashhad, Mashhad, Iran; (4) INAF - OAS, Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Bologna, Italy
Accepted by: Monthly Notices of the Royal Astronomical Society
URL:https://ui.adsabs.harvard.edu/abs/2022arXiv221001136Y/abstract

Using 3D radiation-hydrodynamical simulations, we study the effects of ionising radiation on the formation of second-generation (SG) stars in Globular Clusters (GCs) with multiple stellar populations. In particular, we focus on massive ($10^7 \mathrm{M}_{\odot}$) and young (40-Myr old) GCs. We consider stellar winds from asymptotic giant branch (AGB) stars, ram pressure, gas accretion onto the cluster, and photoionisation feedback of binary stars. We find that the stellar luminosity is strong enough to warm and ionise the intracluster medium, but it does not lead to a significant gas expulsion. The cluster can thus retain the ejecta of AGB stars and the accreted pristine gas. In addition, efficient cooling occurs in the central region of the cluster within $50 \mathrm{Myr}$ from the formation of first generation stars, leading to the formation of SG stars. Our results indicate that the inclusion of photoionisation does not suppress SG formation, but rather delays it by about $\sim10 \mathrm{Myr}$. The time delay depends on the density of the pristine gas, so that a denser medium exhibits a shorter delay in star formation. Moreover, photoionisation leads to a modest decrease in the total SG mass, compared to a model without it.


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