Effects of Type Ia Supernova feedback in young globular clusters

Through 3D hydrodynamical simulations, we explore the impact of Type Ia supernovae (SNe) explosions on the star formation history and chemical properties of second-generation stars in young globular clusters of different masses. Considering clusters with a first generation of asymptotic giant branch (AGB) stars at masses of 10^5 and 10^6 solar masses, moving at a constant velocity through a uniform gas with densities of 10^(−24) and 10^(−23) g/cm^3, second-generation (SG) stars form as the first-generation AGB stars release their ejecta. During this phase, external gas accretion occurs, and SNe Ia explosions begins, carving hot and tenuous bubbles. Three simulated models are analyzed: in the low mass and low density scenario, we observe hiatuses in star formation, with the second generation dominated by a He-rich (Y>0.33) and metal-poor ([Fe/H]<-1.5) population, depicting a scenario highly affected by Type Ia SN feedback without retaining ejecta. In the high mass and low density scenario, continuous star formation is observed, with dominance of He-rich and metal-poor populations similar to the lower mass model. In the high mass and high density scenario, which exhibits the highest star formation rate, the majority of stars form from a mix of AGB ejecta and pristine gas, showing modest helium enrichment. Each model shows a lower SG final mass compared to the corresponding models without SNeIa.