Type Ia supernova feedback effects on globular clusters of different masses

Through 3D hydrodynamical simulations, we explore the impact of Type Ia supernova (SN) explosions on the star formation history and chemical properties of second-generation (SG) stars in young globular clusters with masses of 10^5-10^6 We assume that the SG is formed out of the asymptotic giant branch (AGB) ejecta of first-generation stars plus pristine interstellar medium gas which is modelled as a uniform gas moving at a constant velocity towards the cluster. We tested two values for the infalling gas density of 10^-24 and 10^ -23 Type Ia SNe start to explode together with the release of gas from the most massive AGB stars. Three simulated models are analysed. In the low-mass and low-density scenario, we find SNe Ia quench star formation that however restarts when the gas cools down again in between two explosions. The SG stars are dominated by a He-rich population (Y>0.33), which is poorly diluted by pristine gas. In the high-mass models, star formation is mildly affected, while the He composition is significantly altered as exploding SNe prevent the accretion of pristine gas, and therefore extremely helium-rich stars form. In the high-density model, such weak gas accretion leads to a maximum enhancement in the helium mass fraction that is much larger than the observed one and that does not correlate with the initial cluster mass as is found in models without Type Ia SNe. As for the iron content, small spreads have been found in all models, but the SG is less homogeneous than the FG, at variance with current observations.