The role of Type Ia supernova feedback on the second generation formation in globular clusters

Very little is known about the physical processes which determined the end of star formation in globular clusters (GC). By means of 3D hydrodynamic simulations, we study for the first time how the formation and the chemical properties of second generation (SG) stars in a massive proto-GC are affected by SNe Ia explosions belonging to the first stellar generation, one likely cause for the quenching of star formation in these systems. In our model, the formation of SG stars starts ∼ 40 Myr after the cluster birth and is due to the retention of the fresh ejecta of first generation asymptotic giant branch stars plus accretion of cold, pristine gas. At the same time, SNe Ia start exploding, carving hot and tenuous bubbles in the interstellar medium. I have focused on SNe Ia effects on the iron and helium abundances and studied the role of various parameters in regulating the efficiency of SN Ia feedback. According to our results, SN explosions are able to halt star formation only if the pristine gas is tenuous (with density ∼ 1cm^-3), whereas they have little effects if the pristine gas density is ∼ 10 cm^-3. Finally, we show that gas from SNe Ia may produce an iron spread as found in Type II GCs, an anomalous sub-category of GCs.