Star Formation History of ω Centauri Imprinted in Elemental Abundance Patterns

Abstract

The star formation history of the globular cluster ω Centauri is investigated in the context of an inhomogeneous chemical evolution model in which supernovae induce star formation. The proposed model explains recent observations for ω Cen stars and divides star formation into three epochs. At the end of the first epoch, ~70% of the gas was expelled by supernovae. Asymptotic giant branch stars then supplied s-process elements to the remaining gas during the first interval of ~300 Myr. This explains the observed sudden increase in Ba/Fe ratios in ω Cen stars at [Fe/H] ~ -1.6. Supernovae at the end of the second epoch were unable to expel the gas. Eventually, Type Ia supernovae initiated supernova-induced star formation, and the remaining gas was stripped when the cluster passed through the newly formed disk of the Milky Way. The formation of ω Cen is also discussed in the framework of globular cluster formation triggered by cloud-cloud collisions. In this scenario, the relative velocity of clouds in the collision determines the later chemical evolution in the clusters. A head-on collision of protocluster clouds with a low relative velocity would have converted less than 1% of the gas into stars and promoted the subsequent chemical evolution by supernova-driven star formation. This is consistent with present observed form of ω Cen. In contrast, the other Galactic globular clusters are expected to have formed from more intense head-on collisions, and the resultant clouds would have been too thin for supernovae to accumulate enough gas to form the next generation of stars. This explains the absence of chemical evolution in these other globular clusters.