Rebounding Cores to Build Star Cluster Multiple Populations

TL;DR

This paper introduces a new model explaining multiple stellar populations in star clusters by considering the role of 'failed' molecular cores that re-expand and influence star formation rates, with implications for globular cluster diversity.

Contribution

The model links failed core dynamics to star formation histories and globular cluster properties, offering a novel explanation for observed stellar population variations.

Findings

Failed cores regulate gas density and star formation rates.

Star formation histories depend on core formation efficiencies and failed core return times.

Model constrains progenitor properties of the Orion Nebula Cluster.

Abstract

We present a novel approach to the riddle of star cluster multiple populations. Stars form from molecular cores. But not all cores form stars. Following their initial compression, such 'failed' cores re-expand, rather than collapsing. We propose that their formation and subsequent dispersal regulate the gas density of cluster-forming clumps and, therefore, their core and star formation rates. Clumps for which failed cores are the dominant core type experience star formation histories with peaks and troughs. In contrast, too few failed cores results in smoothly decreasing star formation rates. We identify three main parameters shaping the star formation history of a clump: the star and core formation efficiencies per free-fall time, and the time-scale on which failed cores return to the clump gas. The clump mass acts as a scaling factor. We use our model to constrain the density and mass of the Orion Nebula Cluster progenitor clump, and to caution that the star formation histories of starburst clusters may contain close-by peaks concealed by stellar age uncertainties. Our model generates a great variety of star formation histories. Intriguingly, the chromosome maps and O-Na anti-correlations of old globular clusters also present diverse morphologies. This prompts us to discuss our model in the context of globular cluster multiple stellar populations. More massive globular clusters exhibit stronger multiple stellar population patterns, which our model can explain if the formation of the polluting stars requires a given stellar mass threshold.