Globular clusters (GCs), once thought to be well approximated as simplestellar populations (i.e. all stars having the same age and chemicalabundance), are now known to host a variety of anomalies, such as multiplediscrete (or spreads in) populations in colour-magnitude diagrams and abundancevariations in light elements (e.g., Na, O, Al). Multiple models have been putforward to explain the observed anomalies, although all have seriousshortcomings (e.g., requiring a non-standard initial mass function of stars andGCs to have been initially 10-100 times more massive than observed today).These models also do not agree with observations of massive stellar clustersforming today, which do not display significant age spreads nor have gas/dustwithin the cluster. Here we present a model for the formation of GCs, where lowmass pre-main sequence (PMS) stars accrete enriched material released frominteracting massive binary and rapidly rotating stars onto their circumstellardiscs, and ultimately onto the young stars. As was shown in previous studies,the accreted material matches the unusual abundances and patterns observed inGCs. The proposed model does not require multiple generations ofstar-formation, conforms to known properties of massive clusters forming today,and solves the "mass budget problem" without requiring GCs to have beensignificantly more massive at birth. Potential caveats to the model as well asmodel predictions are discussed.
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