Pre-main sequence accretion and the formation of multiple populations in Globular Clusters

TL;DR

This study examines a model where gas accretion onto low-mass stars explains chemical anomalies in globular clusters, highlighting the timing constraints and implications for initial cluster mass.

Contribution

It demonstrates that accretion timing and stellar mixing processes critically influence chemical signatures, challenging previous models requiring large initial cluster masses.

Findings

Accretion must occur within 2-3 million years to produce observed helium variations.

Lithium abundances can vary greatly depending on accreted mass and timing.

Short accretion phases imply very large initial cluster masses are necessary.

Abstract

We investigate the viability of a model in which the chemical anomalies among Globular Cluster stars are due to accretion of gas onto the protostellar discs of low mass stars. This model has been suggested as a way to reduce the large initial cluster masses required by other models for the formation of multiple stellar generations. We numerically follow the evolution of the accreting stars, and we show that the structure of the seed star does not remain fully convective for the whole duration of the accretion phase. Stellar populations showing discrete abundances of helium in the core, that seem to be present in some clusters, might be formed with this mechanism only if accretion occurs before the core of the stars become radiative (within 2-3Myr) or if a thermohaline instability is triggered, to achieve full mixing after the accretion phase ends. We also show that the lithium abundances in accreted structures may vary by orders of magnitude in equal masses obtained by accreting different masses. In addition, the same thermohaline mixing which could provide a homogeneous helium distribution down to the stellar center, would destroy any lithium surviving in the envelope, so that both helium homogeneity and lithium survival require that the accretion phase be limited to the first couple of million years of the cluster evolution. Such a short accretion phase strongly reduces the amount of processed matter available, and reintroduces the requirement of an extremely large initial mass for the protocluster.