Multiple stellar populations in MOCCA globular cluster models: Transient spatial over-concentration of pristine red giant stars driven by strong dynamical encounters

TL;DR

This study uses MOCCA globular cluster models to show that dynamical encounters can transiently cause pristine first-generation red giant stars to appear more centrally concentrated than enriched second-generation stars, challenging traditional formation scenarios.

Contribution

The paper demonstrates that dynamical interactions can temporarily invert the expected spatial distribution of multiple stellar populations in globular clusters, explaining some observed anomalies.

Findings

Dynamical encounters eject 2P RGB progenitors from cluster centers.

Transient over-concentration of 1P stars can occur in evolved clusters.

MOCCA models can explain observed features in specific Galactic GCs.

Abstract

Recent findings show that, in some Milky Way globular clusters (GCs), pristine red giant branch (RGB) stars are more centrally concentrated than enriched RGB stars. This contradicts most multiple-population formation scenarios, which predict that the enriched population 2p should initially be more concentrated than the pristine population 1P. We analyze a MOCCA GC model that exhibits a higher spatial concentration of 1P RGB stars than 2P RGB stars at 13 Gyr. The MOCCA models assume the asymptotic giant branch (AGB) pollution scenario, where 2P stars are initially more concentrated than 1P stars. Our results indicate that the observed spatial distributions of multiple populations, and possibly their kinematics, are significantly shaped by dynamical interactions. These interactions preferentially eject 2P RGB progenitors from the central regions, leading to a transient over-concentration of 1P RGB stars at late times. This effect is particularly relevant for GCs with present-day of a few $10^5 M_{\odot}$, which have retained only about 10 - 20 percent of their initial mass. Such clusters may appear dynamically young due to heating from a black hole subsystem, even if they have undergone significant mass loss and dynamical evolution. Additionally, the relatively small number of RGB stars in these clusters suggests that interpreting the spatial distributions of multiple populations solely from RGB stars may lead to biased conclusions about the overall distribution of 2P and 1P. The apparent over-concentration of the 1P relative to the 2P is likely a transient effect driven by the preferential removal of 2P RGB progenitors via strong dynamical encounters. MOCCA models of multiple stellar populations based on the AGB scenario may explain anomalous features observed in some Galactic GCs, such as NGC 3201 and NGC 6101.