Binary Star Disruption in Globular Clusters with Multiple Stellar Populations

TL;DR

This study investigates how the presence of a centrally concentrated second-generation stellar subsystem in globular clusters increases the disruption rate of binary stars, leading to fewer binaries in the second-generation population.

Contribution

It quantifies the enhanced binary disruption rate caused by the inner second-generation subsystem in globular clusters, highlighting its impact on binary fractions.

Findings

SG binaries are disrupted more rapidly than FG binaries.

The SG population ends up with a significantly lower binary fraction.

Structural properties of multiple populations influence binary star survival.

Abstract

The discovery of multiple stellar populations in globular clusters raises fundamental questions concerning the formation and dynamical history of these systems. In a previous study aimed at exploring the formation of second-generation (SG) stars from the ejecta of first-generation (FG) AGB stars, and the subsequent dynamical evolution of the cluster, we showed that SG stars are expected to form in a dense subsystem concentrated in the inner regions of the FG cluster. In this paper we explore the implications of the structural properties of multiple-population clusters, and in particular the presence of the inner SG subsystem, for the disruption of binary stars. We quantify the enhancement of the binary disruption rate due to the presence of the central SG subsystem for a number of different initial conditions. Our calculations show that SG binaries, which are assumed to be more concentrated in the cluster inner regions, are disrupted at a substantially larger rate than FG binaries. Assuming a similar initial fraction of FG and SG binaries, our dynamical study indicates that the SG population is now expected to contain a significantly smaller binary fraction than the FG population.