The evolution of the stellar mass function in star clusters

TL;DR

This paper presents a simple, physically motivated model for the evolution of the stellar mass function in star clusters, accounting for various dynamical processes and initial conditions, and validated against N-body simulations.

Contribution

It introduces a versatile, parameter-independent model for stellar mass function evolution that includes stellar evolution, remnants, and dynamical effects, applicable across diverse cluster conditions.

Findings

Low-mass stars are ejected after ~400 Myr.

Mass function depletion depends on disruption time and remnant retention.

Model aligns with N-body simulations under similar conditions.

Abstract

(Abridged) The dynamical ejection of stars from star clusters affects the shape of the stellar mass function (MF) in these clusters, because the escape probability of a star depends on its mass. The objective of this paper is to provide and to apply a simple physical model for the evolution of the MF in star clusters for a large range of the parameter space. The model is derived from the basic principles of two-body encounters and energy considerations. It is independent of the adopted mass loss rate or initial mass function (IMF), and contains stellar evolution, stellar remnant retention, dynamical dissolution in a tidal field, and mass segregation. It is found that the MF evolution in star clusters depends on the disruption time, remnant retention fraction, initial-final stellar mass relation, and IMF. Low-mass stars are preferentially ejected after t~400 Myr. Before that time, masses around 15-20% of the maximum stellar mass are lost. The degree of low-mass star depletion grows for increasing disruption times, but can be quenched when the retained fraction of massive remnants is large. The highly depleted MFs of certain Galactic globular clusters are explained by the enhanced low-mass star depletion that occurs for low remnant retention fractions. Unless the retention fraction is exceptionally large, dynamical evolution always decreases the mass-to-light ratio. The modeled evolution of the MF is consistent with N-body simulations when adopting identical boundary conditions. However, it is found that the results from N-body simulations only hold for their specific boundary conditions and should not be generalised to all clusters. It is concluded that the model provides an efficient method do understand the evolution of the stellar MF in star clusters under widely varying conditions.