Gravothermal oscillations in two-component models of star clusters

TL;DR

This study investigates gravothermal oscillations in two-component star clusters, analyzing their behavior, critical conditions, and validating findings with N-body simulations, highlighting the role of mass segregation and core re-collapse dynamics.

Contribution

It introduces a detailed analysis of gravothermal oscillations in two-component clusters, emphasizing the influence of mass ratios and validating gas model results with N-body simulations.

Findings

Oscillations depend on stellar mass ratios and total component mass ratios.

Re-collapse begins at larger radii during core expansion, halting oscillations.

N-body simulations confirm the gravothermal nature and temperature inversion of oscillations.

Abstract

In this paper, gravothermal oscillations are investigated in two-component clusters with a range of different stellar mass ratios and total component mass ratios. The critical number of stars at which gravothermal oscillations first appeared is found using a gas code. The nature of the oscillations is investigated and it is shown that the oscillations can be understood by focusing on the behaviour of the heavier component, because of mass segregation. It is argued that, during each oscillation, the re-collapse of the cluster begins at larger radii while the core is still expanding. This re-collapse can halt and reverse a gravothermally driven expansion. This material outside the core contracts because it is losing energy both to the cool expanding core and to the material at larger radii. The core collapse times for each model are also found and discussed. For an appropriately chosen case, direct N -body runs were carried out, in order to check the results obtained from the gas model, including evidence of the gravothermal nature of the oscillations and the temperature inversion that drives the expansion.