Growth and Evolution of Thermal Instabilities in Idealized Galaxy-Cluster Cores

TL;DR

This study uses hydrodynamic simulations to explore how thermal instabilities and condensation in galaxy-cluster cores depend on cooling and freefall times, revealing conditions for instability growth and feedback mechanisms.

Contribution

It demonstrates that the ratio of cooling to freefall time governs thermal instability growth and shows geometry has minimal impact on stability in galaxy-cluster cores.

Findings

Instability occurs if tcool /tff < 10 within relevant timescales.

Condensation begins when low-entropy perturbations have tcool /tff < 3.

A feedback efficiency of ~10^-3 maintains thermal balance.

Abstract

Heat input roughly balances radiative cooling in the gaseous cores of galaxy clusters even when the central cooling time is short, implying that cooling triggers a feedback loop that maintains thermal balance. Furthermore, cores with short cooling times tend to have multiphase structure, suggesting that the intracluster medium (ICM) becomes locally thermally unstable for cooling times < 1 Gyr. In this work, we use 2D and 3D hydrodynamic simulations to study the onset of condensation in idealized galaxy-cluster cores. In particular, we look at how the condensation process depends on the ratio of cooling time to freefall time and on the geometry of the gravitational potential. We conclude that the ICM can always evolve to a state in which condensation occurs if given enough time, but that an initial timescale ratio tcool /tff < 10 is needed for thermal instability to grow quickly enough to affect realistic cluster cores within a timescale that is relevant for cosmological structure formation. We find that instability leads to convection and that perturbations continue to grow while the gas convects. Condensation occurs when the timescale ratio in the low-entropy tail of the perturbation distribution drops below tcool /tff < 3, even if the volume-averaged timescale ratio is substantially greater. In our simulations, the geometry of the gravitational potential does not have a strong effect on thermal stability. Finally, we find that if condensation is powering feedback, a conversion efficiency of around 10^-3 for converting the condensed mass into thermal energy is sufficient to maintain thermal balance in the ICM.