# How cold gas continuously entrains mass and momentum from a hot wind

## TL;DR

This paper demonstrates that radiative cooling enables cold gas clouds in galactic winds to continuously entrain mass and momentum from hot winds, explaining the persistent presence of cold gas in galactic environments.

## Contribution

It provides detailed analysis showing that cooling-induced pressure gradients, not Kelvin-Helmholtz instability, drive robust cloud acceleration and growth across various scenarios.

## Key findings

- Cold gas can accelerate to wind speeds and grow in mass via cooling.
- Growth peaks when clouds are nearly co-moving with the wind.
- Magnetic fields alter cloud morphology, creating low-density filaments.

## Abstract

The existence of fast moving, cold gas ubiquitously observed in galactic winds is theoretically puzzling, since the destruction time of cold gas is much smaller than its acceleration time. In previous work, we showed that cold gas can accelerate to wind speeds and grow in mass if the radiative cooling time of mixed gas is shorter than the cloud destruction time. Here, we study this process in much more detail, and find remarkably robust cloud acceleration and growth in a wide variety of scenarios. Radiative cooling, rather than the Kelvin-Helmholtz instability, enables self-sustaining entrainment of hot gas onto the cloud via cooling-induced pressure gradients. Indeed, growth peaks when the cloud is almost co-moving. The entrainment velocity is of order the cold gas sound speed, and growth is accompanied by cloud pulsations. Growth is also robust to the background wind and initial cloud geometry. In an adiabatic Chevalier-Clegg type wind, for instance, the mass growth rate is constant. Although growth rates are similar with magnetic fields, cloud morphology changes dramatically, with low density, magnetically supported filaments which have a small mass fraction but dominate by volume. This could bias absorption line observations. Cloud growth from entraining and cooling hot gas can potentially account for the cold gas content of the CGM. It can also fuel star formation in the disk as cold gas recycled in a galactic fountain accretes and cools halo gas. We speculate that galaxy-scale simulations should converge in cold gas mass once cloud column densities of ${\rm N} \sim 10^{18} \ {\rm cm^{-2}}$ are resolved.