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Galactic outflows driven by feedback mechanisms carry material outwards (Veilleux, Cecil & Bland-Hawthorn 2005) while inflowing gas provides fuel for new star formation (e.g.

One that sits at the very heart is the challenge to understand the multiphase nature of not just the gas within galaxies and their surrounding environment (circumgalactic medium, CGM), but also the flow of this material in and out of galaxies and how this regulates galaxy evolution (often dubbed the Cosmic Baryon Cycle see Tumlinson, Peeples & Werk 2017). A multitude of open problems still surround galaxy formation and evolution today. It is, however, essential towards making the most of our evergrowing body of increasingly detailed observations. Understanding the inherently non-linear, dynamical structures that underlie the complex ecosystems of galaxies is a challenging task. Hydrodynamics, instabilities, turbulence, galaxies: clusters: general, galaxies: evolution, galaxies: haloes 1 INTRODUCTION This opens the door to developing effective subgrid recipes for their inclusion in global-scale galaxy models where they are unresolved. We conclude that many of the physical insights and analytic scalings derived from idealized small-scale simulations of turbulent radiative mixing layers and cloud–wind interactions are directly translatable and applicable to these larger scale cloud populations. Turbulence provides significant pressure support in the clouds, while magnetic fields only play a minor role. Cloud sizes are well described by a power-law distribution and mass growth rates can be modelled using turbulent radiative mixing layer theory. Their presence induces large-scale turbulence, which, in turn, leads to complex cloud morphologies. We focus on analyzing and modelling the origin and properties of these clouds. Dynamical fragmentation of the ISM during superbubble breakout seeds the resulting hot outflow with a population of cool clouds. We present the results of three-dimensional magnetohydrodynamical simulations of tall–box interstellar medium (ISM) patches with clustered supernova-driven outflows. One outstanding problem is the understanding and modelling of the multiphase nature of galactic winds, which play a crucial role in galaxy formation and evolution. Central among these are the multiplicity of feedback channels, which remain incompletely understood.

Galaxies comprise intricate networks of interdependent processes which together govern their evolution.

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