Understanding massive stars is essential for a variety of branches of astronomy including
galaxy and star cluster evolution, nucleosynthesis and supernovae, pulsars, and black …

Understanding the formation of stars in galaxies is central to much of modern astrophysics.
However, a quantitative prediction of the star formation rate and the initial distribution of …

Much of the interstellar medium in disk galaxies is in the form of neutral atomic hydrogen, H
I. This gas can be in thermal equilibrium at relatively low temperatures, T≲ 300 K (the cold …

Context. Density and velocity fluctuations on virtually all scales observed with modern
telescopes show that molecular clouds (MCs) are turbulent. The forcing and structural …

We present Phantom, a fast, parallel, modular, and low-memory smoothed particle
hydrodynamics and magnetohydrodynamics code developed over the last decade for …

We study the impact of stellar winds and supernovae on the multiphase interstellar medium
using three-dimensional hydrodynamical simulations carried out with flash. The selected …

Atomic hydrogen (Hi) is a critical stepping stone in the gas evolution cycle of the interstellar
medium (ISM) of the Milky Way. Hi traces both the cold, premolecular state before star …

Using three-dimensional magnetohydrodynamic simulations, we investigate general
properties of a blast wave shock interacting with interstellar clouds. The pre-shock cloudy …

To study how supernova feedback structures the turbulent interstellar medium, we construct
3D models of vertically stratified gas stirred by discrete supernova explosions, including …

In this paper we present results from a large set of numerical simulations that demonstrate
that H 2 formation occurs rapidly in turbulent gas. Starting with purely atomic hydrogen, large …