Star-forming gas clouds are strongly magnetized, and their ionization fractions are high
enough to place them close to the regime of ideal magnetohydrodyamics on all but the …

Feedback to the interstellar medium from ionizing radiation, stellar winds and supernovae is
central to regulating star formation in galaxies. Owing to their low mass (< 109 solar …

The role of turbulence and magnetic fields is studied for star formation in molecular clouds.
We derive and compare six theoretical models for the star formation rate (SFR)—the …

We study the star formation efficiency (SFE) in simulations and observations of turbulent,
magnetized, molecular clouds. We find that the probability density functions (PDFs) of the …

We use high spatial resolution observations of CO to systematically measure the resolved
size-line width, luminosity-line width, luminosity-size, and mass-luminosity relations of GMCs …

Context. Even though turbulent motions are found everywhere in astrophysical systems, the
origin of this turbulence is poorly understood. When cosmic structures form, they grow in …

We explore what dominant physical mechanism sets the kinetic energy contained in neutral,
atomic (H i) gas. Both supernova (SN) explosions and magnetorotational instability (MRI) …

We use deep adaptive mesh refinement (AMR) simulations of isothermal self-gravitating
supersonic turbulence to study the imprints of gravity on the mass density distribution in …

Probability distribution functions of the total hydrogen column density (N-PDFs) are a
valuable tool for distinguishing between the various processes (turbulence, gravity, radiative …

We investigate the relationship between the velocity dispersion of the gas and the
supernova (SN) rate and feedback efficiency with three-dimensional numerical simulations …