Giant molecular clouds (GMCs) and their stellar offspring are the building blocks of galaxies.
The physical characteristics of GMCs and their evolution are tightly connected to galaxy …

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 …

This is a summary of the 2013 release of the plasma simulation code Cloudy. Cloudy
models the ionization, chemical, and thermal state of material that may be exposed to an …

Star formation is slow in the sense that the gas consumption time is much longer than the
dynamical time. It is also inefficient; star formation in local galaxies takes place in giant …

We evaluate the role of radiation pressure in the dynamics of H ii regions. We first determine
under what conditions radiation pressure is significant in comparison to gas pressure and …

We use 3D hydrodynamical models to investigate the effects of massive star feedback from
winds and supernovae on inhomogeneous molecular material left over from the formation of …

Supernovae (SNe) dominate the energy and momentum budget of stellar feedback, but the
efficiency with which they couple to the interstellar medium (ISM) depends strongly on how …

Star clusters interact with the interstellar medium (ISM) in various ways, most importantly in
the destruction of molecular star-forming clouds, resulting in inefficient star formation on …

We exploit ionization-parameter mapping (IPM) as a powerful tool to measure the optical
depth of star-forming H ii regions. Our simulations using the photoionization code Cloudy …

Context. The past decade has witnessed a large number of Galactic plane surveys at
angular resolutions below 20′′. However, no comparable high-resolution survey exists at …