The interstellar medium (ISM) is inhomogeneous, with clouds of various temperatures and
densities embedded in a tenuous intercloud medium. Shocks propagating through the ISM …

The large number of subordinate lines of a representative ion are found to have a dominant
effect on the force of radiation on material in O star atmospheres. The force is increased over …

Stars do not generally form in isolation. Instead, they form in clusters, and in these clustered
environments, newborn stars can have profound effects on one another and on their parent …

Massive stars produce so much light that the radiation pressure they exert on the gas and
dust around them is stronger than their gravitational attraction, a condition that has long been …

X-ray burst emission during the shock breakout phase of a Type II supernova is investigated
for a 12-solar-mass red giant at the end of its nuclear evolution. A supernova model based …

We demonstrate with a new three-dimensional adaptive mesh refinement code that
perturbations arising from discretization of the equations of self-gravitational hydrodynamics can …

We simulate the early stages of the evolution of turbulent, virialized, high-mass protostellar
cores, with primary attention to how cores fragment and whether they form a small or large …

Forming stars emit a substantial amount of radiation into their natal environment. We use
ORION, an adaptive mesh refinement (AMR) three-dimensional gravito-radiation-hydrodyanics …

We introduce a new computational method for embedding Lagrangian sink particles into a
Eulerian calculation. Simulations of gravitational collapse or accretion generally produce …

We study rapidly accreting, gravitationally unstable disks with a series of idealized global,
numerical experiments using the code ORION. Our numerical parameter study focuses on …