Star formation lies at the center of a web of processes that drive cosmic evolution:
generation of radiant energy, synthesis of elements, formation of planets, and development …

Stars form within molecular clouds but our understanding of this fundamental process
remains hampered by the complexity of the physics that drives their evolution. We review our …

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 present a theoretical framework in which bound stellar clusters arise naturally at the high-
density end of the hierarchy of the interstellar medium (ISM). Due to short free-fall times …

We study the formation and evolution of a sample of Lyman break galaxies in the epoch of
reionization by using high-resolution (∼ 10 pc), cosmological zoom-in simulations part of …

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

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 …

Dusty star-forming galaxies at high redshift (1< z< 3) represent the most intense star-forming
regions in the universe. Key aspects to these processes are the gas heating and cooling …

The star formation rate (SFR) in the Central Molecular Zone (CMZ, ie the central 500 pc) of
the Milky Way is lower by a factor of≥ 10 than expected for the substantial amount of dense …