The first generation of stars, often called Population III (or Pop III), form from metal-free
primordial gas at redshifts z∼ 30 and below. They dominate the cosmic star-formation …

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 …

ABSTRACT JWST observations indicate a surprising excess of luminous galaxies at z∼ 10
and above, consistent with efficient conversion of the accreted gas into stars, unlike the …

We introduce an updated physical model to simulate the formation and evolution of galaxies
in cosmological, large-scale gravity+ magnetohydrodynamical simulations with the moving …

How quasars powered by supermassive black holes formed less than a billion years after
the Big Bang is still one of the outstanding problems in astrophysics, 20 years after their …

We present two new Lagrangian methods for hydrodynamics, in a systematic comparison
with moving-mesh, smoothed particle hydrodynamics (SPH), and stationary (non-moving) …

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 …

Understanding the physics of turbulence is crucial for many applications, including weather,
industry and astrophysics. In the interstellar medium,, supersonic turbulence plays a crucial …

We perform a large set of cosmological simulations of early structure formation and follow
the formation and evolution of 1540 star-forming gas clouds to derive the mass distribution of …

We perform cosmological hydrodynamics simulations with non-equilibrium primordial
chemistry to obtain 59 minihalos that host first stars. The obtained minihalos are used as the …