Stellar multiplicity is a ubiquitous outcome of the star-formation process. The frequency and
main characteristics of multiple systems, and their dependence on primary mass and …

Our Sun and planetary system were born about 4.5 billion years ago. How did this happen,
and what is the nature of our heritage from these early times? This review tries to address …

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 results from the first population synthesis study of protostellar discs. We analyse
the evolution and properties of a large sample of protostellar discs formed in a radiation …

We derive an analytical theory of the prestellar core initial mass function (IMF) based on an
extension of the Press-Schechter statistical formalism. Our approach relies on the general …

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 …

We report the statistical properties of stars, brown dwarfs and multiple systems obtained from
the largest hydrodynamical simulation of star cluster formation to date that resolves masses …

Star formation is inefficient. Only a few per cent of the available gas in molecular clouds
forms stars, leading to the observed low star formation rate (SFR). The same holds when …

The very first stars to form in the universe heralded an end to the cosmic dark ages and
introduced new physical processes that shaped early cosmic evolution. Until now, it was …

We investigate massive star formation in turbulent, magnetized, parsec-scale clumps of
molecular clouds including protostellar outflow feedback using three-dimensional numerical …