Star clusters form in dense, hierarchically collapsing gas clouds. Bulk kinetic energy is
transformed to turbulence with stars forming from cores fed by filaments. In the most compact …

We analyse the first giant molecular cloud (GMC) simulation to follow the formation of
individual stars and their feedback from jets, radiation, winds, and supernovae, using the …

We present a unified description of the scenario of global hierarchical collapse (GHC). GHC
constitutes a flow regime of (non-homologous) collapses within collapses, in which all …

Aim. We have investigated the gas organization within the paradigmatic Integral Shape
Filament (ISF) in Orion in order to decipher whether or not all filaments are bundles of fibers …

Stars are among the most fundamental structures of our Universe. They comprise most of the
baryonic and luminous mass of galaxies; synthesize heavy elements; and inject mass …

In this chapter, we review some historical understanding and recent advances on the Initial
Mass Function (IMF) and the Core Mass Function (CMF), both in terms of observations and …

We analyse the morphology and kinematics of dense filamentary structures produced in a
numerical simulation of a star-forming cloud of 1.4× 104 M⊙ evolving under their own self …

The origin of the observed morphological and kinematic substructure of young star-forming
regions is a matter of debate. We offer a new analysis of data from simulations of globally …

Recent analyses of Gaia data have provided direct evidence that most young stellar clusters
are in a state of expansion, with velocities of the order of∼ 0.5 km s− 1. Traditionally …

Numerical simulations of star formation have found that a power-law mass function can
develop at high masses. In a previous paper, we employed isothermal simulations that …