Atomic hydrogen (Hi) is a critical step** stone in the gas evolution cycle of the interstellar
medium (ISM) of the Milky Way. Hi traces both the cold, premolecular state before star …

Recent studies of the nearest star-forming clouds of the Galaxy at submillimeter wavelengths
with the Herschel Space Observatory have provided us with unprecedented images of 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 …

UV radiation feedback from young massive stars plays a key role in the evolution of giant
molecular clouds (GMCs) by photoevaporating and ejecting the surrounding gas. We …

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 …

Outflows from accreting, rotating, and magnetized systems are ubiquitous. Protostellar
outflows can be observed from radio to X-ray wavelengths in the continuum and a multitude …

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 …

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 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 …

Giant molecular clouds (GMCs) and their stellar offspring are the building blocks of galaxies.
The physical characteristics of GMCs and their evolution are tightly connected to galaxy …