Molecular hydrogen is the most abundant molecule in the universe. It is the first one to form
and survive photo-dissociation in tenuous environments. Its formation involves catalytic …

Understanding the formation of stars in galaxies is central to much of modern astrophysics.
However, a quantitative prediction of the star formation rate and the initial distribution of …

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 …

Supernova (SN) explosions deposit prodigious energy and momentum in their
environments, with the former regulating multiphase thermal structure and the latter …

The star formation rate (SFR) in galactic disks depends on both the quantity of the available
interstellar medium (ISM) gas and its physical state. Conversely, the ISM's physical state …

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

Star formation is a fundamental process for galactic evolution. One issue over the last
several decades has been determining whether star formation is induced by external …

Much of the interstellar medium in disk galaxies is in the form of neutral atomic hydrogen, H
I. This gas can be in thermal equilibrium at relatively low temperatures, T≲ 300 K (the cold …

Within ten nearby (d< 450 pc) Gould belt molecular clouds we evaluate statistically the
relative orientation between the magnetic field projected on the plane of sky, inferred from …

We find that clouds of optically thin, pressure-confined gas are prone to fragmentation as
they cool below∼ 106 K. This fragmentation follows the lengthscale∼ cst cool, ultimately …