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 …

Magnetohydrodynamic (MHD) turbulence is a crucial component of the current paradigms of
star formation, dynamo theory, particle transport, magnetic reconnection, and evolution of …

Giant molecular clouds (GMCs) are the sites of star formation and stellar feedback in
galaxies. Their properties set the initial conditions for star formation and their lifecycles …

Probability distribution functions of the total hydrogen column density (N-PDFs) are a
valuable tool for distinguishing between the various processes (turbulence, gravity, radiative …

Stars form in supersonic turbulent molecular clouds that are self-gravitating. We present an
analytic determination of the star formation rate (SFR) in a gravoturbulent medium based on …

Summary Enzo (Enzo Developers, 2019a) is a block-structured adaptive mesh refinement
code that is widely used to simulate astrophysical fluid flows (primarily, but not exclusively …

Star formation in our Galaxy occurs in molecular clouds that are self-gravitating, highly
turbulent, and magnetized. We study the conditions under which cloud cores inherit large …

High-resolution JWST-MIRI images of nearby spiral galaxies reveal emission with complex
substructures that trace dust heated both by massive young stars and the diffuse interstellar …

We analyse column density and temperature maps derived from Herschel dust continuum
observations of a sample of prominent, massive infrared dark clouds (IRDCs) ie G11. 11 …

Using a suite of 3D hydrodynamical simulations of star-forming molecular clouds, we
investigate how the density probability distribution function (PDF) changes when including …