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 …

Context. While star formation on large molecular cloud scales and on small core and disk
scales has been investigated intensely over the past decades, the connection of the large …

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 …

Strong Alfvénic turbulence develops eddy-like motions perpendicular to the local direction of
magnetic fields. This local alignment induces velocity gradients perpendicular to the local …

Recent developments of the velocity gradient technique (VGT) show that the velocity
gradients provide a reliable tracing of the magnetic field direction in turbulent plasmas. In …

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 …

The interaction of turbulence, magnetic fields, self-gravity, and stellar feedback within
molecular clouds is crucial for understanding star formation. We study the effects of self …

We derive an analytic expression for the transitional column density value (${\eta} _ {t} $)
between the lognormal and power-law form of the probability distribution function (PDF) in …