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 …

In this chapter we review recent advances in understanding the roles that magnetic fields
play throughout the star formation process, gained through observations and simulations of …

We present a study of the relative orientation between the magnetic field projected onto the
plane of sky (B⊥) on scales down to 0.4 pc, inferred from the polarized thermal emission of …

We present synthetic dust polarization maps of simulated molecular clouds with the goal to
systematically explore the origin of the relative orientation of the magnetic field () with …

We present a study of the filamentary structure in the neutral atomic hydrogen (HI) emission
at the 21 cm wavelength toward the Galactic plane using the 16′. 2-resolution observations …

We present a study of the filamentary structure in the emission from the neutral atomic
hydrogen (HI) at 21 cm across velocity channels in the 40′′ and 1.5-km s− 1 resolution …

Magnetic fields of the order of 100 μG observed in young supernova remnants cannot be
amplified by shock compression alone. To investigate the amplification caused by a …

We present high-resolution (∼ 35 au) ALMA Band 6 1.3 mm dust polarization observations
of IRAS 16293. These observations spatially resolve the dust polarization across the two …

We analytically calculate the star formation efficiency and dense self-gravitating gas fraction
in the presence of magneto-gravo-turbulence using the model of Burkhart, which employs a …