Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.
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Magnetic fields in star formation: from clouds to cores
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Sub-Alfvénic MHD simulations with projection effects reproduce the range of observed polarization (μ, σ) values in Orion ISF, showing these statistics alone cannot constrain the 3D Alfvén Mach number.
Magnetic fields remain aligned with projected gravity throughout the DR21 ridge and sub-filaments, indicating guided accretion at rates that can build the ridge in about one million years.
The paper outlines the goals for the SKA-Mid Galactic Plane survey at 10-15 GHz to deliver the first uniform high-resolution view of ionized structures and feedback in the Milky Way.
Polarization observations reveal scale-dependent differences in magnetic field morphology between molecular clouds and clumps, a velocity-dispersion correlation, and unreliable field-strength estimates that contradict flux conservation.
Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.
Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-
Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.
High-resolution magnetic field maps of M17 SW reveal gravity-dominated energy budget with magnetic fields regulating collapse and accretion channels in a near-equipartition state.
Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
Correlations between HI velocity complexity and depolarization plus links between Faraday depth moments and neutral gas structure indicate neutral-dominated ISM regions contribute substantially to diffuse synchrotron emission and Faraday rotation.
Stronger radiation environments produce more massive, hotter protostellar discs whose fragments are large and disruptive rather than planetary-mass.
High-resolution dust polarization and C18O observations in Cepheus A show gravity driving gas accretion while magnetic tension regulates turbulence, producing ordered flows at 2.1e-4 solar masses per year with coherent B-field alignment across scales.
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.
The paper describes the expected capabilities of the SKA-Mid survey to produce a complete map of the Milky Way's magnetic field in the southern hemisphere using rotation measures and polarized emission.
The paper presents predictions and observational plans for Zeeman effect measurements with SKA to provide statistical data on magnetic field strengths across scales in molecular clouds.
Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.
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