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.
On the clump mass concentration within the most massive cores
3 Pith papers cite this work. Polarity classification is still indexing.
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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.
The paper outlines the scientific motivation and expected capabilities of the SKA-Mid 10-15 GHz Galactic Plane survey to provide a uniform census of ionized structures.
citing papers explorer
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Characterising magnetic fields at the onset of star cluster formation: From giant molecular clouds to infrared dark clumps
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.
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Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
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.
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The 10-15 GHz radio continuum survey of the Galactic Plane with SKAO
The paper outlines the scientific motivation and expected capabilities of the SKA-Mid 10-15 GHz Galactic Plane survey to provide a uniform census of ionized structures.