Polarization angle dispersion is systematically underestimated by factors of 1-10 due to scale dependence and beam effects, causing magnetic field strengths in star-forming regions to be overestimated.
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3 Pith papers cite this work, alongside 138 external citations. Polarity classification is still indexing.
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astro-ph.GA 3years
2026 3verdicts
UNVERDICTED 3representative citing papers
Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.
Milky Way linear filaments exhibit no strong B-field alignment and bimodal galactic-plane orientations (parallel near midplane, perpendicular far from it), supporting a super-Alfvénic bubbly disk model.
citing papers explorer
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Systematic underestimation of polarisation angle dispersion and its consequences for magnetic field strength estimates in star-forming regions
Polarization angle dispersion is systematically underestimated by factors of 1-10 due to scale dependence and beam effects, causing magnetic field strengths in star-forming regions to be overestimated.
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Magnetic field alignment with dense cores in the transition between cloud and core scales
Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.
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The Milky Way Atlas for Linear Filaments III: Giant filaments and magnetic fields as evidence of a bubbly Galactic disk
Milky Way linear filaments exhibit no strong B-field alignment and bimodal galactic-plane orientations (parallel near midplane, perpendicular far from it), supporting a super-Alfvénic bubbly disk model.