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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4 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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astro-ph.GA 4years
2026 4representative 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.
New observations confirm hourglass magnetic fields at clump scales in G35.20-0.74, with strengths of approximately 600 μG in G35N and 850 μG in G35S, supporting magnetically regulated collapse in G35N and feedback influence in G35S.
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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Investigation of Hourglass-shaped Magnetic fields in the G35.20-0.74 Star-Forming Complex
New observations confirm hourglass magnetic fields at clump scales in G35.20-0.74, with strengths of approximately 600 μG in G35N and 850 μG in G35S, supporting magnetically regulated collapse in G35N and feedback influence in G35S.
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