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.
Title resolution pending
4 Pith papers cite this work, alongside 230 external citations. Polarity classification is still indexing.
4
Pith papers citing it
230
external citations · OpenAlex
fields
astro-ph.GA 4years
2026 4representative citing papers
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.
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.
citing papers explorer
-
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.
-
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.
-
3D Magnetic Field Vectors in Space: Bubbles, Clouds, and Filaments
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.
- Grain alignment and dust evolution physics with polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra