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.
H., Kirby , L., Dotson , J
6 Pith papers cite this work, alongside 286 external citations. Polarity classification is still indexing.
6
Pith papers citing it
286
external citations · OpenAlex
fields
astro-ph.GA 6years
2026 6representative citing papers
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.
New optical polarization data of over 90,000 stars shows H I filaments in the Riegel-Crutcher cloud tightly aligned with a coherent plane-of-sky magnetic field, indicating magnetic fields shape the cold neutral medium.
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
-
Projection Is All You Need: Interpreting Polarization Measurements in the Orion Clouds with Sub-Alfv\'enic MHD Simulations
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.
-
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.
-
When Magnetic Fields Sculpt the Sky: The Riegel-Crutcher cloud in optical polarization
New optical polarization data of over 90,000 stars shows H I filaments in the Riegel-Crutcher cloud tightly aligned with a coherent plane-of-sky magnetic field, indicating magnetic fields shape the cold neutral medium.
-
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