Magnetic fields remain aligned with projected gravity throughout the DR21 ridge and sub-filaments, indicating guided accretion at rates that can build the ridge in about one million years.
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7 Pith papers cite this work, alongside 554 external citations. Polarity classification is still indexing.
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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.
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.
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
Core-scale magnetic fields in star-forming regions are more disordered than cloud-scale fields and align randomly with core orientations and velocity gradients.
Derives polarization-dependent damping and heating rates for Alfvénic waves in two-fluid weakly ionized plasmas and simulates nonlinear ponderomotive effects and collisional dissipation.
Review summarizing observational data on the Milky Way's magnetic field structure, including spiral alignment, halo components, turbulence, and correlations with interstellar gas and dust.
citing papers explorer
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SIMPLIFI -- Study of Interstellar Magnetic Polarization: a Legacy Investigation of Filaments. I. Magnetically-Guided Accretion onto the DR21 Ridge
Magnetic fields remain aligned with projected gravity throughout the DR21 ridge and sub-filaments, indicating guided accretion at rates that can build the ridge in about one million years.
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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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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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Non-linear Dynamical Stability of Magnetic Polytropes
A mean-field magnetic polytrope model shows radiation pressure can unbind an n=3 polytrope when the central overpressure exceeds roughly 0.15 times a mass-dependent factor under small radial perturbations.
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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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Propagation of waves in weakly ionized two-fluid plasmas. II. Nonlinear Alfv\'enic waves
Derives polarization-dependent damping and heating rates for Alfvénic waves in two-fluid weakly ionized plasmas and simulates nonlinear ponderomotive effects and collisional dissipation.
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The magnetic field of the Milky Way: an observational perspective
Review summarizing observational data on the Milky Way's magnetic field structure, including spiral alignment, halo components, turbulence, and correlations with interstellar gas and dust.