MHD simulations show CNM clouds are elongated along the local magnetic field with lower disorder per column density than the WNM, explaining the f_CNM-polarization trend for low-cloud-count sightlines.
B., et al., 2022, @doi [ ] 10.1093/mnras/stac2448 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.4417P 516
5 Pith papers cite this work. Polarity classification is still indexing.
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UNVERDICTED 5representative citing papers
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.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
Reviews SKA techniques for reconstructing 3D magnetic field vectors in the ISM but presents no new data or derivations.
Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.
citing papers explorer
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Phase-dependent magnetic coherence in the turbulent interstellar medium
MHD simulations show CNM clouds are elongated along the local magnetic field with lower disorder per column density than the WNM, explaining the f_CNM-polarization trend for low-cloud-count sightlines.
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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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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.
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Small-scale Magnetic Fields in the Milky Way and Nearby Galaxies
Review chapter summarizing the importance of small-scale galactic magnetic fields and proposing SKA observation strategies.