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.
Probing the Turbulence Dissipation Range and Magnetic Field Strengths in Molecular Clouds
2 Pith papers cite this work. Polarity classification is still indexing.
2
Pith papers citing it
abstract
We study the turbulent velocity dispersion spectra of the coexistent HCN and HCO+ molecular species as a function of length scale in the M17 star-forming molecular cloud. We show that the observed downward shift of the ion's spectrum relative to that of the neutral is readily explained by the existence of an ambipolar diffusion range within which ion and neutral turbulent energies dissipate differently. We use these observations to evaluate this decoupling scale and show how to estimate the strength of the plane-of-the-sky component of the embedded magnetic field in a completely novel way.
fields
astro-ph.GA 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
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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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.
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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.