PCA of 25 molecular lines across 1001 Orion B cores reveals that chemical diversity is driven by column density, the FUV-to-density ratio G0/n, and freeze-out signatures tied to mean density.
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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.
citing papers explorer
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Chemical diversity of dense cores in Orion B: The role of the environment
PCA of 25 molecular lines across 1001 Orion B cores reveals that chemical diversity is driven by column density, the FUV-to-density ratio G0/n, and freeze-out signatures tied to mean density.
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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.