Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
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8 Pith papers cite this work. Polarity classification is still indexing.
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UNVERDICTED 8representative citing papers
Multi-wavelength MCMC modeling of RCW 38 supports hadronic gamma-ray production with K_ep ≲ 10^{-3} and acceleration efficiency ≳1%, consistent with cosmic-ray composition requirements.
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
Low-energy cosmic ray ionization rates in the Orion region scale with star formation rate as log10 ζ = (1.4±0.70)log10 SFR + (-10.5±2.9), supporting local generation by star formation.
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.
Numerical transport modeling of the Cygnus Bubble finds that spatially dependent Bohm diffusion and strong suppression of the diffusion coefficient over at least 150 pc are required to match the observed gamma-ray spectrum and morphology, implying extreme assumptions for steady hadronic acceleration
Review of cosmic ray production and radio emission in galaxy clusters with recommendations for SKA observations of magnetic fields and low-energy particles.
citing papers explorer
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The cosmic ray ionization rate from H3+ observations can be overestimated due to neglect of time-dependent chemistry
Time-dependent chemistry in 3D MHD simulations leads to H3+ abundances that, when analyzed under steady-state assumptions, imply CRIR values 2-5 times higher than the true input rate, with a median factor of ~3.
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Star Formation Drives Production of Low Energy Cosmic Rays
Low-energy cosmic ray ionization rates in the Orion region scale with star formation rate as log10 ζ = (1.4±0.70)log10 SFR + (-10.5±2.9), supporting local generation by star formation.
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Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds
SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.
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A HINSA view of cosmic-ray ionization in IC 348 and NGC 1333: evidence for a strong low-energy cosmic-ray disparity
HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.