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%.
E., Sipil¨a, O., Segura-Cox, D
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Neglect of time-dependent chemistry causes steady-state analyses of H3+ observations to overestimate the cosmic-ray ionization rate by a median factor of ~3, yielding a revised mean ζ_H2 ≈ 2×10^{-17} s^{-1}.
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.
Ionization rates in the envelopes of NGC-1333 IRAS4A, L1448-C, and L1157 reach 1e-16 to 1e-13 s^{-1}, far above the ISM baseline of 6e-17 s^{-1}.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
citing papers explorer
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
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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The cosmic ray ionization rate from H3+ observations can be overestimated due to neglect of time-dependent chemistry
Neglect of time-dependent chemistry causes steady-state analyses of H3+ observations to overestimate the cosmic-ray ionization rate by a median factor of ~3, yielding a revised mean ζ_H2 ≈ 2×10^{-17} s^{-1}.
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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.
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Evidence of Enhanced Ionization in Protostellar Envelopes
Ionization rates in the envelopes of NGC-1333 IRAS4A, L1448-C, and L1157 reach 1e-16 to 1e-13 s^{-1}, far above the ISM baseline of 6e-17 s^{-1}.
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Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.