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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10 Pith papers cite this work. Polarity classification is still indexing.
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UNVERDICTED 10representative 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.
LTE analysis of ALMA data for AG318-c9 yields molecular parameters and spatial maps for three COMs, compared to G31 as a line-identification template for the ALMAGAL survey.
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.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
SKAO, especially SKA-Mid Band 5, is expected to overcome dust opacity and frequency limits to detect complex prebiotic molecules in high-mass and solar-type protostellar regions.
The paper presents a science case for using SKAO to probe jets, outflows, magnetic fields, dust, and chemistry in young stellar objects at scales of a few au.
The chapter proposes SKA spectroscopic surveys of the inner and outer Milky Way using OH, CH, radio recombination lines, and H2CO to study molecular cloud formation, ionized gas properties, and CO-dark molecular gas.
This review summarizes the role of massive star feedback and projects how SKA radio observations will advance studies of HII regions, stellar winds, cosmic ray acceleration, and magnetic fields.
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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.