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%.
@doi [ ] 10.1051/0004-6361/200911794, https://ui.adsabs.harvard.edu/abs/2009A&A...501..619P 501
5 Pith papers cite this work. Polarity classification is still indexing.
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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.
Magnetic fields remain aligned with projected gravity throughout the DR21 ridge and sub-filaments, indicating guided accretion at rates that can build the ridge in about one million years.
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.
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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A broadband view of the thermal and non-thermal emission from the embedded massive star cluster RCW 38
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.