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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Advection-only galactic wind models fail to reproduce observed vertical radio profiles without unrealistic velocities, synchrotron spectra are biased toward young electrons in dense regions, and bremsstrahlung/Coulomb losses cannot be neglected even when subdominant.
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.
A 1D spherically symmetric Parker transport model with charge-sign and rigidity-dependent parameters fitted via solar-proxy cross-correlation is validated on PAMELA, AMS-02, and ACE data for long-term GCR forecasting.
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.
Radiative filaments in the Cygnus Loop exhibit thermal radio spectra resembling HII regions instead of typical SNR non-thermal emission.
Fermi-LAT and CO data support a hadronic PeVatron scenario for LHAASO J1912+1014u with proton index ~2.2 and total energy (1-5) x 10^49 erg above 1 GeV.
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.
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
Galactic wind advection with a peak velocity of ~700 km/s reproduces cosmic ray spectral hardening from hundreds of GV and softening from a few TV without diffusion breaks, predicts a hard spectrum (index ~2) at 3-5 kpc altitudes consistent with Fermi bubbles, and shows the wind maintains disk metal
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Steady-State or Not? The Evolution of Cosmic Ray Electron Spectra in Galaxies
Time-dependent cosmic ray electron spectra in a simulated galactic disk match steady-state solutions up to 500 GeV but become steeper and more disk-confined at higher energies due to recent injections.