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%.
Title resolution pending
3 Pith papers cite this work. Polarity classification is still indexing.
3
Pith papers citing it
years
2026 3representative citing papers
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.
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
citing papers explorer
-
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%.
-
Revisiting radio synchrotron diagnostics in star-forming galaxies
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.
-
Cosmic-Ray Spectra and Metal Budget Regulated by the Galactic Wind
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