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%.
Interactions of Cosmic Ray Nuclei
4 Pith papers cite this work. Polarity classification is still indexing.
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abstract
We present convenient formulae for the energy losses of energetic atomic nuclei over the entire energy range relevant to the physics of cosmic rays. Results are applied to a leaky-box equation with a complete loss term. Thereby we derive the equilibrium spectrum of cosmic rays in various types of galaxies. We emphasize a spectral break energy at 450 MeV independent of the matter density, resulting from the transition from Coulomb and ionization losses to pion production losses as the relevant cooling process for the cosmic ray nuclei . We comment on the possible cosmic ray origin of the cosmic gamma ray background.
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astro-ph.HE 4years
2026 4verdicts
UNVERDICTED 4representative citing papers
SAETASS is a new open-source code that solves the astroparticle transport equation in spherical symmetry using finite-volume methods and modular operator splitting, validated on test cases and applied to cosmic-ray protons.
Ancient cosmic ray halos from the central galaxy boost Perseus's cool core via inverse-Compton scattering, simultaneously explaining radio minihalo, giant halo, X-ray properties, and gamma-ray data without re-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
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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SAETASS: Solver for Astroparticle Equation of Transport Analysis in Spherical Symmetry
SAETASS is a new open-source code that solves the astroparticle transport equation in spherical symmetry using finite-volume methods and modular operator splitting, validated on test cases and applied to cosmic-ray protons.
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An Inverse-Compton-Boosted Cool Core Unifies Perseus's Radio and X-ray Halos
Ancient cosmic ray halos from the central galaxy boost Perseus's cool core via inverse-Compton scattering, simultaneously explaining radio minihalo, giant halo, X-ray properties, and gamma-ray data without re-acceleration.
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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