A two-component Galactic source model with supernova remnants below 100 TeV and microquasars above, using charge-dependent cutoffs, accounts for cosmic-ray spectra, composition, and the all-particle spectrum up to PeV energies while ruling out nuclei-dependent cutoffs.
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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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Two kinds of Galactic source populations could explain the cosmic-ray observation up to the "knee" region
A two-component Galactic source model with supernova remnants below 100 TeV and microquasars above, using charge-dependent cutoffs, accounts for cosmic-ray spectra, composition, and the all-particle spectrum up to PeV energies while ruling out nuclei-dependent cutoffs.
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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