Self-generated magnetic turbulence in cosmic filaments suppresses low-rigidity UHECR escape for cluster-scale sources, photodisintegrates heavy nuclei into secondary protons below the ankle, and yields neutrino and gamma-ray fluxes compatible with or constrained by current limits.
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3D MHD simulations of CCSN remnants from RSG and WR stars show faster shocks from photoionization and CSM expansion, plus coherent reflected shocks in WR cases, with weakly magnetized bubbles limiting PeV acceleration.
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Self-confinement of ultra-high-energy nuclei in cosmic filaments: implications for the UHECR spectrum and composition
Self-generated magnetic turbulence in cosmic filaments suppresses low-rigidity UHECR escape for cluster-scale sources, photodisintegrates heavy nuclei into secondary protons below the ankle, and yields neutrino and gamma-ray fluxes compatible with or constrained by current limits.
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Multi-Dimensional MHD simulations of young Core-Collapse Supernova Remnants
3D MHD simulations of CCSN remnants from RSG and WR stars show faster shocks from photoionization and CSM expansion, plus coherent reflected shocks in WR cases, with weakly magnetized bubbles limiting PeV acceleration.