Relativistic transport model for beta-particles in homologously expanding kilonova ejecta, incorporating per-species atomic data, shows non-local deposition and escape lower thermalization efficiency with analytic prescriptions supplied for light-curve codes.
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3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
citing papers explorer
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Beta-Particle Transport and Thermalization in Kilonova Ejecta with Detailed Atomic Microphysics
Relativistic transport model for beta-particles in homologously expanding kilonova ejecta, incorporating per-species atomic data, shows non-local deposition and escape lower thermalization efficiency with analytic prescriptions supplied for light-curve codes.
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Clumps in a Cocoon: Geometry and Mixing Set the Universal X-ray to H$\alpha$ Surface Brightness Ratio
3D wind-tunnel simulations in the χ~10^3 regime show clump-cocoon geometry sets SB_X/SB_Hα~3, with Hα fraction fixed by atomic physics and X-ray fraction set by residence time in the X-ray band that scales inversely with pressure.
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Cosmic Rays on Galaxy Scales: Progress and Pitfalls for CR-MHD Dynamical Models
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.