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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9 Pith papers cite this work, alongside 186 external citations. Polarity classification is still indexing.
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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.
Cosmic ray transport requires a propagator P(k,s) that encodes memory and non-diffusive behaviors rather than being reduced to a single diffusion coefficient.
Multiphase ISM simulations show PeV cosmic-ray diffusion coefficients reach 10^30 cm^2 s^-1, with perpendicular transport boosted at thermal phase boundaries while overall transport is controlled by trans-Alfvenic warm and unstable gas.
Wolf-Rayet star clusters show a marginal spatial correlation with unidentified GeV gamma-ray sources, with 11 new cluster associations and 4 isolated WR stars identified as potential emitters from wind termination shocks.
Oblique shocks in massive star clusters accelerate cosmic rays to multi-PeV energies, reproducing the LHAASO-observed knee as a sequence of rigidity-dependent cutoffs from combined supernova and wind shocks.
Alternative ISRF models produce only modest changes to the LHAASO diffuse gamma-ray fit; the associated pp neutrinos remain consistent with IceCube all-sky data and compatible with ANTARES/KM3NeT limits.
A review summarizing pitfalls in older CR-MHD models and progress toward more rigorous treatments that connect microphysical CR scales to galactic dynamics.
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Beyond the Diffusion Coefficient: Propagators and Memory in Cosmic Ray Transport
Cosmic ray transport requires a propagator P(k,s) that encodes memory and non-diffusive behaviors rather than being reduced to a single diffusion coefficient.