Numerical modeling of time-dependent cosmic-ray advection and diffusion in spherically symmetric wind bubbles shows escaping spectra harder than E^{-2} during the wind-driven phase, with low-energy suppression depending on the turbulence model.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
fields
astro-ph.HE 5years
2026 5verdicts
UNVERDICTED 5representative citing papers
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.
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
Numerical transport modeling of the Cygnus Bubble finds that spatially dependent Bohm diffusion and strong suppression of the diffusion coefficient over at least 150 pc are required to match the observed gamma-ray spectrum and morphology, implying extreme assumptions for steady hadronic acceleration
citing papers explorer
-
Time-dependent cosmic-ray escape from wind bubbles: hard spectra formation
Numerical modeling of time-dependent cosmic-ray advection and diffusion in spherically symmetric wind bubbles shows escaping spectra harder than E^{-2} during the wind-driven phase, with low-energy suppression depending on the turbulence model.
-
Wolf-Rayet stars as tracers of gamma-ray emission: Isolated stars and stellar clusters/associations
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 at Supernova Remnants in Massive Star Clusters: A Model for the Cosmic-Ray Knee Observed by LHAASO
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.
-
Direct simulations of very high energy cosmic ray acceleration in 3D MHD model of a compact star cluster
3D MHD simulations of young massive star clusters find proton acceleration to hundreds of TeV near O-star termination shocks, with even faster acceleration to over 100 TeV in under 100 years when a supernova remnant expands inside the core.
-
Suppressed diffusion and gamma-ray emission from the Cygnus Bubble
Numerical transport modeling of the Cygnus Bubble finds that spatially dependent Bohm diffusion and strong suppression of the diffusion coefficient over at least 150 pc are required to match the observed gamma-ray spectrum and morphology, implying extreme assumptions for steady hadronic acceleration