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.
Planetary and Space Science , year = 1965, month = jan, volume = 13, pages =
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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.
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Numerical modeling of cosmic-ray transport in the heliosphere and interpretation of the proton-to-helium ratio in Solar Cycle 24
Numerical and analytical modeling of cosmic-ray transport attributes the long-term variation in the AMS-observed proton-to-helium ratio below 3 GV to mass-to-charge dependence in the heliospheric diffusion coefficient.