Cosmic ray protons and electrons from supernova remnants

The spectrum of cosmic ray protons and electrons released by supernova remnants throughout their evolution is poorly known, because the difficulty in accounting for particle escape confinement downstream a shock front, where both adiabatic radiative losses are present. Here we calculate during supernovae different types, from upstream particles advected liberated at later times. same calculation carried out electrons. magnetic field post-shock region calculated using an analytic treatment amplification due to non--resonant resonant streaming instability saturation. We find that when result growth cosmic-ray--driven alone, remnant indeed different, but such difference becomes appreciable only energies $\gtrsim 100-1000$ GeV, while observations electron require be present as low $\sim 10$ GeV. An effect requires substantial late stages (shock velocity $\ll 1000$ km/s), perhaps not hydrodynamical processes. comment on feasibility conditions speculate possibility spectral shape between may reflect either some unknown acceleration effect, or additional energy cocoons around sources.