Lepto-hadronic Unified Model of \(\gamma\)-ray Supernova Remnants
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Dwarkadas (2013) has similar idea of SNR hadronic \(\gamma\)-ray evolution; also mature SNR evolution.
Cristofari et al. (2013) calculated the flux evolution, but doesn’t compare with observations
We need progenitor mass v.s. bubble size; ambient density distribution; thin shell baryonic mass bushed by wind; SNR evolution in wind environment; electon propagation and cooling; magnetic field strength evolution at SNR shock, etc.