Abstract
Nonthermal radiative properties of three TeV shell-type supernova remnants (SNRs) RX J1713.7?3946, RX?J0852.0?4622, and RCW 86, argued to be expanding into low-density hot bubbles created by the wind of the massive progenitor stars, are investigated based on a semi-analytical solution to diffusive acceleration at nonlinear shocks. In the model, a free-escape boundary upstream of the shock is used to mimic the escape of cosmic rays from the SNR, with the dynamic reaction of the self-generated magnetic field via resonant streaming instability on the shock taken into account. Origins of the ?-rays from the three remnants are studied with appropriate parameters, and consistent results with the multiband observed fluxes are obtained within the nonlinear diffusive shock acceleration regime. The order of the resulting downstream magnetic field strength for the three SNRs is between 60 and 100 ?G, and the observed TeV ?-rays are mainly produced via the decay of neutral ? mesons produced from the hadronic collisions.
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