2011MNRAS.414.3521E

We present calculations of expected continuum emissions from Sedov–Taylor phase Type Ia supernova remnants (SNRs), using the energy spectra of cosmic ray (CR) electrons and protons from non-linear diffusive shock acceleration simulations. A new, general-purpose radiative process code, COSMICP, was employed to calculate the radiation expected from CR electrons and protons and their secondary products. These radio, X-ray and gamma-ray emissions are generally consistent with current observations of Type Ia SNRs. The emissions from electrons in these models dominate the radio through X-ray bands. Decays of π⁰s from p–p collisions mostly dominate the gamma-ray range, although for a hot, low-density ISM case (n_ISM= 0.003/cm3), the pion decay contribution is reduced sufficiently to reveal the inverse Compton contribution to TeV gamma-rays. In addition, we present simple scalings for the contributing emission processes to allow a crude exploration of model parameter space, enabling these results to be used more broadly. We also discuss the radial surface brightness profiles expected for these model SNRs in the X-ray and gamma-ray bands.