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 nonlinear diffusive shock acceleration ( DSA ) 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 \pi ^ { 0 } s from p - p collisions mostly dominate the gamma-ray range , although for a hot , low density ISM case ( n _ { ISM } = 0.003 ~ { } { cm ^ { -3 } } ) , 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 .