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We calculated synchrotron radio emission and [math]-ray emission due to bremsstrahlung, inverse-Compton scattering, and [math]-decay from the remnant of supernova that exploded in the circumstellar matter (CSM) formed by the progenitor's stellar wind. This sort of situation is a possible origin of mixed-morphology supernova remnants (SNRs), like W 49B, which exhibit recombination-radiation spectra in X-ray emission. We assumed that the CSM of 1.5 [math] exists at 0.07–3 pc away from the supernova in the interstellar medium (ISM) of density 0.016 cm[math] . When the blast wave breaks out of the CSM into the ISM, its velocity rapidly increases, and hence particle acceleration is enhanced. The maximum energy of protons reaches [math] 1300 TeV just after the break-out with [math] 0.5% of the explosion energy. We considered the non-thermal emission from the blast-shocked ISM shell after the break-out. Synchrotron radio flux at 1 GHz is tens of Jy, comparable to that observed from mixed-morphology SNRs. Because of low density, the [math]-ray luminosity is dominated by inverse-Compton scattering, which is higher than the [math]-decay luminosity by an order of magnitude. The total [math]-ray luminosity, including bremsstrahlung, is on the order of 10[math] erg s[math] lower than the typical value of 10[math] –10[math] erg s[math] observed from mixed-morphology SNRs. However, if, e.g., [math] 10% of accelerated protons interact with some matter of density of [math] 100 cm[math] , the [math]-decay [math]-ray luminosity would be enhanced to be comparable with the observed value.

*Keywords: *
ISM: supernova remnants;
circumstellar matter

*Journal Article.*
*5350 words.*
*Illustrated.*

*Subjects: *
Stars
;
Interstellar Medium

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