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During the first few hundred days after the explosion, core-collapsesupernovae (SNe) emit down-scattered X-rays and gamma-rays originating fromradioactive line emissions, primarily from the $^{56}$Ni $\rightarrow$$^{56}$Co $\rightarrow$ $^{56}$Fe chain. We use SN models based onthree-dimensional neutrino-driven explosion simulations of single stars andmergers to compute this emission and compare the predictions with observationsof SN 1987A. A number of models are clearly excluded, showing that high-energyemission is a powerful way of discriminating between models. The best modelsare almost consistent with the observations, but differences that cannot bematched by a suitable choice of viewing angle are evident. Therefore, ourself-consistent models suggest that neutrino-driven explosions are able toproduce, in principle, sufficient mixing, although remaining discrepancies mayrequire small changes to the progenitor structures. The soft X-ray cutoff isprimarily determined by the metallicity of the progenitor envelope. The maineffect of asymmetries is to vary the flux level by a factor of ${\sim}$3. Forthe more asymmetric models, the shapes of the light curves also change. Inaddition to the models of SN 1987A, we investigate two models of Type II-P SNeand one model of a stripped-envelope Type IIb SN. The Type II-P models havesimilar observables as the models of SN 1987A, but the stripped-envelope SNmodel is significantly more luminous and evolves faster. Finally, we makesimple predictions for future observations of nearby SNe.

X-Ray and Gamma-Ray Emission From Core-collapse Supernovae: Comparison of Three-dimensional Neutrino-driven Explosions With SN 1987A