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We compute the energy spectra of antideuterons and antihelium in cosmic rays(CRs) in a scenario where hadronic interactions inside supernova remnants(SNRs) can produce a diffusively-shock-accelerated "source component" ofsecondary antinuclei. The key parameters that specify the SNR environment andthe interstellar CR transport are tightly constrained with the new measurementsprovided by the AMS experiment on the B/C ratio and on the antiproton/protonratio. The best-fit models obtained from the two ratios are found to beinconsistent with each other, as the antiproton/proton data require enhancedsecondary production. Thus, we derive conservative (i.e., B/C-driven) andspeculative (antiproton/proton-driven) upper limits to the SNR fluxcontributions for the d and He spectra spectra in CRs, along with theirstandard secondary component expected from CR collisions in the interstellargas. We find that the source component of antinuclei can be appreciable atkinetic energies above a few ~10 GeV/n, but it is always sub-dominant below afew GeV/n, that is the energy window where dark matter (DM) annihilationsignatures are expected to exceed the level of secondary production. We alsofind that the total (standard + SNR) flux of secondary antinuclei is tightlybounded by the data. Thus the presence of interaction processes inside SNRsdoes not critically affect the total background for DM searches.

Production and acceleration of antinuclei in supernova shockwaves