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The antiproton-to-proton ratio in the cosmic-ray spectrum is a sensitiveprobe of new physics. Using recent measurements of the cosmic-ray antiprotonand proton fluxes in the energy range of 1-1000 GeV, we study the contributionto the $\bar{p}/p$ ratio from secondary antiprotons that are produced andsubsequently accelerated within individual supernova remnants. We considerseveral well-motivated models for cosmic-ray propagation in the interstellarmedium and marginalize our results over the uncertainties related to theantiproton production cross section and the time-, charge-, andenergy-dependent effects of solar modulation. We find that the increase in the$\bar{p}/p$ ratio observed at rigidities above $\sim$ 100 GV cannot beaccounted for within the context of conventional cosmic-ray propagation models,but is consistent with scenarios in which cosmic-ray antiprotons are producedand subsequently accelerated by shocks within a given supernova remnant. Inlight of this, the acceleration of secondary cosmic rays in supernova remnantsis predicted to substantially contribute to the cosmic-ray positron spectrum,accounting for a significant fraction of the observed positron excess.

Possible Evidence for the Stochastic Acceleration of Secondary Antiprotons by Supernova Remnants