High-energy antiprotons from old supernova remnants

TL;DR

This paper extends a model explaining positron excesses to predict high-energy antiprotons from old supernova remnants, suggesting a distinctive rise in antiproton-to-proton ratio at high energies, impacting dark matter search strategies.

Contribution

It provides the first preliminary calculation of antiproton flux from old supernova remnants within the same framework as positron production, highlighting a unique high-energy signature.

Findings

Model predicts a rise in antiproton/proton ratio at high energies.

Consistent with current data but offers a testable high-energy prediction.

Implications for dark matter detection via antimatter are discussed.

Abstract

A recently proposed model (arXiv:0903.2794) explains the rise in energy of the positron fraction measured by the PAMELA satellite in terms of hadronic production of positrons in aged supernova remnants, and acceleration therein. Here we present a preliminary calculation of the anti-proton flux produced by the same mechanism. While the model is consistent with present data, a rise of the antiproton to proton ratio is predicted at high energy, which strikingly distinguishes this scenario from other astrophysical explanations of the positron fraction (like pulsars). We briefly discuss important implications for Dark Matter searches via antimatter.