High-energy antiprotons from old supernova remnants

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.

4 pages, 1 figure; minor revision, matches published version

References in corpus (6)

• Observation of an anomalous positron abundance in the cosmic radiation
• A new measurement of the antiproton-to-proton flux ratio up to 100 GeV in the cosmic radiation
• Cosmic-ray positron fraction measurement from 1 to 30 GeV with AMS-01
• The origin of the positron excess in cosmic rays
• Constraints on WIMP Dark Matter from the High Energy PAMELA $\bar{p}/p$ data
• Galactic Cosmic Ray Nuclei as a Tool for Astroparticle Physics

Cited by in corpus (3)

• Inverse Compton constraints on the Dark Matter e+e- excesses
• Constraints on Dark Matter annihilations from reionization and heating of the intergalactic gas
• Extended MSSM Neutralinos as the Source of the PAMELA Positron Excess