Testing Astrophysical Models for the PAMELA Positron Excess with Cosmic Ray Nuclei
- 21 August 2009
- journal article
- research article
- Published by American Physical Society (APS) in Physical Review Letters
- Vol. 103 (8) , 081104
- https://doi.org/10.1103/physrevlett.103.081104
Abstract
The excess in the positron fraction measured by PAMELA has been interpreted as due to annihilation or decay of dark matter in the Galaxy. More prosaically it has been ascribed to direct production of positrons by nearby pulsars or due to pion production during diffusive shock acceleration of hadronic cosmic rays in nearby sources. We point out that measurements of secondary cosmic ray nuclei can discriminate between these possibilities. New data on the titanium-to-iron ratio support the hadronic source model above and enable a prediction for the boron-to-carbon ratio at energies above 100 GeV.Keywords
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This publication has 28 references indexed in Scilit:
- Origin of the Positron Excess in Cosmic RaysPhysical Review Letters, 2009
- TeV Gamma Rays from Geminga and the Origin of the GeV Positron ExcessPhysical Review Letters, 2009
- An anomalous positron abundance in cosmic rays with energies 1.5–100 GeVNature, 2009
- Possible causes of a rise with energy of the cosmic ray positron fractionPhysical Review D, 2009
- PAMELA and dark matterPhysics Letters B, 2009
- Pulsars as the sources of high energy cosmic ray positronsJournal of Cosmology and Astroparticle Physics, 2009
- Decaying dark matter can explain thee±excessesJournal of Cosmology and Astroparticle Physics, 2009
- New positron spectral features from supersymmetric dark matter: A way to explain the PAMELA data?Physical Review D, 2008
- Production and Propagation of Cosmic‐Ray Positrons and ElectronsThe Astrophysical Journal, 1998
- Electrons and positrons in the galactic cosmic raysPhysical Review D, 1995