Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei

Details Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei Testing astrophysical models for the PAMELA positron excess with cosmic ray nuclei

2009-05-19

arxiv.org/abs/0905.3152v3

Phys.Rev.Lett.103:081104,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

4 pages, 2 figures (RevTex4); revised to include additional data in figures and references; accepted for publication in PRL

Scientific paper

10.1103/PhysRevLett.103.081104

The excess in the positron fraction reported by the PAMELA collaboration 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 stochastic acceleration of hadronic cosmic rays in nearby sources. We point out that measurements of secondary nuclei produced by cosmic ray spallation can discriminate between these possibilities. New data on the titanium-to-iron ratio from the ATIC-2 experiment support the hadronic source model above and enable a prediction to be made for the boron-to-carbon ratio at energies above 100 GeV. Presently, all cosmic ray data are consistent with the positron excess being astrophysical in origin.

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