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TeV cosmic-ray electrons from millisecond pulsars

Published online by Cambridge University Press:  20 March 2013

Shota Kisaka  and
Norita Kawanaka
Shota Kisaka
Affiliation:
Institute for Cosmic Ray Research, University of Tokyo, Kashiwa-no-ha 5-1-5, Kashiwa-shi, Chiba, Japan email: [email protected]
Norita Kawanaka
Affiliation:
Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel email: [email protected]
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Abstract

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Recent γ-ray observations by the Fermi Gamma-Ray Space Telescope suggest that the γ-ray millisecond pulsar (MSP) population is separated into two subclasses with respect to pair multiplicity. Here, we calculate the cosmic-ray electron/positron spectra from MSPs. Based on the assumption of equipartition in the pulsar-wind region, the typical energy of electrons/positrons ejected by an MSP with pair multiplicity of the order of unity is ~50 TeV. In this case, we find that a large peak in the 10-50 TeV energy range would be observed in the cosmic-ray electron/positron spectrum. Even if the fraction of pair-starved MSPs is 10%, a large peak would be detectable with future missions such as CALET and CTA.

Keywords

stars: neutroncosmic rays
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 419 - 421
Copyright
Copyright © International Astronomical Union 2013

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