TeV cosmic-ray electrons from millisecond pulsars
Article first published online: 5 MAR 2012
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
Monthly Notices of the Royal Astronomical Society
Volume 421, Issue 4, pages 3543–3549, April 2012
How to Cite
Kisaka, S. and Kawanaka, N. (2012), TeV cosmic-ray electrons from millisecond pulsars. Monthly Notices of the Royal Astronomical Society, 421: 3543–3549. doi: 10.1111/j.1365-2966.2012.20576.x
- Issue published online: 10 APR 2012
- Article first published online: 5 MAR 2012
- Accepted 2012 January 16. Received 2011 December 22; in original form ?
- stars: neutron;
- cosmic rays
Recent γ-ray observations by 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 a 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 per cent, a large peak would be detectable in future observations. We also calculate the contribution from MSPs with high pair multiplicity to the electron/positron spectrum. We suggest that if the multiplicity of the dominant MSP population is ∼103, electrons/positrons from this population may contribute to the observed excess from the background electron/positron flux and positron fraction.