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Cosmic-Ray Positrons Produced by Pulsar Winds from Mature Gamma-Ray Pulsars |
| ZHANG Li1,2,3;K. S. Cheng1,2;MEI Dong-Cheng1,2,3 |
| 1Department of Physics, Yunnan University, Kunming 650091
2Department of Physics, University of Hong Kong, Pokfulam Road, HongKong
3Yunnan Observatory, Chinese Academy of Sciences, Kunming 650011
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| Cite this article: |
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ZHANG Li, K. S. Cheng, MEI Dong-Cheng 2001 Chin. Phys. Lett. 18 701-704 |
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Abstract In the frame of the γ-ray pulsar outer gap model, e± pairs in the pulsar magnetosphere are produced by the cascade of e± pairs through synchrotron radiation of the return current from the outer gap. These pairs are accelerated mono-energetically to relativistic energies in the pulsar wind driven by low-frequency electromagnetic waves. Using Monte Carlo simulations, we generate a sample of the mature γ-ray pulsars in our Galaxy and calculate the positron production rate from these pulsars. With a simple leaky box model, we calculate the ratio of cosmic-ray positron to total electrons. Our result indicates that the pulsar contribution to the cosmic ray positron peaks at about 40 GeV and the observed e+/(e-+e+) ratio can be explained by this model.
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| Keywords:
97.60.Gb
95.85.Nv
95.85.Pw
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Published: 01 May 2001
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