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- W4386022016 abstract "The diffusion coefficients around the pulsar (gamma)-ray halos are highly suppressed compared with the value in the interstellar medium. It is suggested in the literature that the (gamma)-ray halos can be explained by a ballistic-diffusive (BD) propagation without slow diffusion. However, our calculation shows that the BD propagation cannot account for the (gamma)-ray halo profile well. Furthermore, the transfer efficiency of the pulsar spin-down energy to the high-energy electrons and positrons is even larger than 1 in the BD scenario. Therefore, slow diffusion is necessary to account for the pulsar (gamma)-ray halos. Taking the slow diffusion into account, the contribution of positron flux originating from nearby pulsars to the AMS-02 data is reexamined. We may also expect a slow diffusion disk of the Milky Way as many such slow diffusion regions exist. The positron contribution to the AMS-02 data from dark matter annihilation in the new propagation model is also reexamined. We find that the dark matter scenario satisfies all the (gamma)-ray limits in the new propagation model." @default.
- W4386022016 created "2023-08-22" @default.
- W4386022016 creator A5089707820 @default.
- W4386022016 date "2023-08-21" @default.
- W4386022016 modified "2023-09-27" @default.
- W4386022016 title "Slow diffusion around pulsar 𝜸-ray halos and its impact on cosmic rays propagation" @default.
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- W4386022016 doi "https://doi.org/10.32388/75mjfj" @default.
- W4386022016 hasPublicationYear "2023" @default.
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