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Pulsar giant pulse: Coherent instability near light cylinder

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Abstract

Giant pulses (GPs) are extremely bright individual pulses of radio pulsar. In microbursts of Crab pulsar, which is an active GP emitter, zebra-pattern-like spectral structures are observed, which are reminiscent of the “zebra bands” that are observed in type IV solar radio flares. However, band spacing linearly increases with the band center frequency of ∼5-30 GHz. In this study, we propose that the Crab pulsar GP can originate from the coherent instability of plasma near a light cylinder. Further, the growth of coherent instability can be attributed to the resonance observed between the cyclotron-resonant-excited wave and the background plasma oscillation. The particles can be injected into the closed-field line regions owing to magnetic reconnection near a light cylinder. These particles introduce a large amount of free energy that further causes cyclotron-resonant instability, which grows and amplifies radiative waves at frequencies close to the electron cyclotron harmonics that exhibit zebra-pattern-like spectral band structures. Further, these structures can be modulated by the resonance between the cyclotron-resonant-excited wave and the background plasma oscillation. In this scenario, the band structures of the Crab pulsar can be well fitted by a coherent instability model, where the plasma density of a light cylinder should be ~1013-15 cm−3, with an estimated gradient of >5:5 × 105 cm−4. This process may be accompanied by high-energy emissions. Similar phenomena are expected to be detected in other types of GP sources that have magnetic fields of ≃ 106 G in a light cylinder.

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Authors and Affiliations

  1. Key Laboratory for Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China

    WeiYang Wang & XueLei Chen

  2. University of Chinese Academy of Sciences, Beijing, 100049, China

    WeiYang Wang, SongBo Zhang & XueLei Chen

  3. School of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing, 100871, China

    WeiYang Wang & RenXin Xu

  4. National Astronomical Observatories, Chinese Academy of Sciences, Beijing, 100012, China

    JiGuang Lu

  5. Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Beijing, 100012, China

    JiGuang Lu

  6. Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, 210008, China

    SongBo Zhang

  7. CSIRO Astronomy and Space Science, Australia Telescope National Facility, Epping, NSW, 1710, Australia

    SongBo Zhang

  8. International Centre for Radio Astronomy Research, University of Western Australia, Crawley, WA, 6009, Australia

    SongBo Zhang

  9. Center for High Energy Physics, Peking University, Beijing, 100871, China

    XueLei Chen

  10. Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, 100871, China

    Rui Luo & RenXin Xu

  11. Department of Astronomy, School of Physics, Peking University, Beijing, 100871, China

    Rui Luo

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Wang, W., Lu, J., Zhang, S. et al. Pulsar giant pulse: Coherent instability near light cylinder. Sci. China Phys. Mech. Astron. 62, 979511 (2019). https://doi.org/10.1007/s11433-018-9334-y

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