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A possible mechanism for the pulsar radio emission

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Abstract

The possibility of radio emission is considered within a model which produces the beam-plasma system near the pulsar. A longitudinal instability develops near the light cylinder for a particular choice of parameters adopted in the paper. The excited wave strongly oscillates the beam particles perpendicular to its average velocity on one hand, and forms bunches of them on the other hand. Consequently, coherent radiation is expected. The frequency of the emission falls within the radio band, but the intensity turns out to be too low to explain observations. An appreciable enhancement of the beam number density over the Goldreich-Julian value (n b≃BΩ/2πec) is needed if the mechanism discussed in the present paper is responsible for the pulsar radio emission.

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Authors and Affiliations

  1. Dept. of Astronomy, Yale University, New Haven, Conn., USA

    Satoshi Hinata

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  1. Satoshi Hinata
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Hinata, S. A possible mechanism for the pulsar radio emission. Astrophys Space Sci 51, 303–318 (1977). https://doi.org/10.1007/BF00644154

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  • DOI: https://doi.org/10.1007/BF00644154

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