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Expected high-frequency radiation from the 1.5-ms pulsar

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Abstract

The 1.5-ms pulsar PSR1937 +214 has so far been observed only in the radio range1, and X-ray and γ-ray observations at energies of between ∼30 and 1,000 MeV have yielded only upper limits for the radiation flux1–3. An optical identification of the 1.5-ms pulsar has been proposed4, but this identification cannot yet be considered definite. Thus it is of great interest to determine in which spectral region the PSR1937 +214 pulsar shows a radiation maximum. Here I consider how the current pulsar theory answers this question, and show that the 1.5-ms pulsar should be an intense source of γ quanta with an energy of ∼1011 eV below which γ rays freely leave its magnetosphere. The flux of superhard γ quanta emitted by this pulsar may exceed, by an order of magnitude, the flux from the pulsar in the Crab Nebula.

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Authors and Affiliations

  1. Space Research Institute, USSR Academy of Sciences, Moscow, 117810, USSR

    V. V. Usov

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  1. V. V. Usov
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Usov, V. Expected high-frequency radiation from the 1.5-ms pulsar. Nature 305, 409–410 (1983). https://doi.org/10.1038/305409a0

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  • DOI: https://doi.org/10.1038/305409a0

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