Letter | Published:

Energy Emission from a Neutron Star

Naturevolume 216pages567568 (1967) | Download Citation

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Abstract

ALTHOUGH there are still many problems concerning the supernovae, there is little doubt that a very dense stellar core has to be left behind after the explosion (at least in some cases). During the contraction of this core, inverse β reactions take place and transform most of the nuclei and electrons into neutrons. If the mass of the neutron star does not exceed a critical value of about one or two solar masses, a stable equilibrium situation can be reached with the gas pressure balancing the gravitational force.

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References

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    Chau, W. Y., Ap. J., 147, 664 (1967).

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    Woltjer, L., Ap. J., 140, 1309 (1964).

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    Spitzer, L., Electromagnetic Phenomena in Cosmical Physics, Inter. Astro. Union Symposium (1958).

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    Hoyle, F., Narlikar, J., and Wheeler, J. A., Nature, 203, 914 (1964)

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    Landau, L. D., Lifshitz, E. M., in Theory of Fields, second ed. (Addison Wesley, Reading, Mass., 1962).

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    Woltjer, L., in Lectures on High Energy Astrophysics (in the press).

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Affiliations

  1. Center for Radiophysics and Space Research, Cornell University, New York

    • F. PACINI

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DOI

https://doi.org/10.1038/216567a0

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