Letter | Published:

Energy Emission from a Neutron Star

Naturevolume 216pages567568 (1967) | Download Citation



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.

Access optionsAccess options

Rent or Buy article

Get time limited or full article access on ReadCube.


All prices are NET prices.


  1. 1

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

  2. 2

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

  3. 3

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

  4. 4

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

  5. 5

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

  6. 6

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

Download references

Author information


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

    • F. PACINI


  1. Search for F. PACINI in:

About this article

Publication history


Issue Date



Further reading


By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.