Energy Emission from a Neutron Star

Details Energy Emission from a Neutron Star Energy Emission from a Neutron Star

Nov 1967

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1967natur.216..567p&link_type=abstract

Nature, Volume 216, Issue 5115, pp. 567-568 (1967).

Physics

226

Scientific paper

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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