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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PACINI, F. Energy Emission from a Neutron Star. Nature 216, 567–568 (1967). https://doi.org/10.1038/216567a0
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DOI: https://doi.org/10.1038/216567a0
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