Skip to content
BY-NC-ND 3.0 license Open Access Published by De Gruyter June 2, 2014

Zur Theorie der Neutronensterne

P. Gombás and D. Kisdi

Using a semi-empirical theory of interaction between neutrons in atomic nuclei, the average energy of a neutron, the equation of state, and the pressure-compressibility relation is computed for a neutron gas of very high density (n ≈ 1015 gcm-3). The results are applied to the computation of the mass and the radius of a neutron star as a function of the central density. For the critical mass, above which a neutron star cannot exist, a value of 0.96 solar masses is found.

Received: 1966-2-23
Published Online: 2014-6-2
Published in Print: 1966-12-1

© 1946 – 2014: Verlag der Zeitschrift für Naturforschung

This work is licensed under the Creative Commons Attribution-NonCommercial-NoDerivatives 3.0 License.

Scroll Up Arrow