This is a preview of subscription content, log in via an institution to check access.
Refernces
G. Domokos, M. M. Janson andS. Kövesi-Domokos: JHU preprint, to be published inNature.
F. Gürsey:Ann. of Phys.,23, 211 (1963). See alsoR. Penrose:Proc. Roy. Soc.,284 A, 204 (1965).
For a review see,e.g.,E. S. Abers andB. W. Lee:Phys. Rep.,9, 1 (1973). Unless otherwise stated we follow their notation with obvious modification in order to accommodate an arbitrary space-time metric.
B. K. Harrison, K. S. Thorne, M. Wakano andJ. A. Wheeler:Gravitational Theory and Gravitational Collapse, Chap. 3, 10 (Chicago, Ill., 1965).
Including the effects of internuclear forces will not qualitatively change our results. Nuclei will disappear at a lower density than that we have considered. This will have the effect of increasing the radius of our «core».
The Ricci scalar is not an additive quantity, of course, but this ansatz ensures that our eq. (3) yields the correct solution for φ in the region exterior to the star. See ref. (1).G. Domokos, M. M. Janson andS. Kövesi-Domokos: JHU preprint, to be published inNature.
Author information
Authors and Affiliations
Additional information
Research supported by the U.S. Energy Research and Development Administration under Contract No. E(11-1) 3285.
Rights and permissions
About this article
Cite this article
Janson, M.M. Spontaneous symmetry breaking in the interior of a neutron star. Lett. Nuovo Cimento 15, 231–234 (1976). https://doi.org/10.1007/BF02727661
Received:
Published:
Issue Date:
DOI: https://doi.org/10.1007/BF02727661