Superfluidity in Neutron Stars

Details Superfluidity in Neutron Stars Superfluidity in Neutron Stars

Nov 1969

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1969natur.224..673b&link_type=abstract

Nature, Volume 224, Issue 5220, pp. 673-674 (1969).

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232

Scientific paper

MATTER in the interior of a typical neutron star is a mixture of three degenerate interacting quantum liquids-neutrons, protons and electrons, the latter two having a density at most a few per cent that of the neutrons1. The mixture, bounded on the inside by a superdense core of hadrons, muons and so on, and most likely by a solid mantle on the outside2, is of density between 5 × 1013 and 1015 g cm-3. As was first pointed out by Migdal3, and more recently discussed by others4-8, there are quite possibly superfluid states in this interior. Here we discuss certain general features of such states and the extent to which they influence the properties of the star.

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