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Superfluidity and Superconductivity in Neutron Stars

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Abstract

Neutron stars, the compact stellar remnants of core-collapse supernova explosions, are unique cosmic laboratories for exploring novel phases of matter under extreme conditions. In particular, the occurrence of superfluidity and superconductivity in neutron stars will be briefly reviewed.

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Notes

  1. The high temperatures \({\sim }10^7\) K prevailing in neutron star interiors prevent the formation of electron pairs recalling that the highest critical temperatures of terrestrial superconductors do not exceed \({\sim }200\) K. In particular, iron expected to be present in the outermost layers of a neutron star was found to be superconducting in 2001, but with a critical temperature \(T_{\mathrm{c}}\simeq 2\) K (Shimizu et al. 2001). See also Ginzburg (1969).

  2. A given channel is denoted by \(^{2S+1}L_J\), where J is the total angular momentum, L is the orbital angular momentum, and S the spin of nucleon pair.

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Acknowledgements

This work has been supported by the Fonds de la Recherche Scientifique – FNRS (Belgium) under grant n\(^\circ \) CDR J.0187.16, and by the European Cooperation in Science and Technology (COST) action MP1304 NewCompStar.

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    N. Chamel

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Chamel, N. Superfluidity and Superconductivity in Neutron Stars. J Astrophys Astron 38, 43 (2017). https://doi.org/10.1007/s12036-017-9470-9

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