Chapter

Physics of Neutron Star Interiors

Volume 578 of the series Lecture Notes in Physics pp 30-53

Date:

Superfluidity in Neutron Star Matter

  • Umberto LombardoAffiliated withDipartimento di Fisica, Università di Catania
  • , Hans-Josef SchulzeAffiliated withDepartament d’Estructura i Constituents de la Matèria, Universitat de Barcelona

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Abstract

The research on the superfluidity of neutron matter can be traced back to Migdal’s observation that neutron stars are good candidates for being macroscopic superfluid systems [1]. And, in fact, during more than two decades of neutron-star physics the presence of neutron and proton superfluid phases has been invoked to explain the dynamical and thermal evolution of a neutron star. The most striking evidence is given by post-glitch timing observations [2],[3], but also the cooling history is strongly influenced by the possible presence of super- fluid phases [4],[5]. On the theoretical side, the onset of superfluidity in neutron matter or in the more general context of nuclear matter was investigated soon after the formulation of the Bardeen, Cooper, and Schrieffer (BCS) theory of superconductivity [6] and the pairing theory in atomic nuclei [7],[8].