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Superfluidity in Neutron Star Matter

  • Umberto Lombardo
  • Hans-Josef Schulze
Chapter
Part of the Lecture Notes in Physics book series (LNP, volume 578)

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].

Keywords

Fermi Surface Nuclear Matter Neutron Matter Symmetric Nuclear Matter Interaction Kernel 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer-Verlag Berlin Heidelberg 2001

Authors and Affiliations

  • Umberto Lombardo
    • 1
  • Hans-Josef Schulze
    • 2
  1. 1.Dipartimento di FisicaUniversità di CataniaCataniaItaly
  2. 2.Departament d’Estructura i Constituents de la MatèriaUniversitat de BarcelonaBarcelonaSpain

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