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Relativistic Superfluid Models for Rotating Neutron Stars

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Physics of Neutron Star Interiors

Part of the book series: Lecture Notes in Physics ((LNP,volume 578))

Abstract

This article starts by providing an introductory overview of the theoretical mechanics of rotating neutron stars as developed to account for the frequency variations, and particularly the discontinuous glitches, observed in pulsars. The theory suggests, and the observations seem to confirm, that an essential role is played by the interaction between the solid crust and inner layers whose superfluid nature allows them to rotate independently. However many significant details remain to be clarified, even in much studied cases such as the Crab and Vela. The second part of this article is more technical, concentrating on just one of the many physical aspects that needs further development, namely the provision of a satisfactorily relativistic (local but not microscopic) treatment of the effects of the neutron superfluidity that is involved.

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  1. Observatoire de Paris, 92195, Meudon, France

    Brandon Carter

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  1. Brandon Carter
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  1. Fachbereich Physik, Universität Rostock, 18051, Rostock, Deutschland

    David Blaschke

  2. Institut de Physique Nuclaire, Groupe de Physique Theorique, 15, rue Georges Clemenceau, 91406, Orsay Cedex, France

    Armen Sedrakian

  3. Institute for Nuclear and Particle Astrophysics Nuclear Science Division, Lawrence Berkeley National Lab., Berkeley, CA, 94720, USA

    Norman K. Glendenning

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Carter, B. (2001). Relativistic Superfluid Models for Rotating Neutron Stars. In: Blaschke, D., Sedrakian, A., Glendenning, N.K. (eds) Physics of Neutron Star Interiors. Lecture Notes in Physics, vol 578. Springer, Berlin, Heidelberg. https://doi.org/10.1007/3-540-44578-1_3

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