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Quasinormal modes of superfluid neutron stars

L. Gualtieri1, E. M. Kantor2, M. E. Gusakov2,3, and A. I. Chugunov2

  • 1Dipartimento di Fisica, “Sapienza” Università di Roma and Sezione INFN Roma1, Piazzale Aldo Moro 5, 00185, Roma, Italy
  • 2Ioffe Physical-Technical Institute of the Russian Academy of Sciences, Polytekhnicheskaya 26, 194021 Saint-Petersburg, Russia
  • 3Saint-Petersburg State Polytechnical University, Polytekhnicheskaya 29, 195251 Saint-Petersburg, Russia

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Phys. Rev. D 90, 024010 – Published 2 July, 2014

DOI: https://doi.org/10.1103/PhysRevD.90.024010

Abstract

We study nonradial oscillations of neutron stars with superfluid baryons, in a general relativistic framework, including finite temperature effects. Using a perturbative approach, we derive the equations describing stellar oscillations, which we solve by numerical integration, employing different models of nucleon superfluidity, and determining frequencies and gravitational damping times of the quasinormal modes. As expected by previous results, we find two classes of modes, associated to superfluid and non-superfluid degrees of freedom, respectively. We study the temperature dependence of the modes, finding that at specific values of the temperature, the frequencies of the two classes of quasinormal modes show avoided crossings, and their damping times become comparable. We also show that, when the temperature is not close to the avoided crossings, the frequencies of the modes can be accurately computed by neglecting the coupling between normal and superfluid degrees of freedom. Our results have potential implications on the gravitational wave emission from neutron stars.

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Phys. Rev. D 90, 024010– Published 2 July, 2014
  • Received 1 May 2014

© 2014 American Physical Society

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