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Temperature effects in pulsating superfluid neutron stars

Elena M. Kantor1,2 and Mikhail E. Gusakov1

  • 1Ioffe Physical Technical Institute, Polytekhnicheskaya 26, 194021 St.-Petersburg, Russia
  • 2St.-Petersburg State Polytechnical University, Polytekhnicheskaya 29, 195251 St.-Petersburg, Russia

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Phys. Rev. D 83, 103008 – Published 26 May, 2011

DOI: https://doi.org/10.1103/PhysRevD.83.103008

Abstract

We study the effects of finite stellar temperatures on the oscillations of superfluid neutron stars. The importance of these effects is illustrated with a simple example of a radially pulsating general relativistic star. Two main effects are taken into account: (i) temperature dependence of the entrainment matrix and (ii) the variation of the size of superfluid region with temperature. Four models are considered, which include either one or both of these two effects. Pulsation spectra are calculated for these models, and asymptotes for eigenfrequencies at temperatures close to critical temperature of neutron superfluidity are derived. It is demonstrated that models that allow for the temperature effect (ii) but disregard the effect (i), yield unrealistic results. Eigenfunctions for the normal- and superfluid-type pulsations are analyzed. It is shown that superfluid pulsation modes practically do not appear at the neutron-star surface and, therefore, can hardly be observed by measuring the modulation of the electromagnetic radiation from the star. The e-folding times for damping of pulsations due to the shear viscosity and nonequilibrium modified Urca processes are calculated and their asymptotes at temperatures close to the neutron critical temperature, are obtained. It is demonstrated that superfluid pulsation modes are damped by 1–3 orders of magnitude faster than normal modes.

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Phys. Rev. D 83, 103008– Published 26 May, 2011
  • Received 18 February 2011

© 2011 American Physical Society

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