Inertial modes of neutron stars with a superfluid core

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14 Citations (Scopus)

Abstract

We investigate the modal properties of inertial modes of rotating neutron stars with a core filled with neutron and proton superfluids, taking account of entrainment effects between the superfluids. In this paper, the entrainment effects are modelled by introducing a parameter 77 so that there is no entrainment state at η = 0. We find that inertial modes of rotating neutron stars with a superfluid core are split into two families, which we call ordinary fluid inertial modes (i-modes) and superfluid inertial modes (i s-modes). The two superfluids in the core counter-move for the i s-modes. For the i0-modes, K0 = lim Ω→0 ω/Ω is only weakly dependent on the entrainment parameter η, where Ω and ω are the angular frequency of rotation and the oscillation frequency observed in the corotating frame of the star, respectively. For the ismodes, on the other hand, |K0| increases almost linearly as η increases. Avoided crossings as functions of η are therefore quite common between i- and i s-modes. We find that some of the is-modes that are unstable against the gravitational radiation reaction at η = 0 become stable when η is larger than ηcrit. the value of which depends on the mode. Since the radiation-driven instability associated with the current multipole radiation is quite weak for the inertial modes and the mutual friction damping in the superfluid core is strong, the instability caused by the inertial modes will be easily suppressed unless the entrainment parameter η is extremely small and the mutual friction damping is sufficiently weak.

Original languageEnglish
Pages (from-to)207-222
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume344
Issue number1
DOIs
Publication statusPublished - 2003 Sep 1

Keywords

  • Instabilities
  • Stars: Neutron
  • Stars: Oscillations
  • Stars: Rotation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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