Rotational modes of nonisentropic stars and the gravitational radiation-driven instability

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Abstract

Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan; yoshida@astr.tohoku.ac.jp, lee@astr.tohoku.ac.jp We investigate the properties of the r-mode and the inertial mode of slowly rotating, nonisentropic, Newtonian stars by taking account of the effects of the Coriolis force and the centrifugal force. The Coriolis force is the dominant restoring force for both the r-mode and the inertial mode, which are also called the rotational mode in this paper. For the velocity field produced by the oscillation modes the r-mode has the dominant toroidal component over the spheroidal component, while the inertial mode has the comparable toroidal and spheroidal components. In nonisentropic stars the specific entropy of the fluid depends on the radial distance from the center, and the interior structure is in general divided into two kinds of layers of fluid stratification that are stable or unstable against convection. Because of the nonisentropic structure, low-frequency oscillations of the star are affected by the buoyant force, which has no effects on oscillations of isentropic stars. In this paper we employ simple polytropic models with the polytropic index n = 1 as the background neutron star models for the modal analysis. For the nonisentropic models we consider only two cases, that is, the models with the stable fluid stratification in the whole interior and the models that are fully convective. For simplicity we call these two kinds of models "radiative" and "convective" in this paper. For both cases, we assume that the deviation of the models from isentropic structure is small. Examining the dissipation timescales due to the gravitational radiation and several viscous processes for the polytropic neutron star models, we find that the gravitational radiation-driven instability of the nodeless r-modes associated with l′ = |m| remains strong even in the nonisentropic models, where l′ and m are the indices of the spherical harmonic function representing the angular dependence of the eigenfunction. Calculating the rotational modes of the radiative models as functions of the angular rotation frequency Ω, we find that the inertial modes are strongly modified by the buoyant force at small Ω, where the buoyant force as a dominant restoring force becomes comparable to or stronger than the Coriolis force. Because of this property, we obtain the mode sequences in which the inertial modes at large Ω are identified as g-modes or the r-modes with l′ = |m| at small Ω. We also note that as Ω increases from Ω = 0 the retrograde g-modes become retrograde inertial modes, which are unstable against the gravitational radiation reaction.

Original languageEnglish
Pages (from-to)353-366
Number of pages14
JournalAstrophysical Journal, Supplement Series
Volume129
Issue number1
DOIs
Publication statusPublished - 2000 Jul 1

Keywords

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

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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