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Radial oscillations of viscous stars at finite temperature

Amanda Guerrieri1,*, Gabriel S. Rocha2,†, Gabriel S. Denicol2,‡, and Raissa F. P. Mendes2,1,§

  • *Contact author: amguerrieri@cbpf.br
  • †Contact author: gabrielsr@id.uff.br
  • ‡Contact author: gsdenicol@id.uff.br
  • §Contact author: rfpmendes@id.uff.br
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Phys. Rev. D 114, 083054 – Published 29 October, 2026

DOI: https://doi.org/10.1103/1qmk-yr46

Abstract

We study the radial oscillation spectrum of relativistic stars within Israel-Stewart and Navier-Stokes theories, extending previous analyses to include heat diffusion and a thermodynamically consistent finite-temperature equation of state. The inclusion of heat flux gives rise to a distinct thermal sector in the mode spectrum, whose structure closely mirrors the dispersion relations of an infinite dissipative fluid. Within Israel-Stewart theory, the thermal modes transition from purely damped to propagating behavior above a critical overtone number, providing a finite-size realization of relativistic second sound in compact stars. Remarkably, the finite stellar geometry can push even the fundamental thermal mode into the propagating regime—a feature with no continuum analogue. For the class of equations of state considered here, where finite-temperature corrections enter as controlled, Sommerfeld-type perturbations of a cold polytrope, the thermal sector couples only weakly to the ordinary fluid oscillation spectrum, with the coupling being of second order in a suitable temperature parameter. We further show that the discrete stellar spectrum is well captured by an analytic ansatz constructed from the flat-spacetime dispersion relations, with the star’s finite radius discretizing the continuous mode structure. Our results complete the analysis of radial oscillations of viscous stars by incorporating the last remaining dissipative degree of freedom within the Israel-Stewart framework.

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Phys. Rev. D 114, 083054– Published 29 October, 2026
  • Received 1 July 2026
  • Accepted 29 September 2026
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