Effect of viscosity and thermal conductivity on the radial oscillation and relaxation of relativistic stars

Abstract

In this paper we present a generic formulation of the linearized dynamical equations governing small adiabatic radial oscillations of relativistic stars. The dynamical equations are derived by taking into consideration those effects of viscosity and thermal conductivity of neutron-star matter which directly determine the minimum period of observable pulsars. A variational principle is applied to determine a discrete set of eigenfunctions with complex eigenvalues. The real and imaginary parts of eigenvalues represent the squared natural frequencies and relaxation time of radial oscillations of non-rotating neutron stars, respectively. We provide a suitable framework which may be supplemented with various potential species of cold-nuclear-matter models to compute the spectra of the normalized eigenfrequencies with a certain numerical precision. In the last section, we provide a qualitative estimation of the rate at which viscosity and thermal conductivity drain the kinetic energy of radial oscillation mode in reasonably uniform neutron stars, without relying on explicit numerical computations.

References in corpus (5)

• Analytical study of anisotropic compact star models
• Shear viscosity in neutron star cores
• Reaction rates and transport in neutron stars
• Gravitational waves from f-modes excited by the inspiral of highly eccentric neutron star binaries
• Relativistic Lagrangian displacement field and tensor perturbations

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• Testing a nonlinear solution of the Israel-Stewart theory