2005/02/28 by M. E. Gusakov, D. G. Yakovlev, O. Y. Gnedin · 1 citation
Engineering · Physics and Astronomy · #Astrophysical Phenomena and Observations #Geophysics and Sensor Technology #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2005.09295.x
published as Mon.Not.Roy.Astron.Soc.361:1415,2005 · 10 pages, 3 figures, an important reference to the paper by Finzi & Wolf (1968) is added; analytical consideration of the problem (Section 5) is essentially extended
openalex publication_date 2005/08/03 · arxiv created 2005/08/04 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We have derived a set of equations to describe the thermal evolution of a neutron star which undergoes small-amplitude radial pulsations. We have taken into account, within the framework of the general theory of relativity, the pulsation damping due to the bulk and shear viscosity and the accompanying heating of the star. The neutrino emission of a pulsating non-superfluid star and its heating due to the bulk viscosity are calculated assuming that both processes are determined by the non-equilibrium modified Urca process. Analytical and numerical solutions to the set of equations of the stellar evolution are obtained for linear and strongly non-linear deviations from beta-equilibrium. It is shown that a pulsating star may be heated to very high temperatures, while the pulsations damp very slowly with time as long as the damping is determined by the bulk viscosity (a power-law damping over 100–1000 yr). The contribution of the shear viscosity to the damping becomes important in a rather cool star with a low pulsation energy.