Saturation of the f-mode instability in neutron stars: I. Theoretical framework

Pantelis Pnigouras; Kostas D. Kokkotas

doi:10.1103/physrevd.92.084018

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arXiv · 1509.01453

Saturation of the f-mode instability in neutron stars: I. Theoretical framework

Pantelis Pnigouras·Kostas D. Kokkotas

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Abstract

The basic formulation describing quadratic mode coupling in rotating Newtonian stars is presented, focusing on polar modes. Due to the Chandrasekhar-Friedman-Schutz mechanism, the f-mode (fundamental oscillation) is driven unstable by the emission of gravitational waves. If the star falls inside the so-called instability window, the mode's amplitude grows exponentially, until it is halted by nonlinear effects. Quadratic perturbations form three-mode networks inside the star, which evolve as coupled oscillators, exchanging energy. Coupling of the unstable f-mode to other (stable) modes can lead to a parametric resonance and the subsequent saturation of its amplitude, thus suppressing the instability. The saturation point determines the amplitude of the gravitational-wave signal obtained from an individual source, as well as the evolutionary path of the latter inside the instability window.

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Pantelis Pnigouras, Kostas D. Kokkotas. 2015-12-27. Saturation of the f-mode instability in neutron stars: I. Theoretical framework. https://doi.org/10.1103/physrevd.92.084018

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