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This book presents a study of the saturation of unstable f-modes
(fundamental modes) due to low-order nonlinear mode coupling. Since
their theoretical prediction in 1934, neutron stars have remained
among the most challenging objects in the Universe. Gravitational
waves emitted by unstable neutron star oscillations can be used to
obtain information about their inner structure, that is, the
equation of state of dense nuclear matter. After its initial growth
phase, the instability is expected to saturate due to nonlinear
effects. The saturation amplitude of the unstable mode determines
the detectability of the generated gravitational-wave signal, but
also affects the evolution of the neutron star. The study shows
that the unstable (parent) mode resonantly couples to pairs of
stable (daughter) modes, which drain the parent's energy and make
it saturate via a mechanism called parametric resonance
instability. Further, it calculates the saturation amplitude of the
most unstable f-mode multipoles throughout their so-called
instability windows.
This book presents a study of the saturation of unstable f-modes
(fundamental modes) due to low-order nonlinear mode coupling. Since
their theoretical prediction in 1934, neutron stars have remained
among the most challenging objects in the Universe. Gravitational
waves emitted by unstable neutron star oscillations can be used to
obtain information about their inner structure, that is, the
equation of state of dense nuclear matter. After its initial growth
phase, the instability is expected to saturate due to nonlinear
effects. The saturation amplitude of the unstable mode determines
the detectability of the generated gravitational-wave signal, but
also affects the evolution of the neutron star. The study shows
that the unstable (parent) mode resonantly couples to pairs of
stable (daughter) modes, which drain the parent's energy and make
it saturate via a mechanism called parametric resonance
instability. Further, it calculates the saturation amplitude of the
most unstable f-mode multipoles throughout their so-called
instability windows.
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