Gravitational radiation back-reaction from f-modes on neutron stars
arXiv:2109.05076 · doi:10.1093/mnras/stac009
Abstract
The problem of the gravitational radiation damping of neutron star fundamental () mode oscillations has received considerable attention. Many studies have looked at the stability of such oscillations in rapidly rotating stars, calculating the growth/decay rate of the mode amplitude. In this paper, we look at the relatively neglected problem of the radiation reaction on the spin of the star. We specialise greatly to the so-called Kelvin modes: the modes of oscillation of (initially) non-rotating incompressible stars. We find the unexpected result that the excitation of a mode of angular momentum on an initially non-rotating star ends up radiating an angular momentum to infinity, leaving the star itself with a bulk angular momentum of . This result is interesting in itself, and also will have implications for the angular momentum budgets of spinning down neutron stars, should such modes be excited.
arXiv comment18 pages, 1 figure, 2 appendices. Paragraph added to the end of Section 6. Accepted for publication in MNRAS
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