Gravitational radiation back-reaction from f-modes on neutron stars
Gravitational radiation back-reaction from f-modes on neutron stars
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DOI：
10.1093/mnras/stac009
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发表时间：
2021-09
期刊：
影响因子：
--
通讯作者：
G. Yim;D. Jones
中科院分区：
文献类型：
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作者：
G. Yim;D. Jones
中子星星基模振荡的引力辐射阻尼问题一直受到人们的关注。许多研究都着眼于快速旋转恒星中这种振荡的稳定性，计算模式振幅的增长/衰减率。本文研究了相对被忽视的辐射反应对星星自旋的影响。我们非常专注于所谓的开尔文模式：（最初）非旋转不可压缩恒星的振荡模式。我们发现了一个意想不到的结果，即在一个初始不旋转的星星上激发一个角动量$\delta J$的模式，最终辐射出一个角动量$2 \delta J$到无穷大，使星星本身的角动量为$-\delta J$。这一结果本身就很有趣，而且如果这种模式被激发，也会对自旋下降的中子星的角动量预算产生影响。
The problem of the gravitational radiation damping of neutron star fundamental ($f$) 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 $\delta J$ on an initially non-rotating star ends up radiating an angular momentum $2 \delta J$ to infinity, leaving the star itself with a bulk angular momentum of $-\delta J$. 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.