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Tidally induced stellar oscillations: converting modelled oscillations excited by hot Jupiters into observables
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2020-10-30 , DOI: 10.1093/mnras/staa3394
Andrew Bunting 1 , Caroline Terquem 1, 2
Affiliation  

We calculate the conversion from non-adiabatic, non-radial oscillations tidally induced by a hot Jupiter on a star to observable spectroscopic and photometric signals. Models with both frozen convection and an approximation for a perturbation to the convective flux are discussed. Observables are calculated for some real planetary systems to give specific predictions. Time-dependent line broadening and the radial velocity signal during transit are both investigated as methods to provide further insight into the nature of the stellar oscillations. The photometric signal is predicted to be proportional to the inverse square of the orbital period, $P^{-2}$, as in the equilibrium tide approximation. However, the radial velocity signal is predicted to be proportional to $ P^{-1}$, and is therefore much larger at long orbital periods than the signal corresponding to the equilibrium tide approximation, which is proportional to $P^{-3}$. The prospects for detecting these oscillations and the implications for the detection and characterisation of planets are discussed.

中文翻译:

潮汐引起的恒星振荡:将热木星激发的模拟振荡转换为可观测的

我们计算了从恒星上的热木星潮汐引起的非绝热、非径向振荡到可观测的光谱和光度信号的转换。讨论了具有冻结对流和对流扰动近似值的模型。为一些真实的行星系统计算可观测值以给出具体的预测。随时间变化的谱线加宽和凌日过程中的径向速度信号都被研究作为进一步了解恒星振荡本质的方法。光度信号预计与轨道周期的平方反比成正比,$P^{-2}$,如在平衡潮汐近似中。然而,径向速度信号预计与$P^{-1}$成正比,因此,在长轨道周期中,它比对应于平衡潮汐近似值的信号大得多,后者与 $P^{-3}$ 成正比。讨论了探测这些振荡的前景以及对行星探测和表征的影响。
更新日期:2020-10-30
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