论文标题
Coralie radial-velocity搜索周围进化的恒星（级联）III的同伴。新的木星主机明星：使用苔丝数据对HD 29399进行深入分析
Coralie radial-velocity search for companions around evolved stars (CASCADES) III. A new Jupiter host-star: in-depth analysis of HD 29399 using TESS data
论文作者
论文摘要
语境。增加检测到的系外行星的数量远非轶事，尤其是对于需要长时间观察持续时间的长期行星。更多的检测意味着更好地理解系外行星种群的统计特性，其宿主恒星的详细建模还可以详细讨论星空星际相互作用和行星系统的轨道演变。目标。在发现新的行星系统的背景下，我们旨在通过径向速度测量值，宿主星的地震表征以及对系统的轨道演化进行建模，对HD 29399及其伴侣进行完整的研究。方法。作为Cascades调查的一部分，在位于La Silla天文台（智利）的1.2-M瑞士望远镜上安装的Coralie光谱仪获得了高清29399的高分辨率光谱。我们使用互相关函数曲线的矩以及恒星作为诊断的光度变异性来区分恒星和行星诱导的信号。为了建模宿主星，我们将正向建模与全球和局部最小化方法和反转技术相结合。我们还研究了在动态和平衡潮汐的影响下研究系统的轨道历史。结果。我们提出了对长期巨型行星的检测。将这些测量结果与苔丝的光度观察结合在一起，我们能够彻底建模宿主恒星并研究系统的轨道演化。我们得出了$ 1.17 \ pm 0.10〜m _ {\ odot} $和$ 1.59 \ pm 0.08〜m_ {jup} $的恒星和行星质量，分别为6.2 Gyr。我们表明，动态和平衡潮没有能够影响地球的轨道演变。此外，没有预测系统进化的预测。
Context. Increasing the number of detected exoplanets is far from anecdotal, especially for long-period planets that require a long duration of observation. More detections imply a better understanding of the statistical properties of exoplanet populations, and detailed modelling of their host stars also enables thorough discussions of star-planet interactions and orbital evolution of planetary systems. Aims. In the context of the discovery of a new planetary system, we aim to perform a complete study of HD 29399 and its companion by means of radial-velocity measurements, seismic characterisation of the host-star, and modelling of the orbital evolution of the system. Methods. High-resolution spectra of HD 29399 were acquired with the CORALIE spectrograph mounted on the 1.2- m Swiss telescope located at La Silla Observatory (Chile) as part of the CASCADES survey. We used the moments of the cross-correlation function profile as well as the photometric variability of the star as diagnostics to distinguish between stellar and planetary-induced signals. To model the host star we combined forward modelling with global and local minimisation approaches and inversion techniques. We also studied the orbital history of the system under the effects of both dynamical and equilibrium tides. Results. We present the detection of a long-period giant planet. Combining these measurements with photometric observations by TESS, we are able to thoroughly model the host star and study the orbital evolution of the system. We derive stellar and planetary masses of $1.17 \pm 0.10~ M_{\odot}$ and $1.59 \pm 0.08 ~M_{Jup}$, respectively, and an age for the system of 6.2 Gyr. We show that neither dynamical nor equilibrium tides have been able to affect the orbital evolution of the planet. Moreover, no engulfment is predicted for the future evolution of the system.
