Transits of Known Planets Orbiting a Naked-eye Star
Transits of Known Planets Orbiting a Naked-eye Star
复制标题
DOI：
10.3847/1538-3881/aba835
复制
发表时间：
2020-07
期刊：
影响因子：
--
通讯作者：
S. Kane;Selccuk Yalccinkaya;H. Osborn;P. Dalba;L. Nielsen;A. Vanderburg;T. Movcnik;N. Hinkel
中科院分区：
文献类型：
--
作者：
S. Kane;Selccuk Yalccinkaya;H. Osborn;P. Dalba;L. Nielsen;A. Vanderburg;T. Movcnik;N. Hinkel
一些最具科学价值的凌日行星是那些已经从径向速度（RV）调查中知道的行星。这主要是因为它们的轨道有很好的特征，它们优先围绕RV调查目标的明亮恒星运行。凌日系外行星测量卫星（TESS）提供了一个机会，以系统的方式调查大多数已知的系外行星系统，以探测它们的行星可能的凌日。HD 136352 （Nu2 Lupi）是一颗裸眼（V = 5.78） g型主序恒星，通过RV高精度径向速度行星搜索器（HARPS）光谱仪的监测，发现它拥有三颗轨道周期分别为11.6、27.6和108.1天的行星。我们提出了HD 136352系统的两颗内行星的凌日探测和特征，分别揭示了行星b和c的R⊕和R⊕半径。我们将新的HARPS观测数据与来自Keck/高分辨率梯队光谱仪和英澳望远镜的RV数据以及来自12区的TESS光度测量相结合，对系统参数进行了完整的分析。综合数据分析得出行星b和c的体积密度分别为g cm−3和g cm−3，从而将它们放置在半径谷的两侧。多过境行星系统、明亮的主恒星以及行星内部和大气的多样性的结合，意味着它可能成为小世界大气和轨道特征的基石系统。
Some of the most scientifically valuable transiting planets are those that were already known from radial velocity (RV) surveys. This is primarily because their orbits are well characterized and they preferentially orbit bright stars that are the targets of RV surveys. The Transiting Exoplanet Survey Satellite (TESS) provides an opportunity to survey most of the known exoplanet systems in a systematic fashion to detect possible transits of their planets. HD 136352 (Nu2 Lupi) is a naked-eye (V = 5.78) G-type main-sequence star that was discovered to host three planets with orbital periods of 11.6, 27.6, and 108.1 days via RV monitoring with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph. We present the detection and characterization of transits for the two inner planets of the HD 136352 system, revealing radii of R⊕ and R⊕ for planets b and c, respectively. We combine new HARPS observations with RV data from the Keck/High Resolution Echelle Spectrometer and the Anglo-Australian Telescope, along with TESS photometry from Sector 12, to perform a complete analysis of the system parameters. The combined data analysis results in extracted bulk density values of g cm−3 and g cm−3 for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multitransiting planet system, the bright host star, and the diversity of planetary interiors and atmospheres means this will likely become a cornerstone system for atmospheric and orbital characterization of small worlds.