论文标题
绕着裸眼星的已知行星过渡
Transits of Known Planets Orbiting a Naked-Eye Star
论文作者
论文摘要
一些最有价值的过境行星是从径向速度（RV）调查中已经知道的行星。这主要是因为它们的轨道具有很好的特征，并且优先是轨道明亮的恒星，这是RV调查的目标。过渡系外行星调查卫星（{\ it 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，以检测其行星的可能过渡。 HD〜136352（NU $^2 $ 〜lupi）是裸眼（$ v = 5.78 $）G型主序列星，被发现可通过带有HARPS光谱图的RV监测来容纳三个行星，轨道时期为11.6、27.6和108.1天。我们介绍了HD〜136352系统的两个内部行星的过渡的检测和表征，显示半径为$ 1.482^{+0.058} _ { - 0.056} $〜$〜$〜$ r_ \ oplus $和$ 2.608^{+0.078} $ _ _ = $ 0.078} $ { - 0.077777} 分别。我们将新的HARPS观察与来自Keck/Hires和AAT的RV数据结合在一起，以及{\ it Tess}的光度法，以对系统参数进行完整的分析。合并的数据分析以$ρ_b= 7.8^{+1.2} _ { - 1.1} $ 〜gcm $^{ - 3} $和$ρ_c= 3.50^{+0.41} _ { - 0.41} _ { - 0.36} $ 〜gcm $^gcm^gcm^{-3.501} $ os in Planes in Planes of Planes of Planes in Splane for Planes b'{ - 0.36} $ 〜gcm $^gcm^gcm^{ - gcm^gcm^{ - gcm^gcm^{ - 3.501} $ for Planes in Planes in Splanes，山谷。多运输行星系统，明亮的宿主恒星以及行星内部和气氛的多样性的组合意味着这可能成为小世界大气和轨道表征的基石系统。
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 ({\it 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 (Nu$^2$~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 HARPS spectrograph. We present the detection and characterization of transits for the two inner planets of the HD~136352 system, revealing radii of $1.482^{+0.058}_{-0.056}$~$R_\oplus$ and $2.608^{+0.078}_{-0.077}$~$R_\oplus$ for planets b and c, respectively. We combine new HARPS observations with RV data from Keck/HIRES and the AAT, along with {\it 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 $ρ_b = 7.8^{+1.2}_{-1.1}$~gcm$^{-3}$ and $ρ_c = 3.50^{+0.41}_{-0.36}$~gcm$^{-3}$ for planets b and c, respectively, thus placing them on either side of the radius valley. The combination of the multi-transiting 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.
