论文标题
旋转的巨大行星三人旋转的星星高清184010
A Trio of Giant Planets Orbiting Evolved Star HD 184010
论文作者
论文摘要
我们报告了围绕进化的Star HD 184010（HR 7421，HIP 96016）的三重巨型行星系统的发现。这一发现基于冈山星球搜索计划的观察结果，这是一项精确的径向速度调查，在2004年4月至6月之间在冈山天体物理天文台进行了。恒星是K0类型，位于红色巨型分支的开头。 It has a mass of $1.35_{-0.21}^{+0.19} M_{\odot}$, a radius of $4.86_{-0.49}^{+0.55} R_{\odot}$, and a surface gravity $\log g$ of $3.18_{-0.07}^{+0.08}$.行星系统由三个巨型配置中的三个巨型行星组成：行星的最低质量为$ m _ {\ rm {b}} \ sin i = 0.31 _ { - 0.04}^{+0.04}^{+0.03} m _ { 0.30 _ { - 0.05}^{+0.04} m _ {\ rm {j}} $，和$ m _ {\ rm {d}} \ sin i = 0.45 _ { - 0.45 _ { - 0.06}^{+0.04}^{+0.04} M _ {美元$ p _ {\ rm {d}} = 836.4 _ { - 8.4}^{+8.4} \ \ \ rm {d} $，它们源自三组射击辐射速度数据。轨道周期的比率接近$ p _ {\ rm {d}}：p _ {\ rm {c}}}：p _ {\ rm {b}} \ sim 21：12：7 $，这意味着邻近行星之间的周期比均低于$ 2：$ 2：1 $ $。动态稳定性分析表明，行星应具有近圆形轨道。该系统可以在1 GYR上保持稳定，从共同计划轨道，低偏心率（$ e = 0.05 $）和等于从最佳拟合圆形轨道拟合中得出的最小质量的行星质量初始化。此外，行星不太可能具有平均运动共振。 HD 184010系统是唯一的：它是第一个发现具有高度进化的星（$ \ log g <3.5 $ cgs）和两个以上的巨型行星的系统，它们均具有中间轨道周期（$ 10^2 \ \ \ \ \ rm {d} <p <p <10^3^3 \ \ \ \ rm {d} $）。
We report the discovery of a triple-giant-planet system around an evolved star HD 184010 (HR 7421, HIP 96016). This discovery is based on observations from Okayama Planet Search Program, a precise radial velocity survey, undertaken at Okayama Astrophysical Observatory between 2004 April and 2021 June. The star is K0 type and located at beginning of the red-giant branch. It has a mass of $1.35_{-0.21}^{+0.19} M_{\odot}$, a radius of $4.86_{-0.49}^{+0.55} R_{\odot}$, and a surface gravity $\log g$ of $3.18_{-0.07}^{+0.08}$. The planetary system is composed of three giant planets in a compact configuration: The planets have minimum masses of $M_{\rm{b}}\sin i = 0.31_{-0.04}^{+0.03} M_{\rm{J}}$, $M_{\rm{c}}\sin i = 0.30_{-0.05}^{+0.04} M_{\rm{J}}$, and $M_{\rm{d}}\sin i = 0.45_{-0.06}^{+0.04} M_{\rm{J}}$, and orbital periods of $P_{\rm{b}}=286.6_{-0.7}^{+2.4}\ \rm{d}$, $P_{\rm{c}}=484.3_{-3.5}^{+5.5}\ \rm{d}$, and $P_{\rm{d}}=836.4_{-8.4}^{+8.4}\ \rm{d}$, respectively, which are derived from a triple Keplerian orbital fit to three sets of radial velocity data. The ratio of orbital periods are close to $P_{\rm{d}}:P_{\rm{c}}:P_{\rm{b}} \sim 21:12:7$, which means the period ratios between neighboring planets are both lower than $2:1$. The dynamical stability analysis reveals that the planets should have near-circular orbits. The system could remain stable over 1 Gyr, initialized from co-planar orbits, low eccentricities ($e=0.05$), and planet masses equal to the minimum mass derived from the best-fit circular orbit fitting. Besides, the planets are not likely in mean motion resonance. HD 184010 system is unique: it is the first system discovered to have a highly evolved star ($\log g < 3.5$ cgs) and more than two giant planets all with intermediate orbital periods ($10^2\ \rm{d} < P < 10^3\ \rm{d}$).
