Spectroscopic and photometric analysis of the eclipsing binary HIP 7666 with δ Scuti pulsations
Spectroscopic and photometric analysis of the eclipsing binary HIP 7666 with δ Scuti pulsations
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对具有 δ Scuti 脉动的食双星 HIP 7666 进行光谱和光度分析
DOI：
10.1093/mnras/stab2063
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发表时间：
2021-07
影响因子：
4.8
通讯作者：
Ma Lu
中科院分区：
文献类型：
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作者：
Feng Guojie;Esamdin Ali;Fu Jianning;Zhang Yanping;Niu Hubiao;Li Chunqian;Liu Nian;Cang Tianqi;Michel Raul;Fox Machado Lester;Wang Liang;Pi Qingfeng;Bai Chunhai;Xu Jing;Isk;ar Abdusamatjan;Zeng Xiangyun;Ma Lu
2015年10月至2016年2月，在三次观测任务中，对食双星HIP 7666的22个夜晚进行了新的多色光度观测。2015年冬季、2016年冬季和2019年冬季也分别进行了高分辨率和低分辨率的光谱观测。给出了全位相覆盖的光速曲线和径向速度曲线。所有的光极小时间都被用来计算轨道周期(2.3722200(4)天)和新的星历。得到了HIP7666的光度解和恒星物理参数，表明HIP7666是一个绝对参数为M1=1.53(3)M⊙，r1=2.08(2)R⊙，logL1/L⊙=0.99(3)，logG1=3.98(2)，mbol1=2.26(8)，Tef，1=7100(100)K，M2=1.23(3)M⊙，R2=1.06(2)R⊙，logL2/L⊙=0.13(4)的分离双星。次要的Log G2=4.47(2)，Mbol2=4.4(1)，Tef，2=6029(67)K。根据帕尔秒等时线和台地演化轨迹分别估计了1.69亿年和1.755年的年龄。在H-R图上，主组分已演化到晚期，次生组分仍处于主层序的早期阶段。频率分析得到f1=24.631(4)Cd−1，f2=21.193(1)Cd−1和f3=28.07(7)Cd−1的三个频率。模型和观测之间的比较表明，主要成分最有可能是p模非径向δ刀尖振荡器。
New multi-color photometric observations were carried out on 22 nights in three observation missions between Oct. 2015 and Feb. 2016 for eclipsing binary HIP 7666. High- and low-resolution spectroscopic observations were also carried out in the winters of 2015, 2016, and 2019, respectively. The fully phase-covered light curves and radial velocity curves are presented. All times of light minima are used to calculate the orbital period (2.3722200(4) days) and new ephemerides. The photometric solution and stellar physical parameters are derived, showing that HIP 7666 is a detached binary with the absolute parameters M1 = 1.53(3) M⊙, R1 = 2.08(2) R⊙, log L1/L⊙ = 0.99(3), log g1 = 3.98(2), Mbol1 = 2.26(8), Teff, 1 = 7100(100) K for the primary, and M2 = 1.23(3) M⊙, R2 = 1.06(2) R⊙, log L2/L⊙ = 0.13(4), log g2 = 4.47(2), Mbol2 = 4.4(1), Teff, 2 = 6029(67) K for the secondary. The age of 1.69 Gyr and 1.755 Gyr are estimated from PARSEC isochrones and MESA evolutionary tracks, respectively. In H-R diagram, the primary component has evolved to the late stages, while the secondary still locates at the early stages of the main sequence. Frequency analysis yields three frequencies of f1 = 24.631(4) cd−1, f2 = 21.193(1) cd−1, and f3 = 28.07(7) cd−1. Comparisons between models and observations suggest that the primary component is most likely a p-mode non-radial δ Scuti oscillator.