New multicolour photometric observations were carried out on 22 nights in three observation missions between 2015 October and 2016 February 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 [2.372 2200(4) d] 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 Herzsprung–Russell (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.

中文翻译：

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食双星 HIP 7666 与 δ Scuti 脉动的光谱和光度分析

在 2015 年 10 月至 2016 年 2 月的三个观测任务中，在 22 个晚上进行了新的多色光度观测，以食双星 HIP 7666。还分别在 2015 年、2016 年和 2019 年冬季进行了高分辨率和低分辨率光谱观测. 给出了全相位覆盖的光变曲线和径向速度曲线。所有的光最小值都用于计算轨道周期 [2.372 2200(4) d] 和新星历。推导出光度解和恒星物理参数，表明HIP 7666是一个分离的双星，绝对参数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 初级, 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 对于次级。1.69 Gyr 和 1.755 Gyr 的年龄分别根据秒差等时线和台地演化轨迹估算。在 Herzsprung-Russell (H-R) 图中，主成分已演化到晚期，而次要成分仍位于主序列的早期。频率分析产生三个频率 f1 = 24.631(4) cd-1、f2 = 21.193(1) cd-1 和 f3 = 28.07(7) cd-1。模型和观察结果之间的比较表明，主要成分很可能是 p 模式非径向 δ Scuti 振荡器。而次要仍位于主序的早期阶段。频率分析产生三个频率 f1 = 24.631(4) cd-1、f2 = 21.193(1) cd-1 和 f3 = 28.07(7) cd-1。模型和观察结果之间的比较表明，主要成分很可能是 p 模式非径向 δ Scuti 振荡器。而次要仍位于主序的早期阶段。频率分析产生三个频率 f1 = 24.631(4) cd-1、f2 = 21.193(1) cd-1 和 f3 = 28.07(7) cd-1。模型和观察结果之间的比较表明，主要成分很可能是 p 模式非径向 δ Scuti 振荡器。