标题： KIC 10080943：一个包含两个压力模和重力模双模式脉动星的偏心双星系统 显示英文标题

标题： KIC 10080943: An eccentric binary system containing two pressure- and gravity-mode hybrid pulsators

摘要： γ杜鹃座型和δ天琴座型变星覆盖了低质量和大质量主序星之间的过渡区域，因此对于检验恒星模型至关重要。当它们处于双星系统中时，我们可以结合两种独立的方法来推导出关键信息，例如精确的基本参数以辅助恒星地震学建模。在开普勒光变曲线中，KIC10080943目标已经发现了重力模式和压力模式脉动的清晰特征。地面光谱观测揭示了该目标是一个双线谱联星系统。我们展示了对四年开普勒测光数据和高分辨率光谱数据的分析，以得出可用于评估中间质量恒星结构与演化理论预测的观测限制。我们使用光谱分解方法确定了两颗恒星的大气参数，并推导出行星轨道要素。通过PHOEBE软件，我们模拟了光变曲线中双星的椭圆度变化和反射信号，并利用经典的傅里叶技术分析了脉动模式。我们表明，双曲线偏心率系统KIC10080943包含两颗质量分别为$M_1=2.0\pm0.1~M_\odot$和$M_2=1.9\pm0.1~M_\odot$的混合脉动变星，半径分别为$R_1=2.9\pm0.1~R_\odot$和$R_2=2.1\pm0.2~R_\odot$。我们检测到两颗恒星的g模和p模中存在旋转分裂现象，并用这些数据初步估算两颗恒星的核心到表面自转速率，未来更详细的恒星地震学建模将改进这一估算结果。 显示英文摘要

摘要： Gamma Doradus and delta Scuti pulsators cover the transition region between low mass and massive main-sequence stars, and as such, are critical for testing stellar models. When they reside in binary systems, we can combine two independent methods to derive critical information, such as precise fundamental parameters to aid asteroseismic modelling. In the Kepler light curve of KIC10080943, clear signatures of gravity- and pressure-mode pulsations have been found. Ground-based spectroscopy revealed this target to be a double-lined binary system. We present the analysis of four years of Kepler photometry and high-resolution spectroscopy to derive observational constraints with which to evaluate theoretical predictions of the stellar structure and evolution for intermediate-mass stars. We used the method of spectral disentangling to determine atmospheric parameters for both components and derive the orbital elements. With PHOEBE, we modelled the ellipsoidal variation and reflection signal of the binary in the light curve and used classical Fourier techniques to analyse the pulsation modes. We show that the eccentric binary system KIC10080943 contains two hybrid pulsators with masses $M_1=2.0\pm0.1~M_\odot$ and $M_2=1.9\pm0.1~M_\odot$, with radii $R_1=2.9\pm0.1~R_\odot$ and $R_2=2.1\pm0.2~R_\odot$. We detect rotational splitting in the g modes and p modes for both stars and use them to determine a first rough estimate of the core-to-surface rotation rates for the two components, which will be improved by future detailed seismic modelling.