AI 中文总结
该研究首次全面分析分离食双星V0757 Pup，确认其主星为γ Doradus型脉动星，测定恒星参数、脉动特性等，未发现第三体伴星，所得距离与Gaia DR3结果吻合
AI 中文摘要
分离食双星（EA）系统中的脉动星可提供诸多重要物理信息，用于约束恒星结构与演化理论。迄今为止，在食双星系统中发现的γ Doradus（GDOR）星不足50颗，使其成为研究恒星内部g模式脉动的重要目标。我们对V0757 Pup（TIC 6939791）开展了全面的物理与脉动分析，该天体是经TESS任务（扇区7、34、61、88）观测、并通过泰国国家望远镜地基光谱观测跟进的分离食双星系统。结合光变曲线建模与中分辨率光谱推导的视向速度，我们高精度确定了恒星基本结构与大气参数：该系统包含一颗F2V型主星（质量M₁=1.305±0.026M☉，半径R₁=1.643±0.020R☉）与一颗G1V型伴星（质量M₂=0.934±0.030M☉，半径R₂=0.941±0.079R☉）。我们对残差光变曲线进行了详细的频率分析，识别出两个独立的主导脉动频率，分别为f≈0.79 c/d与0.98 c/d；结合推导的脉动常数Q≈0.6 d，确认主星为γ Doradus型脉动星。食甚时间变化（ETV）分析显示，现有数据集未探测到第三体伴星，该结果得到Gaia天体测量分析的支持。演化建模表明该系统年龄约2.2 Gyr，主星预计将在约1 Gyr后充满洛希瓣。此外，我们基于轨道与SED建模计算得到距离d≈350 pc，与Gaia DR3视差距离高度吻合。
英文摘要
Pulsating stars in detached eclipsing binary (EA) systems are known for providing many important physical informations which constrain both stellar structure and evolution theories. To date, fewer than 50 $γ$ Doradus (GDOR) stars have been found in eclipsing binary systems, making them important targets to study \textit{g}-mode pulsation inside the stars. We present a comprehensive physical and pulsational analysis of V0757 Pup (TIC 6939791), a detached eclipsing binary system observed by the TESS mission (Sectors 7, 34, 61, and 88) and followed up with ground-based spectroscopy from the Thai National Telescope. By combining light curve modeling with radial velocities derived from medium-resolution spectra, we determined the fundamental stellar and atmospheric parameters with high precision. The system consists of an F2V primary ($M_1=1.305\pm0.026M_\odot, R_1=1.643\pm0.020R_\odot$) and a G1V secondary ($M_2=0.934\pm0.030M_\odot, R_2=0.941\pm0.079R_\odot$). We performed a detailed frequency analysis of the residual light curves, identifying two dominant independent pulsation frequencies at $f\sim0.79$ c/d and $0.98$ c/d. These frequencies, along with the derived pulsation constant ($Q\sim0.6$ d), confirm the primary component as a $γ$ Doradus pulsator. An analysis of Eclipse Timing Variations (ETV) reveals non detection of third body companions with current available dataset, strengthen by the result of \textit{Gaia} astrometric analysis. Evolutionary modeling indicates the system is $\sim2.2$ Gyr old, with the primary expected to fill its Roche lobe in $\sim1$ Gyr. Additionally, we calculate a distance of $d\approx350$ pc based on orbital and SED modeling, which is in excellent agreement with the \textit{Gaia} DR3 parallax distance.
Comments22 pages, 15 figures, submitted to PASJ. Comments are welcome
