食双星再讨论。第十八篇：F型系统OO Pegasi
Rediscussion of eclipsing binaries. Paper XVIII. The F-type system OO Pegasi
AI总结：
本文基于TESS光变曲线和已发表光谱数据重新分析分离食双星OO Peg，测定两子星质量与半径，发现主星更热更大更亮但质量略低，并给出与Gaia DR3一致的距离，未探测到脉动。
摘要：
OO Peg是一个分离食双星系统，包含两颗晚A型恒星，处于周期为2.985天的圆轨道上。利用已发表的光谱结果和来自凌星系外行星巡天卫星（TESS）的光变曲线，我们测定它们的质量分别为1.69 ± 0.09和1.74 ± 0.06太阳质量，半径分别为2.12 ± 0.03和1.91 ± 0.03太阳半径。TESS数据质量很高，但来自两个来源的视向速度存在差异，妨碍了精确的质量测量。主星明确比伴星更热、更大、更亮，但其质量较低（尽管显著性仅为1.1σ）。利用已发表的视星等和温度，我们得出距离为238.8 ± 6.1秒差距，与Gaia DR3视差一致。尽管两颗子星都位于盾牌座δ型不稳定带内，我们没有发现脉动的证据。需要更广泛的光谱观测来增进我们对该系统的理解。
英文摘要：
OO Peg is a detached eclipsing binary system containing two late-A-type stars in a circular orbit with a period of 2.985 d. Using published spectroscopic results and a light curve from the Transiting Exoplanet Survey Satellite (TESS) we determine their masses to be 1.69 +/- 0.09 and 1.74 +/- 0.06 Msun, and their radii to be 2.12 +/- 0.03 and 1.91 +/- 0.03 Rsun. The TESS data are of high quality, but discrepancies in the radial velocities from two sources prevent a precise mass measurement. The primary star is definitively hotter, larger and more luminous than its companion, but its mass is lower (albeit to a significance of only 1.1 sigma). Using published apparent magnitudes and temperatures, we find a distance of 238.8 +/- 6.1 pc, in agreement with the Gaia DR3 parallax. Although both components are in the delta Scuti instability strip, we find no evidence of pulsations. More extensive spectroscopy is needed to improve our understanding of the system.
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