论文标题
AI腓尼基的苔丝光曲线
The TESS light curve of AI Phoenicis
论文作者
论文摘要
从观察到脱落的二进制恒星的观察结果中得出的正常恒星的准确质量和半径对于测试恒星模型至关重要，如果质量和半径足够精确且准确，则可能对校准这些模型中的自由参数有用。我们旨在测量明亮黯淡的二进制AI PHE中恒星的精确质量和半径，并量化这些估计值中系统误差的水平。我们使用几种不同的方法对AI PHE的苔丝光曲线进行建模，并结合来自多个来源的光谱轨道，以估算出恒星质量和半径，以及强大的误差估计。我们发现，不同方法在光曲线分析方面的一致性非常好，但是有些方法低估了模型参数的错误。源自现代梯形光谱仪获得的光谱轨道的半光谱轨道的半扩张量与0.1％以内一致。 AI PHE中的星星为$ m_1 = 1.1938 \ pm 0.0008 m _ {\ odot} $和$ m_2 = 1.2438 \ pm 0.0008m _ {\ odot} $，radii是$ r_1 = 1.8050 = 1.8050 \ pm 0.0022 r __2 = $ __2 0.0023 r _ {\ odot} $。我们得出的结论是，使用现代棘轮光谱仪获得的苔丝和光谱的光度法，可以测量明亮黯淡的二进制恒星中恒星的准确质量和半径。我们为在此精确度上发表束缚二进制恒星的质量和半径提供了建议。
Accurate masses and radii for normal stars derived from observations of detached eclipsing binary stars are of fundamental importance for testing stellar models and may be useful for calibrating free parameters in these model if the masses and radii are sufficiently precise and accurate. We aim to measure precise masses and radii for the stars in the bright eclipsing binary AI Phe, and to quantify the level of systematic error in these estimates. We use several different methods to model the TESS light curve of AI Phe combined with spectroscopic orbits from multiple sources to estimate precisely the stellar masses and radii together with robust error estimates. We find that the agreement between different methods for the light curve analysis is very good but some methods underestimate the errors on the model parameters. The semi-amplitudes of the spectroscopic orbits derived from spectra obtained with modern echelle spectrographs are consistent to within 0.1%. The masses of the stars in AI Phe are $M_1 = 1.1938 \pm 0.0008 M_{\odot}$ and $M_2 = 1.2438 \pm 0.0008M_{\odot}$, and the radii are $R_1 = 1.8050 \pm 0.0022 R_{\odot}$ and $R_2 = 2.9332 \pm 0.0023 R_{\odot}$. We conclude that it is possible to measure accurate masses and radii for stars in bright eclipsing binary stars to a precision of 0.2% or better using photometry from TESS and spectroscopy obtained with modern echelle spectrographs. We provide recommendations for publishing masses and radii of eclipsing binary stars at this level of precision.
