论文标题
黯然失色的二进制恒星的基本有效温度测量。
Fundamental effective temperature measurements for eclipsing binary stars I. Development of the method and application to AI Phoenicis
论文作者
论文摘要
需要进行准确，精确的有效温度（T $ _ {\ rm eff} $）测量的星星来测试出色的气氛模型并校准经验方法以确定T $ _ {\ rm eff} $。目前，很少有标准恒星用于校准矮星的温度指标。盖亚（Gaia）的视频现在使许多矮人星星在剥落二进制方面的许多矮星，从原则上使t $ _ {\ rm eff} $进行测量。我们旨在开发一种使用高精度测量的方法，可用于脱落的二进制恒星，Gaia视差和多波长光度法，以获得准确，精确的基本有效温度，可用于建立一组基准星星。我们选择良好的二进制AI腓尼基进行测试，因为它具有非常精确的绝对参数和广泛的档案光度法。该方法使用恒星半径和视差将恒星用于蚀二进制。我们使用贝叶斯方法从观察到的幅度，颜色和通量比从两颗恒星中获取两颗恒星的集成侧磁通量。 F7V组件的AI Phoenicis两星的基本有效温度为$ 6199 \ pm22 $ k，K0IV组件的基本有效温度为$ 5094 \ pm16 $ k。通量量表中的零点错误导致T $ _ {\ rm eff} $中的系统错误仅为0.2％（$ \ $ \ $ 11K）。我们发现，这些结果与分析细节（例如模型光谱的选择）相对可靠。我们的方法可以应用于在一定范围的波长范围内用半径，视差和光度测量的黯然失色的二进制恒星。用这种方法确定的具有基本有效温度的恒星可以在未来的调查中用作基准。
Stars with accurate and precise effective temperature (T$_{\rm eff}$) measurements are needed to test stellar atmosphere models and calibrate empirical methods to determine T$_{\rm eff}$. There are few standard stars currently available to calibrate temperature indicators for dwarf stars. Gaia parallaxes now make it possible, in principle, to measure T$_{\rm eff}$ for many dwarf stars in eclipsing binaries. We aim to develop a method that uses high-precision measurements of detached eclipsing binary stars, Gaia parallaxes and multi-wavelength photometry to obtain accurate and precise fundamental effective temperatures that can be used to establish a set of benchmark stars. We select the well-studied binary AI Phoenicis to test our method, since it has very precise absolute parameters and extensive archival photometry. The method uses the stellar radii and parallax for stars in eclipsing binaries. We use a Bayesian approach to obtain the integrated bolometric fluxes for the two stars from observed magnitudes, colours and flux ratios. The fundamental effective temperature of two stars in AI Phoenicis are $6199\pm22$ K for the F7V component and $5094\pm16$ K for the K0IV component. The zero-point error in the flux scale leads to a systematic error of only 0.2% ($\approx$ 11K) in T$_{\rm eff}$. We find that these results are robust against the details of the analysis, such as the choice of model spectra. Our method can be applied to eclipsing binary stars with radius, parallax and photometric measurements across a range of wavelengths. Stars with fundamental effective temperatures determined with this method can be used as benchmarks in future surveys.
