论文标题
从苔丝和开普勒的光线曲线的肢体变暗测量
Limb darkening measurements from TESS and Kepler light curves of transiting exoplanets
论文作者
论文摘要
不准确的肢体镶嵌模型可能是分析传播系外行星和黯然失色的二进制恒星系统的光曲线的重要误差源。为了测试已发表的肢体变形模型的准确性，我将恒星大气模型预测的肢体变形曲线与从开普勒和蒂斯任务观察到的过境外部超球体系统中的43个FGK型恒星的高质量光曲线测得的肢体变形曲线。比较使用参数进行$ h^{\ prime} _1 =i_λ（\ frac {2} {3} {3}）$和$ h^{\ prime} _2 = h^{\ prime} _1 -i_λ（\ frac {\ frac {1} {1} {3} {3} {3} {3} {3}）视线与表面正常矢量之间的角度的余弦。这些参数直接解释和对计算方式的细节不敏感。我发现，大多数（但不是全部）肢体变形数据的列表与观察到的$ h^{\ prime} _1 $和$ h^{\ prime} _2 $的观察值非常吻合。与观察到的值归因于平均垂直磁场强度的效果相比，有一个很小但显着的偏移$ΔH^{\ prime} _1 \约0.006 $，大约归因于这些不活跃的太阳能星星的照片中预期的g，g，g，但对于典型的典型构成典型的恒星模型而言，这并没有考虑到这些不活跃的太阳能型星星。简要讨论了这些结果对通过柏拉图任务测量的行星半径精确的含义。
Inaccurate limb-darkening models can be a significant source of error in the analysis of the light curves for transiting exoplanet and eclipsing binary star systems. To test the accuracy of published limb-darkening models, I have compared limb-darkening profiles predicted by stellar atmosphere models to the limb-darkening profiles measured from high-quality light curves of 43 FGK-type stars in transiting exoplanet systems observed by the Kepler and TESS missions. The comparison is done using the parameters $h^{\prime}_1 = I_λ(\frac{2}{3})$ and $h^{\prime}_2 = h^{\prime}_1 - I_λ(\frac{1}{3})$, where $I_λ(μ)$ is the specific intensity emitted in the direction $μ$, the cosine of the angle between the line of sight and the surface normal vector. These parameters are straightforward to interpret and insensitive to the details of how they are computed. I find that most (but not all) tabulations of limb-darkening data agree well with the observed values of $h^{\prime}_1$ and $h^{\prime}_2$. There is a small but significant offset $Δh^{\prime}_1 \approx 0.006$ compared to the observed values that can be ascribed to the effect of a mean vertical magnetic field strength $\approx 100$\,G that is expected in the photospheres of these inactive solar-type stars but that is not accounted for by typical stellar model atmospheres. The implications of these results for the precision of planetary radii measured by the PLATO mission are discussed briefly.
