论文标题
UVBY，UBVRIJHK，SDSS UGRIZ，GAIA，KEPLER和TESS光度法系统的Power-2肢体系数
Power-2 limb-darkening coefficients for the uvby, UBVRIJHK, SDSS ugriz, Gaia, Kepler, and TESS photometric systems
论文作者
论文摘要
肢体变暗是一种重要的恒星现象，必须在恒星光谱，黯然失色的二进制，过境行星系统和微透明事件的研究中考虑。 Power-2肢体变形定律与出色的大气模型预测的特定强度相匹配：它比其他两参数定律更好，并且仅被四参数定律所超越。对Power-2定律的肢体变形系数的预测不广泛。因此，我们使用Atlas（平行）代码生成的出色气氛模型来计算它们。计算了空间任务Gaia，Kepler和Tess以及光度法系统UVBY，UBVRIJHK和SDSS UGRIZ的肢体变形系数。通过采用Levenberg-Marquardt最小化方法来进行计算，以最小化的方法进行了计算，并在100均等的Angles中进行了分辨率。我们使用了9586个模型气氛，覆盖19个金属性，有效温度为3500至50000 K，log G值从0.0到5.0，以及0、1、2、4和8 km的微涡轮速度。我们比其他两参数法律证实了Power-2法律的优越性。这与广泛使用的二次定律特别相关。在需要两参数法的情况下，我们建议使用Power-2法律。
Limb darkening is an important stellar phenomenon and must be accounted for in the study of stellar spectra, eclipsing binaries, transiting planetary systems, and microlensing events. The power-2 limb-darkening law provides a good match to the specific intensities predicted by stellar atmosphere models: it is better than other two-parameter laws and is only surpassed by the four-parameter law. Predictions of the limb-darkening coefficients for the power-2 law are not widely available. We therefore compute them, using stellar atmosphere models generated by the ATLAS (plane-parallel) code. Limb-darkening coefficients were computed for the space missions Gaia, Kepler, and TESS as well as for the photometric systems uvby, UBVRIJHK, and SDSS ugriz.The calculations were performed by adopting the Levenberg-Marquardt least-squares minimisation method and were computed with a resolution of 100 equally spaced viewing angles. We used 9586 model atmospheres covering 19 metallicities, effective temperatures of 3500 to 50000 K, log g values from 0.0 to 5.0, and microturbulent velocities of 0, 1, 2, 4, and 8 km. We confirm the superiority of the power-2 law, in terms of the quality of the fits, over other two-parameter laws. This is particularly relevant for the quadratic law, which is widely used. We recommend the use of the power-2 law in cases where a two-parameter law is needed.
