Static and dynamic spherical stellar atmospheres applied to optical interferometry

恒星的定量研究一直是天体物理学的主要成功之一，由于在成像恒星表面方面的变革性改进，测量恒星亮度到百万分之一，并确定恒星距离到1%，它正在过渡到更高的水平。为了解释这些数据，我们开发了一个强大的计算机程序来表示球状恒星大气，其特征是三个基本参数：光度、质量和半径。利用现有的光度和半径数据，我们能够得出单星的质量，这对恒星的年龄施加了有意义的限制。我们正在扩展这个计算机程序，将径向脉动纳入其中，以便将其应用于重要的造父变星，这对于测量银河系以外的距离是必不可少的。这些数值模型将使我们更深入地了解造父变星，并使我们能够调查我们之前的分析结果，即脉动驱动造父变星的质量，影响观测和我们对这些恒星生命历史的解释。

The quantitative study of stars has been one of the major successes of astrophysics, and it is transitioning to even higher levels thanks to tranformative improvements in imaging stellar surfaces, measuring stellar brightnesses to 1 part per million and determining stellar distances to a fraction of 1%. To interpret these data, we have developed a robust computer program to represent spherical stellar atmospheres characterized by their three fundamental parameters: luminosity, mass and radius. Using existing data for luminosities and radii, we are able to derive the masses of single stars, which puts meaningful limits on the star's age. We are extending this computer program to incorporate radial pulsation in order to apply it to the important Cepheid variable stars, which are essential for measuring distances beyond the Milky Way. These numerical models will give us a much deeper understanding of the Cepheid variables, as well as enabling us to investigate our previous analytic result that pulsation drives mass from Cepheids, affecting both the observations and our interpretation of the life histories of these stars.