Spectroscopic eclipse mapping of mass-accreting Algol-type stars with pulsating components

我们想利用高分辨光谱的时间序列来研究具有脉动分量的质量吸积的大陵型系统。从分析光谱线轮廓的变化观察到的整个轨道周期，包括日食，我们要提取的信息，全球恒星参数的组件，以及对脉动的原色。我们希望建立一个代码，计算合成恒星线轮廓的食双星观察光盘集成光。恒星参数将通过调整相应的模型参数，如旋转速度、旋转和轨道轴倾角、恒星半径、边缘变暗和恒星大气参数来得出，以适应观测。在食期间，大陵型系统的脉动分量表现出非径向脉动模的振幅和相位调制。这些调制是由于遮蔽分量引起的屏蔽效应。我们的方法使用光谱线的全部信息内容来模拟这种筛选。我们希望将非径向脉动模式的计算包括到我们的模型中，并尝试将其用于通过日食映射进行模式识别。结果将与恒星的地震模型进行比较。

We want to investigate mass-accreting Algol-type systems with pulsating components by using time series of high-resolution spectra. From the analysis of spectral line profile variations observed over the full orbital period including eclipses we want to extract information on global stellar parameters of the components as well as on the pulsations of the primaries. We want to establish a code that computes synthetic stellar line profiles of eclipsing binaries observed in disk-integrated light. Stellar parameters will be derived by adjusting the corresponding model parameters like rotation velocity, inclinations of rotation and orbital axes, stellar radii, limb darkening, and parameters of the stellar atmospheres to fit the observations. During eclipses, the pulsating components of Algol-type systems show amplitude and phase modulations of the non-radial pulsation modes. These modulations are due to the screening effect caused by the eclipsing component. Our method models this screening using the full information content of spectral lines. We want to include the calculation of non-radial pulsation modes into our model and try to use it for a mode identification by eclipse mapping. Results will be compared to seismologic models of the stars.