具有脉动分量的南方食系统的综合分析：HM、V632 Sco和TT Vel的实例
Comprehensive analysis of southern eclipsing systems with pulsating components: The cases of HM Pup, V632 Sco and TT Vel
摘要：
这项工作提出了一个广泛的分析性质的三个南方半分离食双星托管的脉动分量，即HM Pup，V632斯科，TT Vel。系统的多重过滤光度观测主要是在2018-2021年间使用位于澳大利亚和智利的望远镜获得的。这些观测结果与凌日系外行星勘测卫星（TESS）的数据相结合，对脉动进行了详细分析。光谱类型和径向速度是由澳大利亚国立大学的2.3米望远镜和宽视场摄谱仪获得的光谱确定的。对数据进行建模，并导出所有组件的绝对参数。光变曲线残差进一步分析，使用傅立叶变换技术的脉动频率的测定。使用理论模型，最可能的模式的主振荡也确定。还对所有系统的轨道周期变化进行了分析，并提出了最有可能的轨道周期调制机制。这些系统的物理性质与其他类似的情况进行了比较，其组件的位置绘制在M-R和HR图。最后，脉动性能的振荡组件进行比较，目前已知的系统中的这种类型的轨道脉动周期和日志g脉动周期图。根据定义，这些系统被确定为oEA星，其主星是$δ$ Scuti型的脉动星，而在它们的Na I D光谱中存在来自演化的次级成分的质量流的证据。
英文摘要：
This work presents an extensive analysis of the properties of three southern semi-detached eclipsing binaries hosting a pulsating component, namely HM Pup, V632 Sco, and TT Vel. Systematic multi-filtered photometric observations were obtained using telescopes located in Australia and Chile mostly between 2018-2021. These observations were combined with data from the Transiting Exoplanet Survey Satellite (TESS) mission for a detailed analysis of pulsations. Spectral types and radial velocities were determined from spectra obtained with the Australian National University's 2.3 m telescope and Wide Field Spectrograph. The data are modelled and the absolute parameters of all components are derived. The light curve residuals are further analysed using Fourier transformation techniques for the determination of the pulsation frequencies. Using theoretical models, the most probable modes of the principal oscillations are also identified. Eclipse-timing variation analysis is also made for all systems and the most likely mechanisms modulating the orbital period are proposed. The physical properties of these systems are compared with other similar cases and the locations of their components are plotted in the M-R and HR diagrams. Finally, the pulsational properties of the oscillating components are compared with currently known systems of this type within the orbital-pulsation period and log g-pulsation period diagrams. These systems are identified as oEA stars by definition, with the primaries to be pulsating stars of $δ$ Scuti type, while evidence of mass flow from the evolved secondary components is present in their Na I D spectra.
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