论文标题
在高质量的二进制系统VV Orionis中，β头球脉冲脉冲和变化的轨道倾斜度
A beta Cephei pulsator and a changing orbital inclination in the high-mass eclipsing binary system VV Orionis
论文作者
论文摘要
我们对基于苔丝卫星的光度法的高质量黯然失色的二进制系统VV ORI进行了分析。主恒星（B1V，9.5 MSUN）显示β头孢菌搏动，次级脉冲（B7V，3.8 MSUN）可能是一个缓慢的B恒星。我们检测到51个显着的振荡频率，包括两个相当于轨道频率的多个多重组，表明脉动潮湿。我们分析了苔丝光曲线和发表的径向速度，以确定系统的物理特性。这两颗恒星只是其脉动类型的第二种，具有精确的质量。目前，轨道倾斜度也正在减少，这可能是由于引力与第三身体的相互作用所致。
We present an analysis of the high-mass eclipsing binary system VV Ori based on photometry from the TESS satellite. The primary star (B1V, 9.5 Msun) shows beta Cephei pulsations and the secondary (B7V, 3.8 Msun) is possibly a slowly-pulsating B star. We detect 51 significant oscillation frequencies, including two multiplets with separations equal to the orbital frequency, indicating that the pulsations are tidally perturbed. We analyse the TESS light curve and published radial velocities to determine the physical properties of the system. Both stars are only the second of their pulsation type with a precisely-measured mass. The orbital inclination is also currently decreasing, likely due to gravitational interactions with a third body.
