标题： V455 Car：三合星系统中振荡掩食型Algol型双星 显示英文标题

标题： V455 Car: an oscillating eclipsing Algol-type binary in triple star system

摘要： 半人马座V455是一个南方振荡食甚型密近三星系统，轨道周期为5.132888天。 我们基于凌星系外行星巡天卫星的第一批测光解显示它是一个半分离的双星系统，次级星几乎充满其洛希瓣。 光变曲线中显著的奥康奈尔效应可以通过初级分量上的热点来解释，这可能是由于次级分量到初级分量的质量转移。 绝对参数确定为：对于初级星为$M_{1} = 5.30 \pm 1.10 \, \rm M_{\odot}$, $R_{1} = 3.17 \pm 0.22 \, \rm R_{\odot}$；对于次级星为$M_{2} = 1.58 \pm 0.32 \, \rm M_{\odot}$, $R_{2} = 6.66 \pm 0.46 \, \rm R_{\odot}$。 \textbf{基于$O-C$分析，我们发现了一个$P_3=26.62(\pm1.66)\,yr$的周期性变化。 这种周期性振荡表明可能存在一个最小质量为$0.59(\pm0.13)\,\rm M_{\odot}$的第三天体。}。 推测次级星经历了更长的演化过程，导致双星系统中经历了一个质量比反转。 我们的频率分析发现，半人马座V455的初级星可能是一颗SPB/SLF星。 本研究报道了一个振荡食甚型半人马座V455三星系统的新型实例，该系统具有SPB/SLF初级星和红巨星，表明大质量双星中存在大量第三体的观测结果强有力。 显示英文摘要

摘要： V455 Car is a southern oscillating eclipsing Algol-type system with an orbital period of 5.132888 days. Our first photometric solutions based on the Transiting Exoplanet Survey Satellite indicate that it is a semi-detached binary with the secondary star is almost filling its Roche lobe. The noticeable O'Connell effect in light curve could be explained by hot spot on the primary component, which may be attributed to the mass transfer from the secondary component to the primary one. The absolute parameters are determined as: $M_{1} = 5.30 \pm 1.10 \, \rm M_{\odot}$, $R_{1} = 3.17 \pm 0.22 \, \rm R_{\odot}$ for the primary, and $M_{2} = 1.58 \pm 0.32 \, \rm M_{\odot}$, $R_{2} = 6.66 \pm 0.46 \, \rm R_{\odot}$ for the secondary. \textbf{Based on $O-C$ analysis, we find a periodic variation of $P_3=26.62(\pm1.66)\,yr$. The periodic oscillation suggests a possible third body with a minimal mass of $0.59(\pm0.13)\,\rm M_{\odot}$}. It is speculated that the secondary star has undergone a longer evolution, leading to a mass ratio reversal being experienced in the binary system. Our frequency analysis finds that the primary of V455 Car may be an SPB/SLF star. This study reports a novel example of an oscillating eclipsing Algol-type system featuring an SPB/SLF primary star and a red giant star, which suggest that strong observational results for a high incidence of third bodies in massive binaries.