偏心双星V731造父变星的绝对尺寸和拱点运动
Absolute Dimensions and Apsidal Motion of the Eccentric Binary V731 Cephei
摘要：
对偏心双星V731 Cep的新的和现有的光度、光谱和空间分布数据进行了详细分析。利用互相关技术得到了该系统的光谱轨道根数。根据UBVRcIc光变曲线的视向速度解，V731 Cep由两颗质量为M $_{1}$ =2.577的主序星组成（0.098）M $_{\odot}$，M $_{2}$ =2.017（0.084）M $_{\odot}$，半径R $_{1}$ =1.823（0.030）R $_{\odot}$，R $_{2}$ =1.717（0.025）R $_{\odot}$，温度T $_{eff1}$ =10700（200）K，T $_{eff2}$ =9265（220）K，在倾角为88 $^{\circ}$ .70（0.03）的轨道上，彼此之间的距离为a=23.27（0.29）R $_{\odot}$。O-C残差的分析产生了一个相当长的拱点运动周期U=10000（2500）年相比，系统的观测历史。相对论对V731 Cep拱点运动观测率的贡献是显著的（76%）。系统的绝对尺寸和拱点运动特性的组合产生了与理论（log $\bar{k}_{2,theo}$ =-2.32）相一致的观测内部结构参数（log $\bar{k}_{2,obs}$ =-2.36）。通过两种方法（贝叶斯和进化轨迹）对该双星系统的演化研究表明，该系统的t= 1.33亿（26）万年，金属丰度为[M/H]=-0.04（0.02）dex。V731 Cep在空间分布和演化性质上与附近的疏散星团NGC 7762（$ρ\sim3^{\circ}$ .9）有相似之处，这表明V731 Cep可能是从NGC 7762蒸发出来的。
英文摘要：
A detailed analysis of new and existing photometric, spectroscopic and spatial distribution data of the eccentric binary V731 Cep was performed. Spectroscopic orbital elements of the system were obtained by means of cross-correlation technique. According to the solution of radial velocities with UBVRcIc light curves, V731 Cep consists of two main-sequence stars with masses M$_{1}$=2.577 (0.098) M$_{\odot}$, M$_{2}$=2.017 (0.084) M$_{\odot}$, radii R$_{1}$=1.823 (0.030) R$_{\odot}$, R$_{2}$=1.717 (0.025) R$_{\odot}$, and temperatures T$_{eff1}$=10700 (200) K, T$_{eff2}$=9265 (220) K separated from each other by a=23.27 (0.29) R$_{\odot}$ in an orbit with inclination of 88$^{\circ}$.70 (0.03). Analysis of the O--C residuals yielded a rather long apsidal motion period of U=10000(2500) yr compared to the observational history of the system. The relativistic contribution to the observed rates of apsidal motion for V731 Cep is significant (76%). The combination of the absolute dimensions and the apsidal motion properties of the system yielded consistent observed internal structure parameter (log$\bar{k}_{2,obs}$=-2.36) compared to the theory (log$\bar{k}_{2,theo}$=-2.32). Evolutionary investigation of the binary by two methods (Bayesian and evolutionary tracks) shows that the system is t=133(26) Myr old and has a metallicity of [M/H]=-0.04(0.02) dex. The similarities in the spatial distribution and evolutionary properties of V731 Cep with the nearby ($ρ\sim3^{\circ}$.9) open cluster NGC 7762 suggests that V731 Cep could have been evaporated from NGC 7762.
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