被忽略的近接触双星Cl* Melotte 111 AV 1224的光度和光谱观测
Photometric and spectroscopic observations of the neglected near-contact binary Cl* Melotte 111 AV 1224
摘要：
本文对短周期双星Cl ~*~Melotte~111~AV~1224进行了光度学和光谱学研究。在2014年至2017年的三次观测运行中获得的$B$，$V$和$R$通带的测量结果以及2014年获得的中等分辨率光谱，与SuperWASP和LAMOST项目的公共数据一起进行了分析。我们的光变曲线显示出明显的不对称性和可变的O 'Connell效应。SuperWASP测光被用来推导一个平均的0.345225天的双周期。对$(O-C)$图的分析表明，轨道周期以$dP/dt = -3.87 \times 10^{-6}$天/年的速率减小，这可能是由质量较大的组分向质量较小的组分的质量转移引起的。该系统被发现是一个单线光谱二进制与系统速度，$γ= 1 \pm 3$ Km s $^{-1}$，和半振幅，K $_{1}$ = 21 $\pm$ 5 Km s $^{-1}$。初步估计其光谱分类和有效温度分别为K 0 VPDMATHABMU 1和PDMATHABMVK。光度和光谱解表明Cl ~*~Melotte~111~AV~1224是一个低质量比（$q=m_{2}/m_{1} \sim 0.11$）、低倾角（$\sim ~ 38^{\circ}$）的近接触体系。主星和伴星的质量、半径和光度分别估计为$1.02 \pm 0.06\, M_\odot$、$1.23 \pm 0.05\, R_\odot $、$1.01 \pm 0.06\, L_\odot$和$0.11 \pm 0.08\, M_\odot$、$0.45 \pm 0.05\, R_\odot$、$0.10 \pm 0.06\, L_\odot$。边缘接触，加上周期的减少，这表明该二元系统可能是在一个关键的演化阶段，预测的热弛豫振荡理论。
英文摘要：
This paper presents a photometric and spectroscopic study of the short-period binary star Cl*~Melotte~111~AV~1224. Measurements in the $B$, $V$, and $R$ passbands obtained during three observing runs between 2014 and 2017 and medium-resolution spectra secured in 2014, are analyzed together with public data from the SuperWASP and LAMOST projects. Our light curves show marked asymmetry with a variable O'Connell effect. The SuperWASP photometry is used to derive a mean binary period of 0.345225 days. The analysis of the $(O-C)$ diagram reveals that the orbital period is decreasing at a rate of $dP/dt = -3.87 \times 10^{-6}$ days yr$^{-1}$, which may be caused by mass transfer from the more-massive component to the less-massive one. The system is found to be a single-lined spectroscopic binary with a systemic velocity, $γ= 1 \pm 3$ Km s$^{-1}$, and a semi-amplitude, K$_{1}$ = 21 $\pm$ 5 Km s$^{-1}$. The spectral classification and the effective temperature of the primary component are estimated to be K0V $\pm$ 1 and $5200 \pm 150$ K, respectively. The photometric and spectroscopic solutions reveal that Cl*~Melotte~111~AV~1224 is a low-mass ratio ($q=m_{2}/m_{1} \sim 0.11$), low-inclination ($\sim ~ 38^{\circ}$) near-contact system. The masses, radii and luminosity for the primary and secondary are estimated to be $1.02 \pm 0.06\, M_\odot$, $1.23 \pm 0.05\, R_\odot $, $1.01 \pm 0.06\, L_\odot$ and $0.11 \pm 0.08\, M_\odot$, $0.45 \pm 0.05\, R_\odot$, $0.10 \pm 0.06\, L_\odot$, respectively. The marginal contact, together with the period decrease, suggests that this binary system may be at a key evolutionary stage, as predicted by the theory of thermal relaxation oscillations.
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