The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component
The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component
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DOI：
10.1017/pasa.2012.016
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发表时间：
2012-10
影响因子：
6.3
通讯作者：
H. A. Dal;E. Si̇pahi̇
中科院分区：
文献类型：
--
作者：
H. A. Dal;E. Si̇pahi̇
本文结合模型和BVRI光变曲线的分析结果，讨论了V1464 Aql的性质。分析表明，系统的质量比为q = 0.71 ± 0.02，系统倾角（i）为38°.45 ± 0°.22。取主成分温度为7420 ± 192 K，则副成分温度为6232 ± 161 K。第一部分的质量为1.74 ± 0.05 M，第二部分的质量为1.23 ± 0.01 M。发现主要组件的半径为2.10 ± 0.05 R，而次级组件的半径为1.80 ± 0.01 R。揭示了系统不应该出现任何食，我们证明了大幅度的主要变化应该是由于椭球效应造成的。事实上，傅立叶分析也支持这一结果。在文献中，我们第一次揭示了它的主要组成部分是一颗盾牌座δ星星。BVRI带的搏动周期分别为58.482 ± 0.002、58.482 ± 0.001、60.966 ± 0.002和60.964 ± 0.003分钟。我们在log（P orb）-log（P pulse）平面中绘制V1464 Aql。使用超过160个二进制，其一个或两个组件是脉动的，我们得出了一个新的线性拟合在日志（P orb）日志（P脉冲）平面的每种类型的二进制。利用各组的线性拟合，我们得到了不同类型脉动星的log（P orb）和log（P pulse）之间的新刻度。此外，还首次对光谱类型为O和B的脉动星进行了校准。V1464 Aql似乎位于其他椭球和密近双星附近。因此，我们将V1464 Aql列为一个新的候选者，可能是包含盾牌座δ的椭球变星。
Abstract Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component’s temperature as 7420 ± 192 K, we found that the temperature of the secondary is 6232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M⊙, while it is 1.23 ± 0.01 M⊙ for the secondary. The primary component’s radius was found to be 2.10 ± 0.05 R⊙, while it was found as 1.80 ± 0.01 R⊙ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log (P orb)–log (P pulse) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb)–log (P pulse) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb) and log (P pulse) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.