V1464 Aql的性质：一个新的具有δ Scuti分量的椭球变星
The Nature of V1464 Aql: A New Ellipsoidal Variable with a Delta Scuti Component
摘要：
考虑到从模型和BVRI光变曲线的分析所获得的结果，我们讨论了V1464 Aql的性质。分析表明，系统的质量比为q=0.71（0.02），系统倾角为38.45（0.22）°。取第一组分的温度为7420（192）K，得到第二组分的温度为6232（161）K。主成分的质量为1.74（0.05）Msun，而副成分的质量为1.23（0.01）Msun。发现初级组件的半径为2.10（0.05）Rsun，而次级组件的半径为1.80（0.01）Rsun。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。在BVRI带中，脉冲周期分别为58.482（0.002）、58.482（0.001）、60.966（0.002）、60.964（0.003）分钟。我们在log（Porb）-log（Ppulse）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平面上的日志（Porb）日志（Ppulse）的每一个类型的二进制。利用各组的线性拟合，我们得到了不同类型脉动星的log（Porb）和log（Ppulse）之间的新刻度。此外，还首次获得了O型和B型脉动星的刻度。V1464 Aql似乎位于其他椭球和密近双星附近。因此，我们将V1464 Aql列为具有盾牌座δ分量的椭球变星的新候选者。
英文摘要：
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) deg. 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) Msun, while it is 1.23(0.01) Msun for the secondary. The primary component's radius was found to be 2.10(0.05) Rsun, while it was found as 1.80(0.01) Rsun 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 delta Scuti star. The period of pulsation was found to be 58.482(0.002), 58.482(0.001), 60.966(0.002), 60.964(0.003) minutes in BVRI bands, respectively. We plotted V1464 Aql in the plane of log(Porb)-log(Ppulse). Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the plane of log(Porb)-log(Ppulse) for each type binary. Using the linear fit of each group, we obtained new calibrations between log(Porb) and log(Ppulse) for different type pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars from the 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 delta Scuti component.
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