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Photometric and Spectroscopic Analysis of Four Contact Binaries
The Astronomical Journal ( IF 5.3 ) Pub Date : 2021-04-09 , DOI: 10.3847/1538-3881/abea0c
A. Panchal 1, 2 , Y. C. Joshi 1
Affiliation  

We present the photometric and spectroscopic analysis of four W UMa binaries J015829.5+260333 (hereinafter as J0158), J030505.1+293443 (hereinafter as J0305), J102211.7+310022 (hereinafter as J1022), and KW Psc. The VR c I c band photometric observations are carried out with the 1.3 m Devasthal Fast Optical Telescope (DFOT). For low-resolution spectroscopy, we used the 2 m Himalayan Chandra Telescope (HCT) as well as the archival data from the 4 m LAMOST survey. The systems J0158 and J0305 show a period increase rate of 5.26( 1.72) 10−7 days yr−1 and 1.78( 1.52) 10−6 days yr−1, respectively. The period of J1022 is found to be decreasing with a rate of 4.22 ( 1.67) 10−6 days yr−1. The period analysis of KW Psc displays no change in its period. The PHOEBE package is used for the light-curve modeling and basic parameters are evaluated with the help of the GAIA parallax. The asymmetry of light curves is explained with the assumption of cool spots at specific positions on one of the components of the system. On the basis of temperatures, mass ratios, fill-out factors, and periods, the system J1022 is identified as a W-subtype system while the others show some mixed properties. To probe the chromospheric activities in these W UMa binaries, their spectra are compared with the known inactive stars’ spectra. The comparison shows emission in H α , H β , and Ca II. To understand the evolutionary status of these systems, the components are plotted in mass–radius and mass–luminosity planes with other well characterized binary systems. The secondary components of all the systems are away from ZAMS, which indicates that the secondary is more evolved than the primary component.



中文翻译:

四种接触双星的光度和光谱分析

我们介绍了四个 W UMa 双星 J015829.5+260333(以下称为 J0158)、J030505.1+293443(以下称为 J0305)、J102211.7+310022(以下称为 J1022)和 Psc 的光度和光谱分析。该VR ÇÇ波段测光观测与1.3微米Devasthal快速光学望远镜(DFOT)进行。对于低分辨率光谱,我们使用了 2 m 喜马拉雅钱德拉望远镜 (HCT) 以及来自 4 m LAMOST 调查的档案数据。系统J0158和J0305分别显示5.26( 1.72) 10 -7 days yr -1和1.78( 1.52) 10 -6 days yr -1的周期增长率。发现 J1022 的周期以 4.22 ( 1.67) 10 的速率下降 -6天 年-1。KW Psc 的周期分析显示其周期没有变化。PHOEBE 包用于光曲线建模,并在 GAIA 视差的帮助下评估基本参数。光变曲线的不对称性是通过假设系统组件之一的特定位置上的冷点来解释的。根据温度、质量比、填充因子和周期,系统 J1022 被确定为 W 亚型系统,而其他系统则显示出一些混合特性。为了探测这些 W UMa 双星的色球活动,将它们的光谱与已知的不活动恒星的光谱进行比较。比较显示在H αH β和 Ca II 中的发射 . 为了了解这些系统的演化状态,将组件绘制在质量-半径和质量-光度平面上,并与其他已充分表征的双星系统一起绘制。所有系统的次要组件都远离 ZAMS,这表明次要组件比主要组件更进化。

更新日期:2021-04-09
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