食双星DS Psc的观测与研究  

Photometric Studies of the Eclipsing Binary DS Psc

作　　者：张燕平[1] 蒋明栋[1] 张孝斌[2] 付建宁[1] 陈孝钿 白宇[1] 

机构地区：[1]北京师范大学天文系,北京100875 [2]中国科学院国家天文台,北京100012

出　　处：《天文学报》2014年第4期288-301,共14页Acta Astronomica Sinica

基　　金：国家自然科学基金委员会与中国科学院天文联合基金项目(U1231202;11178007);科技部973项目(2013CB834900);中央高校基本科研业务费专项资金资助

摘　　要：捅要从2009年到2014年,对食双星DS Psc进行了多色测光和光谱观测,得到了完整覆盖的B、V、R 3色光变曲线以及一批新的光变极小时刻,并首次确定了该双星系统的光谱型.综合已有极小时刻数据,采用O-C方法进行周期分析,得到了新的轨道周期及历元公式.利用Wilson-Devinney方法,对观测所得光变曲线作了拟合分析,首次得到了该双星系统的测光轨道初解.结果表明DS Psc为一个光谱型约为G7V的过相接双星系统.其轨道倾角为66.6°,质量比为2.506.由于其小质量的次子星具有比大质量主子星更高的表面温度,因此DS Psc应属于W次型的W UMa型双星.New multi-color photometric and spectroscopic observations were made for the eclipsing binary DS Psc from 2009 to 2014,leading to the light curves in B,V,and R bands with a complete phase coverage.Forty-one new times of light minimum are determined,and the spectral types of the binary system are deduced.The O-C method is applied to get the orbital period and the epoch formula,combined with the times of light minimum in literature.The light curves are fitted to get the photometric solution of the binary system,by using the Wilson-Devinney code.The result shows that DS Psc is an over-contact binary with the spectral type of G7V,the orbital inclination of 66.6°,and the mass ratio of 2.506.Since the less-massive component has higher surface temperature than the more-massive one,DS Psc should belong to the W subtype of W UMa type binary stars.

关 键 词：双星 密近 双星 食 恒星 个别 DS PSC 

分 类 号：P144[天文地球—天体物理]