Search for companions in visual binary systems using precise radial-velocity measurements
Search for companions in visual binary systems using precise radial-velocity measurements
复制标题
使用精确的径向速度测量在视觉双星系统中搜索伴星
DOI：
10.1093/pasj/psy054
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发表时间：
2018
影响因子：
2.3
通讯作者：
Sato Bun’ei
中科院分区：
文献类型：
--
作者：
Katoh Noriyuki;Itoh Yoichi;Sato Bun’ei
在恒星形成的早期阶段，三重和四重系统的频率被认为是很高的。一些多系统在前主序列相衰变。主序星的多样性为双星系统的演化提供了线索。这项工作使用精确的径向速度测量来寻找视觉双星系统的五个组成部分的伴星。2007年至2012年，使用安装在冈山天体物理天文台(OAO)1.88米反射器上的高色散回声光谱仪(HIDES)监测了它们的径向速度。结合前人的工作，这项工作为这五个天体寻找了轨道周期小于9 yr的伴星。我们发现ADS 6190 A和BDS 10966A的径向速度存在周期性变化。ADS 7311 A、31 dra A和31 dra B的径向速度显示出显著的趋势。ADS 6190 A是一颗双星，轨道周期为366.2 d，次星的最小质量为0.5。对ADS 7311 A的径向速度进行了3200 d的观测.我们排除了行星质量伴星是导致ADS 10966 A径向速度下降趋势的原因.这项工作证实了BDS 10966 A径向速度的周期变化为771.1 d.平分分析没有发现谱线的不对称性与BDS 10966 A的径向速度之间的相关性.我们拒绝将光球的非径向振荡作为径向速度变化的来源.这种变化可能是由表面不均匀引起的旋转调制引起的。本文推导的31 dra A的轨道元素与前人的一致。31 dra A系统是一个sb1双星，其最小质量比为0.30 ？ 0.08。31 Dra B的径向速度呈现周期性变化。得到的轨道元与前人报道的轨道元基本一致。这种变化是由一颗环绕恒星的行星引起的。
The frequency of triple and quadruple systems is considered to be high in the early phase of star formation. Some multiple systems decay in the pre-main-sequence phase. The multiplicity of main-sequence stars provides clues about the evolution of binary systems. This work searched for companions of five components of visual binary systems using precise radial-velocity measurements. Their radial velocities were monitored from 2007 to 2012 using the HIgh Dispersion Echelle Spectrograph (HIDES) installed on the Okayama Astrophysical Observatory (OAO) 1.88 m reflector. In combination with previous work, this work searched for companions with an orbital period of less than 9 yr for the five bodies. We found periodic variations in the radial velocities for ADS 6190 A and BDS 10966A. The radial velocities of ADS 7311 A, 31 Dra A, and 31 Dra B show significant trends. ADS 6190 A is an SB1 binary with an orbital period of 366.2 d. The minimum mass of the secondary star is 0.5. The radial velocity of ADS 7311 A was monitored for an observational span of 3200 d. We rejected a planetary-mass companion as the cause of a decreasing trend in the radial velocity of ADS 7311 A. This work confirmed that the periodic variation in the radial velocity of BDS 10966 A is 771.1 d. Bisector analysis did not reveal a correlation between the asymmetry of a spectral line and the radial velocity of BDS 10966 A. We rejected nonradial oscillation of the photosphere as the source of the radial velocity variation. The variation may be caused by the rotational modulation owing to surface inhomogeneity. The orbital elements of 31 Dra A derived in this paper are consistent with those in a previous paper. 31 Dra A system is an SB1 binary with a minimum mass ratio of 0.30 ± 0.08. 31 Dra B exhibits a periodic variation in radial velocity. The orbital elements derived in this work are consistent with those reported previously by others. The variation is caused by a circumstellar planet.