论文标题
一个世纪以上的$δ$ CETI变异性调查
Over a century of $δ$ Ceti variability investigation
论文作者
论文摘要
我们提出了2014 - 2018年径向速度测量$δ$ CETI的活动的结果。结合我们对脉动周期的确定与历史数据相结合，我们得出的结论是，观察到的变化最有可能的解释是在轨道上的最低质量为$ 1.10 \ pm 0.05 m _ {\ odot} $的次级成分，其周期为$ 169 \ pm 6 $。因此，我们将内在的，进化期的变化率修改为不大于$ 0.018 \ pm 0.004 $ s/Center，这明显低于以前的估计，并且与Neilson＆Ignace的进化模型一致（2015年）。我们在径向速度期刊中没有发现任何明显的多重频率，例如Aerts等人报道的频率。 （2006年）在大多数卫星的光度数据中。使用JMMC恒星直径目录的干涉角尺寸为$δ$ CETI，我们使用降压通量法确定了恒星的几个物理参数。事实证明，与使用Aerts等人的不同方法获得的$δ$ CETI相比，$δ$ CETI的质量较低和较慢的演变与较低的质量和较慢的演变是一致的。 （2006）和Neilson＆Ignace（2015）。
We present results of a 2014-2018 campaign of radial velocity measurements of $δ$ Ceti. Combining our determination of pulsation period with historical data we conclude that the most likely explanation of observed changes is the presence of a secondary component with a minimum mass of $1.10 \pm 0.05 M_{\odot}$ on an orbit with a period of $169 \pm 6$ years. Consequently, we revised the intrinsic, evolutionary period change rate to not larger than $0.018 \pm 0.004$ s/century, which is significantly lower than previous estimations and is consistent with evolutionary models of Neilson & Ignace (2015). We did not find any significant multiperiodic frequencies in radial velocity periodograms such as those reported by Aerts et al. (2006) in photometric data from MOST satellite. Using interferometric angular size of $δ$ Ceti from JMMC Stellar Diameters Catalogue we determined several physical parameters of the star with bolometric flux method. They turned out to be consistent with most previous deteminations, confirming lower mass and slower evolution of $δ$ Ceti than obtained using different methods by Aerts et al. (2006) and Neilson & Ignace (2015).
