标题： 长期掩食结束时的PMS星V1184 Tau (CB 34V) 显示英文标题

标题： The PMS star V1184 Tau (CB 34V) at the end of prolonged eclipse

摘要： V1184 Tau (CB 34V)位于博克星云CB 34的视野内，于1993年被发现为一个大振幅变星。 根据该恒星变异性假设的第一种说法，它是在1951年至1993年间爆发的FU奥里星候选体。 在后续观测中，这颗恒星表现出大振幅变异性，被解释为由尘埃周围的星云遮挡所致。 我们将V1184 Tau (CB 34V)纳入高度可变的前主序目标列表，以确定此物体亮度变化的原因。 本文展示了2008年至2015年期间获得的年轻恒星天体V1184 Tau的BVRI测光观测数据。 这些数据是我们从2000年开始对该恒星进行光学测光监测的延续，并持续至今。 V1184 Tau的测光观测在两个天文台使用两台中型望远镜和两台小型望远镜进行。 我们的结果显示，在最大亮度期间，这颗恒星显示出典型T Tauri星的特征。 然而，在亮度深最小值期间，V1184 Tau更类似于UX猎户座天体。 亮度的深幅下降始于2003年，到2015年结束，此时恒星已恢复至最大亮度。 下降期间的光变曲线显然是不对称的，因为亮度降低的时间是上升时间的两倍。 色-星等图上观察到的颜色反转也证实了尘埃周围星云的遮挡是造成亮度大振幅变化的原因。 显示英文摘要

摘要： V1184 Tau (CB 34V) lies in the field of the Bok globule CB 34 and was discovered as a large amplitude variable in 1993. According to the first hypothesis of the variability of the star, it is a FU Orionis candidate erupted between 1951 and 1993. During subsequent observations, the star manifests large amplitude variability interpreted as obscuration from circumstellar clouds of dust. We included V1184 Tau (CB 34V) in our target list of highly variable pre-main-sequence stars to determine the reasons for the variations in the brightness of this object. Data from BVRI photometric observations of the young stellar object V1184 Tau, obtained in the period 2008-2015, are presented in the paper. These data are a continuation of our optical photometric monitoring of the star began in 2000 and continuing to date. The photometric observations of V1184 Tau were performed in two observatories with two medium-sized and two small telescopes. Our results indicate that during periods of maximum light the star shows characteristics typical of T Tauri stars. During the observed deep minimum in brightness, however, V1184 Tau is rather similar to UX Orionis objects. The deep drop in brightness began in 2003 ended in 2015 as the star has returned to maximum light. The light curve during the drop is obviously asymmetric as the decrease in brightness lasts two times longer than the rise. The observed colour reverse on the colour-magnitude diagrams is also confirmation of obscuration from circumstellar clouds of dust as a reason for the large amplitude variability in the brightness.