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首页> 外文期刊>PASJ: Publications of the Astronomical Society of Japan >The W-subtype active contact binary PZ UMa with a possible more massive tertiary component
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The W-subtype active contact binary PZ UMa with a possible more massive tertiary component

机译：W-Subtype有源接触二元PZ UMA，具有可能的巨大三级组分

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Two sets of multiple-color (B, V, R-C, I-C) light curves of PZ UMa were observed independently with the 2.4 m telescope at the Thai National Observatory and the 1 m telescope at Yunnan Observatories. The light curves were analyzed with the Wilson-Devinney program and the two sets of light curves produced consistent results, which shows that PZ UMa is a W-subtype contact binary with an extreme mass ratio (M-1/M-2 = 0.18). The basic physical parameters of PZ UMa were determined to be M-2 = 0.77(2) M-circle dot, M-1 = 0.14(1) M-circle dot, R-2 = 0.92(1) R-circle dot, R-1 = 0.43(1) R-circle dot, L-2 = 0.46(2) L-circle dot, and L-1 = 0.15(3) L-circle dot. The orbital period analysis of PZ UMa revealed a 13.22 yr periodicity, which implies that there may be a tertiary component orbiting around the binary system. The mass and orbital radius of the tertiary component were calculated to be M-3 = 0.88 M-circle dot and a(3) = 3.67 au, if the orbit was coplanar with the central binary system. It is interesting that the minimum mass of the tertiary was calculated to be M-3min = 0.84 M-circle dot, which means the tertiary component is even larger than the primary star and the secondary one of PZ UMa. PZ UMa is a late-type contact binary with stellar activity. The O'Connell effect appeared on its light curves when it was observed in 2016 April. However, the O'Connell effect reversed when the target was observed again in 2016 December. The changes of the O'Connell effect on such a short time-scale strongly support the occurrence of rapidly changing magnetic activity in this W UMa binary.
机译：在泰国国家天文台的2.4米望远镜和云南观察仪的1米望远镜，独立地观察到PZ UMA的两组多色（B，V，R-C，I-C，I-C）光曲线。用Wilson-Devinney程序分析光曲线，两组光曲线产生了一致的结果，结果表明PZ UMA是具有极其质量比（M-1 / M-2 = 0.18）的W-亚型接触二进制二进制。将PZ UMA的基本物理参数确定为M-2 = 0.77（2）m圆点，M-1 = 0.14（1）m圆点，R-2 = 0.92（1）r圈点， R-1 = 0.43（1）r圈点，L-2 = 0.46（2）L圆点，L-1 = 0.15（3）L圈点。 PZ UMA的轨道周期分析显示为13.22年的周期性，这意味着可能存在围绕二元体系进行三级组分。如果轨道与中央二元系统共面，则计算第三组分的质量和轨道半径为M-3 = 0.88M圆点和A（3）= 3.67 Au。有趣的是，将第三次的最小质量计算为M-3min = 0.84 m圆点点，这意味着叔成分甚至大于PZ UMA中的初级星和二级。 PZ UMA是具有恒星活性的后期接触二进制。 o'connell效应在2016年4月观察到的光线曲线上。然而，2016年12月再次观察目标时，O'Connell效应逆转。 O'connell对这种短时间级别的影响的变化强烈地支持该W uma二进制中快速改变磁性活性的发生。

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