对WASP-43 b和TrES-3 b凌星主食的测光后续观测及凌星中心时刻变化研究
发布时间：2018-08-14 17:41
【摘要】：使用紫金山天文台盱眙观测站近地天体望远镜对WASP-43 b和TrES-3 b分别做了2次和4次凌星主食的测光后续观测.经过较差测光和光变曲线拟合,分别得到了两个系统的相关物理参数,结果与之前的文献结果吻合.结合多篇文献中的数据,对两个系统凌星中心时刻的观测残差O-C分别作了线性和二次函数拟合,根据线性拟合得到了行星的轨道周期及凌星中心时刻变化即TTV,分析后认为在两个系统中尚未发现明显的周期性TTV信号,并给出了WASP-43和TrES-3系统中1:2轨道共振位置上可能存在行星的质量上限分别为1.826和1.504个地球质量.通过二次函数拟合,尚未发现TrES-3b存在长期TTV即轨道衰变;证认了WASP-43 b可能存在轨道衰变,得到其轨道衰变率P=(-0.005248±0.001714)s·yr~(-1),并与文献中的相关结果做了比较,还据此计算出了该系统的恒星潮汐质量参数下限为Q_*~'≥1.5×10~5,并分别对两个系统中不同的Q_*~'值给出了相应的行星剩余寿命.
[Abstract]:The near-Earth object telescope of Xuyi Observatory of Zijinshan Observatory has been used to observe WASP-43 b and TrES-3 b twice and 4 times respectively. The physical parameters of the two systems are obtained by the fitting of the differential photometry and the photovariation curve, and the results are in agreement with the previous literatures. Based on the data in many literatures, the linear and quadratic function fitting of the observed residual O-C of the central moments of the two systems is made. According to the linear fitting, the orbital period of the planet and the change of the central moment of the Lexus are obtained. It is concluded that no obvious periodic TTV signals have been found in the two systems. The upper mass limits of the possible planets at the resonance position of 1:2 orbit in the WASP-43 and TrES-3 systems are 1.826 and 1.504 respectively. By quadratic function fitting, it has not been found that there is a long term TTV that is orbital decay in TrES-3b, and the orbital decay rate P = (-0.005248 卤0.001714) s ~ (-1) of WASP-43 b may exist, and the results are compared with those in literature. Based on this, the lower limit of the mass parameters of the stellar tides is calculated to be Q _ T '鈮，
本文编号：2183617
[Abstract]:The near-Earth object telescope of Xuyi Observatory of Zijinshan Observatory has been used to observe WASP-43 b and TrES-3 b twice and 4 times respectively. The physical parameters of the two systems are obtained by the fitting of the differential photometry and the photovariation curve, and the results are in agreement with the previous literatures. Based on the data in many literatures, the linear and quadratic function fitting of the observed residual O-C of the central moments of the two systems is made. According to the linear fitting, the orbital period of the planet and the change of the central moment of the Lexus are obtained. It is concluded that no obvious periodic TTV signals have been found in the two systems. The upper mass limits of the possible planets at the resonance position of 1:2 orbit in the WASP-43 and TrES-3 systems are 1.826 and 1.504 respectively. By quadratic function fitting, it has not been found that there is a long term TTV that is orbital decay in TrES-3b, and the orbital decay rate P = (-0.005248 卤0.001714) s ~ (-1) of WASP-43 b may exist, and the results are compared with those in literature. Based on this, the lower limit of the mass parameters of the stellar tides is calculated to be Q _ T '鈮，
本文编号：2183617
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