The planets around nn serpentis: still there
The planets around nn serpentis: still there
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DOI：
10.1093/mnras/stt1903
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发表时间：
2013-10
影响因子：
4.8
通讯作者：
T. Marsh;S. Parsons;M. Bours;S. Littlefair;C. Copperwheat;V. Dhillon;E. Breedt;C. Caceres;M. Schreiber
中科院分区：
文献类型：
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作者：
T. Marsh;S. Parsons;M. Bours;S. Littlefair;C. Copperwheat;V. Dhillon;E. Breedt;C. Caceres;M. Schreiber
我们提出了25个新的日食时间的白色矮二进制NN Ser采取的高速相机ULTRACAM的威廉赫歇尔望远镜和新技术望远镜，上升相机的利物浦望远镜和HAWK-I的甚大望远镜测试的双行星模型，提出解释在过去25年的日食时间测量的变化。行星模型以出色的成绩通过了测试，正确地预测了自2010年以来日食时间的36秒的渐进滞后，与之前8年的精确时间相比。假设两个轨道都是偏心的，我们发现轨道周期分别为7.9 ± 0.5和15.3 ± 0.3年，质量分别为2.3 ± 0.5和7.3 ± 0.3兆焦耳。我们还发现动态长寿轨道与数据一致，与2：1和5：2的周期比。相对于最佳拟合模型，数据分散了0.07秒，在某种程度上是任何提出的食紧凑物体行星宿主中最精确的。尽管精度很高，但轨道拟合的简并性阻止了对双星周期变化和N体效应的显著测量。最后，我们指出了一个主要的缺陷与以前的动态稳定性分析的NN Ser，并通过扩展，与一些类似的系统的分析。
We present 25 new eclipse times of the white dwarf binary NN Ser taken with the high-speed camera ULTRACAM on the William Herschel Telescope and New Technology Telescope, the RISE camera on the Liverpool Telescope and HAWK-I on the Very Large Telescope to test the two-planet model proposed to explain variations in its eclipse times measured over the last 25 yr. The planetary model survives the test with flying colours, correctly predicting a progressive lag in eclipse times of 36 s that has set in since 2010 compared to the previous 8 yr of precise times. Allowing both orbits to be eccentric, we find orbital periods of 7.9 ± 0.5 and 15.3 ± 0.3 yr, and masses of 2.3 ± 0.5 and 7.3 ± 0.3 MJ. We also find dynamically long-lived orbits consistent with the data, associated with 2:1 and 5:2 period ratios. The data scatter by 0.07 s relative to the best-fitting model, by some margin the most precise of any of the proposed eclipsing compact object planet hosts. Despite the high precision, degeneracy in the orbit fits prevents a significant measurement of a period change of the binary and of N-body effects. Finally, we point out a major flaw with a previous dynamical stability analysis of NN Ser, and by extension, with a number of analyses of similar systems.