Rotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoring
Rotation periods and astrometric motions of the Luhman 16AB brown dwarfs by high-resolution lucky-imaging monitoring
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通过高分辨率幸运成像监测卢曼 16AB 棕矮星的自转周期和天体运动
DOI：
10.1051/0004-6361/201526899
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发表时间：
2015-10
期刊：
影响因子：
--
通讯作者：
S. C
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文献类型：
--
作者：
L. Mancini;P. Giacobbe;S. P. Littlefair;J. Southworth;V. Bozza;M. Damasso;M. Dominik;M. Hundertmark;U. G. Jørgensen;D. Juncher;A. Popovas;M. Rabus;S. Rahvar;R. W. Schmidt;J. Skottfelt;C. Snodgrass;A. Sozzetti;K. Alsubai;D. M. Bramich;S. Calchi Novati;S. C
对棕矮星的光度变化进行监测可以提供有关其冷大气中云结构的有用信息。棕矮星双星系统Luhman 16 AB是此类研究的一个有趣目标，因为它的组成部分位于L/T过渡区，并显示出高水平的变化。Luhman 16 AB也是第三个最接近太阳系的系统，这使得精确的天体测量调查与地面facilities.AimsThe目的的工作是估计旋转周期和研究天体测量运动的两个components.MethodsWe监测Luhman 16 AB在为期两年的幸运成像相机安装在丹麦1.54米望远镜在拉西拉，通过一个特殊的长通滤波器，这使我们能够清楚地将两颗褐矮星分解成单个物体。一个强烈的监测的目标也进行了超过16个夜晚，在其中我们观察到的峰-峰变异为0.20 ± 0.02马格和0.34 ± 0.02马格的Luhman 16 A和16 B，results.ResultsWe使用的16夜的时间序列数据来估计旋转周期的两个组件。我们发现Luhman 16 B的自转周期为5.1 ± 0.1 h，与以前的测量结果非常一致。对于Luhman 16 A，我们报告说它的旋转速度比它的同伴慢，即使我们无法得到一个可靠的确定，我们的数据表明旋转周期约为8小时。这意味着这两个组成部分的旋转轴很好地对齐，并表明这两个物体经历了相同的吸积过程。利用2年的完整观测资料研究了Luhman 16 AB的天体运动。我们预测该系统的运动与之前基于两个月监测的估计不一致，但无法证实或反驳该系统中存在其他行星质量的天体。
ContextPhotometric monitoring of the variability of brown dwarfs can provide useful information about the structure of clouds in their cold atmospheres.The brown-dwarf binary system Luhman 16AB is an interesting target for such a study, because its components stand at the L/T transition and show high levels of variability. Luhman 16AB is also the third closest system to the solar system, which allows precise astrometric investigations with ground-based facilities.AimsThe aim of the work is to estimate the rotation period and study the astrometric motion of both components.MethodsWe have monitored Luhman 16AB over a period of two years with the lucky-imaging camera mounted on the Danish 1.54 m telescope at La Silla, through a speciali+zlong-pass filter, which allowed us to clearly resolve the two brown dwarfs into single objects. An intense monitoring of the target was also performed over 16 nights, in which we observed a peak-to-peak variability of 0.20 ± 0.02 mag and 0.34 ± 0.02 mag for Luhman 16A and 16B, respectively.ResultsWe used the 16-night time-series data to estimate the rotation period of the two components. We found that Luhman 16B rotates with a period of 5.1 ± 0.1 h, in very good agreement with previous measurements. For Luhman 16A, we report that it rotates more slowly than its companion, and even though we were not able to get a robust determination, our data indicate a rotation period of roughly 8 h. This implies that the rotation axes of the two components are well aligned and suggests a scenario in which the two objects underwent the same accretion process. The 2-year complete data set was used to study the astrometric motion of Luhman 16AB. We predict a motion of the system that is not consistent with a previous estimate based on two months of monitoring, but cannot confirm or refute the presence of additional planetary-mass bodies in the system.
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DOI：
10.1088/0067-0049/182/1/205
发表时间：
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期刊：
The Astrophysical Journal Supplement Series
影响因子：
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作者：
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通讯作者：
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影响因子：
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DOI：
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发表时间：
2014-02
期刊：
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影响因子：
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DOI：
10.1088/2041-8205/767/1/l1
发表时间：
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影响因子：
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