由HST时间分辨光谱得到的Luhman 16 AB云结构演化图
Maps of Evolving Cloud Structures in Luhman 16AB from HST Time-Resolved Spectroscopy
摘要：
WISE J104915.57-531906.1是距离我们太阳系最近的褐矮星双星，由两颗处于L/T转换的褐矮星组成：Luhman 16 A和B。本文给出了Luhman 16 A的第一张图和Luhman 16 B两个时期的图。我们的地图是通过应用Aeolus创建的，Aeolus是一种马尔可夫链蒙特卡罗代码，可以使用哈勃太空望远镜的G141和G102 grisms绘制褐矮星和其他超冷大气的大气层顶部结构，以Luhman 16 A和B的光变曲线。Aeolus在Luhman 16 A和B的大气层顶部获得了三个或四个点，表面覆盖率分别为19%-32%（取决于假设的5小时或8小时的旋转周期）或21%-38.5%（取决于观测时期）。最佳拟合模型的亮点的亮度温度比背景大气层顶部高约200 K。我们将我们的Luhman 16 B地图与之前出版的唯一地图进行了比较。有趣的是，我们的地图包含一个大的，比背景低纬度大气层顶部更冷的点（DT~51 K），与以前的Luhman 16 B地图一致。最后，我们报告了在Luhman 16 B光变曲线中重新出现的特征的检测，这些光变曲线彼此相隔数十个旋转。我们推测这一特征与Luhman 16 B的大气层顶结构有关。
英文摘要：
WISE J104915.57-531906.1 is the nearest brown dwarf binary to our Solar system, consisting of two brown dwarfs in the L/T transition: Luhman 16A & B. In this paper we present the first map of Luhman 16A, and maps of Luhman 16B for two epochs. Our maps were created by applying Aeolus, a Markov-Chain Monte Carlo code that maps the top-of-the-atmosphere structure of brown dwarf and other ultracool atmospheres, to light curves of Luhman 16A & B using the Hubble Space Telescope's G141 and G102 grisms. Aeolus retrieved three or four spots in the top-of-the-atmosphere of Luhman 16A & B, with a surface coverage of 19%-32% (depending on an assumed rotational period of 5 hr or 8 hr) or 21%-38.5% (depending on the observational epoch) respectively. The brightness temperature of the spots of the best-fit models was ~200 K hotter than the background top-of-the-atmosphere. We compared our Luhman 16B map with the only previously published map. Interestingly, our map contained a large, cooler (DT~51 K) than the background top-of-the-atmosphere spot that lay at low latitudes, in agreement with the previous Luhman 16B map. Finally, we report the detection of a feature reappearing in Luhman 16B light curves that are separated by tens of hundreds of rotations from each other. We speculate this feature is related to top-of-the-atmosphere structures of Luhman 16B.
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