论文标题
发现带有准球形质量损失的棕色矮人
Discovery of a brown dwarf with quasi-spherical mass-loss
论文作者
论文摘要
我们报告了与淡淡的恒星对象相关的椭圆形外壳SSTC2D J163134.1-24006相关的偶然发现，作为“ Ophiuchus Disk调查的一部分，使用Alma）（Odisea）（Odisea）（旨在研究Ophiuchus $ ophiuchus opistion $ co $ ophiuchus of 230 ghz ostrist $ clots of 230 ghz ostrip of 23030303030303030303030303030年）的项目。 （j = 2-1），$^{13} $ co（j = 2-1）和c $^{18} $ co（j = 2-1）在band-6中可读取的行。值得注意的是，我们检测到$ \ sim $ 3 $ 3 $^{“} $ $ \ times $ 4 $ 4 $^{”} $的明亮$^{12} $ CO椭圆形发射，to sstc2d J163134.1-24006，没有230 GHz连续检测。 Based on the observed near-IR spectrum taken with the Very Large Telescope (KMOS), the brightness of the source, its 3-dimensional motion, and Galactic dynamic arguments, we conclude that the source is not a giant star in the distant background ($>$5 - 10 kpc) and is most likely to be a young brown dwarf in the Ophiuchus cloud, at a distance of just $\sim$139 pc.这是年轻的棕色矮人中准球形质量损失的第一个报告。我们建议观察到的壳可以与氘融合产生的热脉冲有关，氘的融合尚不清楚，但是对于一个少数Myr年龄的短时间内，子赛物体有望发生，与该地区的物体的年龄一致。其他更异国情调的场景，例如与行星同伴的合并，不能从当前的观察结果中排除。
We report the serendipitous discovery of an elliptical shell of CO associated with the faint stellar object SSTc2d J163134.1-24006 as part of the "Ophiuchus Disk Survey Employing ALMA" (ODISEA), a project aiming to study the entire population of protoplanetary disks in the Ophiuchus Molecular Cloud from 230 GHz continuum emission and $^{12}$CO (J=2-1), $^{13}$CO (J=2-1) and C$^{18}$CO (J=2-1) lines readable in Band-6. Remarkably, we detect a bright $^{12}$CO elliptical shape emission of $\sim$ 3$^{"}$ $\times$ 4$^{"}$ towards SSTc2d J163134.1-24006 without a 230 GHz continuum detection. Based on the observed near-IR spectrum taken with the Very Large Telescope (KMOS), the brightness of the source, its 3-dimensional motion, and Galactic dynamic arguments, we conclude that the source is not a giant star in the distant background ($>$5 - 10 kpc) and is most likely to be a young brown dwarf in the Ophiuchus cloud, at a distance of just $\sim$139 pc. This is the first report of quasi-spherical mass loss in a young brown dwarf. We suggest that the observed shell could be associated with a thermal pulse produced by the fusion of deuterium, which is not yet well understood, but for a sub-stellar object is expected to occur during a short period of time at an age of a few Myr, in agreement with the ages of the objects in the region. Other more exotic scenarios, such as a merger with planetary companions, cannot be ruled out from the current observations.
