关于年轻恒星[Ne II ]发射的起源：甚大望远镜的中红外和光学观测
On the origin of [Ne II] emission in young stars: mid-infrared and optical observations with the Very Large Telescope
摘要：
（Arxiv的摘要版本）我们提供了直接的约束的起源[Ne II]发射在15个年轻的恒星使用高空间和光谱分辨率的观测与VISIR在VLT，使我们能够研究运动学的发射气体。此外，我们还将[Ne II]线与三颗恒星在UVES下观察到的光学禁戒线进行了比较。在7颗恒星中发现了[Ne II]线，其中第一次确认的是在Herbig Be恒星V892 Tau中发现的[Ne II]。在四种情况下，大的蓝移线表明起源于喷流。在两颗恒星中，小的位移和不对称的轮廓表明起源于光蒸发风。CoKu Tau 1，靠近边缘，显示了一条以恒星静止速度为中心的空间不可分辨的线，尽管交叉色散质心从恒星的一侧移动到另一侧的10 AU范围内，作为波长的函数。谱线轮廓是对称的，机翼延伸到大约+-80 km/s。[Ne II]线的起源可能是由于双极射流或磁盘。对于具有VLT-UVES观测的恒星，在几种情况下，光学禁戒线的轮廓和位移与[Ne II]线的轮廓非常相似，这表明这些线在同一区域发射。与斯皮策获得的通量相比，用VISIR观察到的一般趋势是较低的线通量。我们发现线的半峰全宽和线的峰值速度之间没有相关性。[Ne II]线在大部分样本中仍然未被检测到，这表明斯皮策在这些恒星中检测到的发射可能会延长。
英文摘要：
{Abridged version for ArXiv}. We provide direct constraints on the origin of the [Ne II] emission in 15 young stars using high-spatial and spectral resolution observations with VISIR at the VLT that allow us to study the kinematics of the emitting gas. In addition we compare the [Ne II] line with optical forbidden lines observed for three stars with UVES. The [Ne II] line was detected in 7 stars, among them the first confirmed detection of [Ne II] in a Herbig Be star, V892 Tau. In four cases, the large blueshifted lines indicate an origin in a jet. In two stars, the small shifts and asymmetric profiles indicate an origin in a photo-evaporative wind. CoKu Tau 1, seen close to edge-on, shows a spatially unresolved line centered at the stellar rest velocity, although cross-dispersion centroids move within 10 AU from one side of the star to the other as a function of wavelength. The line profile is symmetric with wings extending up to about +-80 km/s. The origin of the [Ne II] line could either be due to the bipolar jet or to the disk. For the stars with VLT-UVES observations, in several cases, the optical forbidden line profiles and shifts are very similar to the profile of the [Ne II] line, suggesting that the lines are emitted in the same region. A general trend observed with VISIR is a lower line flux when compared with the fluxes obtained with Spitzer. We found no correlation between the line full-width at half maximum and the line peak velocity. The [Ne II] line remains undetected in a large part of the sample, an indication that the emission detected with Spitzer in those stars is likely extended.
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