论文标题
磁盘风的演变来自光学和红外线的联合研究
The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines
论文作者
论文摘要
我们分析了涵盖[OI] 6300 Angstrom和[NEII] 12.81微米线的高分辨率（DV = <10km/s）光谱，来自不同进化阶段的31个磁盘样品。在光波长下工作后，我们使用高斯轮廓拟合[NEII]线，并将其分类为HVC（LVC），如果相对于恒星径向速度，该线质心比30 km/s的蓝光更少（较少）。与[OI]通常伴有LVC的[OI]不同，所有17个具有[NEII]检测的来源均具有HVC或LVC。 [NEII]在高增生器（MACC> 10 $^{ - 8} $ msun/yr）方面优先检测到HVC，而LVC则在低MACC，低[OI]亮度和大型红外光谱指数（N13-31）的来源中发现。有趣的是，[NEII]和[OI] LVC亮度表现出与N13-31相反的行为：随着内部灰尘磁盘的耗竭（较高的N13-31），[neii]的光度在[OI]弱弱时增加。 [NEII]和[OI] HVC曲线通常与质心和FWHM相似，显示了微型射流中震动气体的预期行为。相比之下，[NEII] LVC曲线通常比[OI]轮廓更蓝色和狭窄。 FWHM和Centroid vs.磁盘倾斜度表明，[NEII] LVC主要从缓慢而广角的风中痕迹无绑的气体，但并未完全失去其发射区域的开普勒签名。我们绘制一个进化方案，该方案可以解释[OI]和[NEII]结果，并包括在内部，大部分是分子的MHD风中筛选硬（〜1KeV）X射线。
We analyze high-resolution (dv=<10km/s) optical and infrared spectra covering the [OI] 6300 angstrom and [NeII] 12.81 micron lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the [NeII] lines and classify them into HVC (LVC) if the line centroid is more (less) blueshifted than 30 km/s with respect to the stellar radial velocity. Unlike for the [OI] where a HVC is often accompanied by a LVC, all 17 sources with a [NeII] detection have either a HVC or a LVC. [NeII] HVCs are preferentially detected toward high accretors (Macc > 10$^{-8}$ Msun/yr) while LVCs are found in sources with low Macc, low [OI] luminosity, and large infrared spectral index (n13-31). Interestingly, the [NeII] and [OI] LVC luminosities display an opposite behaviour with n13-31: as the inner dust disk depletes (higher n13-31) the [NeII] luminosity increases while the [OI] weakens. The [NeII] and [OI] HVC profiles are generally similar with centroids and FWHMs showing the expected behaviour from shocked gas in micro-jets. In contrast, the [NeII] LVC profiles are typically more blueshifted and narrower than the [OI] profiles. The FWHM and centroid vs. disk inclination suggest that the [NeII] LVC predominantly traces unbound gas from a slow, wide-angle wind that has not lost completely the Keplerian signature from its launching region. We sketch an evolutionary scenario that could explain the combined [OI] and [NeII] results and includes screening of hard (~1keV) X-rays in inner, mostly molecular, MHD winds.
