The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines
The Evolution of Disk Winds from a Combined Study of Optical and Infrared Forbidden Lines
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DOI：
10.3847/1538-4357/abba3c
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发表时间：
2020-09
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通讯作者：
I. Pascucci;A. Banzatti;U. Gorti;M. Fang;K. Pontoppidan;R. Alexander;G. Ballabio;S. Edwards;C. Salyk;G. Sacco;E. Flaccomio;G. Blake;A. Carmona;C. Hall;I. Kamp;H. Käufl;G. Meeus;M. Meyer;T. Pauly;S. Steendam;M. Sterzik
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作者：
I. Pascucci;A. Banzatti;U. Gorti;M. Fang;K. Pontoppidan;R. Alexander;G. Ballabio;S. Edwards;C. Salyk;G. Sacco;E. Flaccomio;G. Blake;A. Carmona;C. Hall;I. Kamp;H. Käufl;G. Meeus;M. Meyer;T. Pauly;S. Steendam;M. Sterzik
我们分析了来自不同演化阶段的31个盘样品的高分辨率（Δv ≤ 10 km s−1）光学和红外光谱，包括[O i] λ6300和[Ne ii] 12.81 μm谱线。在光学波长的工作之后，我们使用高斯轮廓来拟合[Ne ii]线，并将它们分为高速分量（HVC）或低速分量（LVC），如果线的质心相对于恒星径向速度的蓝移大于或小于30 km s−1，则分别进行分类。与[O i]不同，其中HVC通常伴随着LVC，具有[Ne ii]检测的所有17个源具有HVC或LVC。[Ne ii] HVC在高吸积体（M yr−1）附近被优先探测到，而LVC则在低[O i]光度和大红外光谱指数（n13-31）的源中被发现。有趣的是，[Ne ii]和[O i] LVC亮度在n13-31时表现出相反的行为：随着内部尘埃盘的耗尽（较高的n13-31），[Ne ii]亮度增加，而[O i]减弱。[Ne ii]和[O i] HVC曲线通常是相似的，质心和半高宽显示了微射流中冲击气体的预期行为。相比之下，[Ne ii] LVC分布通常比[O i]分布更蓝移且更窄。的FWHM和质心与磁盘倾角表明，[Ne II] LVC主要跟踪未结合的气体从一个缓慢的，广角风，还没有完全失去开普勒签名从其发射区域。我们勾画了一个进化的情况下，可以解释合并[O i]和[Ne ii]的结果，包括屏蔽硬（101千电子伏）X射线在内部，主要是分子，MHD风。
We analyze high-resolution (Δv ≤ 10 km s−1) optical and infrared spectra covering the [O i] λ6300 and [Ne ii] 12.81 μm lines from a sample of 31 disks in different evolutionary stages. Following work at optical wavelengths, we use Gaussian profiles to fit the [Ne ii] lines and classify them into high-velocity component (HVC) or low-velocity component (LVC) if the line centroid is more or less blueshifted than 30 km s−1 with respect to the stellar radial velocity, respectively. Unlike for the [O i], where an HVC is often accompanied by an LVC, all 17 sources with an [Ne ii] detection have either an HVC or an LVC. [Ne ii] HVCs are preferentially detected toward high accretors ( M⊙ yr−1), while LVCs are found in sources with low , low [O i] luminosity, and large infrared spectral index (n13–31). Interestingly, the [Ne ii] and [O i] LVC luminosities display an opposite behavior with n13–31: as the inner dust disk depletes (higher n13–31), the [Ne ii] luminosity increases while the [O i] weakens. The [Ne ii] and [O i] HVC profiles are generally similar, with centroids and FWHMs showing the expected behavior from shocked gas in microjets. In contrast, the [Ne ii] LVC profiles are typically more blueshifted and narrower than the [O i] profiles. The FWHM and centroid versus disk inclination suggest that the [Ne ii] 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 [O i] and [Ne ii] results and includes screening of hard (∼1 keV) X-rays in inner, mostly molecular, MHD winds.