对上天球的高分辨率光学观测：吸积和盘风共同演化的证据
A High-resolution Optical Survey of Upper Sco: Evidence for Coevolution of Accretion and Disk Winds
摘要：
磁流体动力学（MHD）和光蒸发风被认为在行星形成盘的演化和扩散中起着重要作用。在这里，我们分析了高分辨率（$Δv \sim$ 7公里$^{-1}$）的光学光谱从样本的115 T金牛星在$\sim 5-10$ Myr上斯科协会和专注于[O I] $λ$ 6300和H $α$线跟踪盘风和吸积，分别。我们的样本覆盖了很大的光谱类型范围，我们将其分为温暖（G 0-M3）和凉爽（晚于M3），以便于与年轻地区进行比较。我们在87个具有原行星盘的上SCO源中的45个中检测到[O I] $λ$ 6300线，并且在45个中的32个中基于H $α$轮廓和等效宽度进行吸积。所有[O I] $λ$ 6300上Sco曲线均具有低速（质心$< -30$ kms $^{-1}$，LVC）发射，并且大多数（36/45）可通过单个高斯（SC）拟合。质心速度和半高宽的SC分布与磁流体圆盘风的分布一致。我们还发现，上Sco样品与年轻样品一样，也遵循同样的吸积光度$-$ LVC [O I] $λ$ 6300光度关系和SC FWHM与WISE W3-W 4谱指数之间的反相关。这些结果表明，吸积和盘风共同演变，并作为内部磁盘清除，风排放产生进一步远离恒星。最后，我们的大光谱范围的覆盖范围显示，冷星有较大的FWHM标准化的恒星质量比温暖的恒星，表明[O I] $λ$ 6300的发射产生更接近低质量/低光度的恒星。
英文摘要：
Magnetohydrodynamic (MHD) and photoevaporative winds are thought to play an important role in the evolution and dispersal of planet-forming disks. Here, we analyze high-resolution ($Δv \sim$ 7 kms$^{-1}$) optical spectra from a sample of 115 T Tauri stars in the $\sim 5-10$ Myr Upper Sco association and focus on the [O I]$λ$6300 and H$α$ lines to trace disk winds and accretion, respectively. Our sample covers a large range in spectral type and we divide it into Warm (G0-M3) and Cool (later than M3) to facilitate comparison with younger regions. We detect the [O I]$λ$6300 line in 45 out of 87 upper sco sources with protoplanetary disks and 32 out of 45 are accreting based on H$α$ profiles and equivalent widths. All [O I] $λ$6300 Upper Sco profiles have a low-velocity (centroid $< -30$ kms$^{-1}$, LVC) emission and most (36/45) can be fit by a single Gaussian (SC). The SC distribution of centroid velocities and FWHMs is consistent with MHD disk winds. We also find that the Upper Sco sample follows the same accretion luminosity$-$LVC [O I]$λ$6300 luminosity relation and the same anti-correlation between SC FWHM and WISE W3-W4 spectral index as the younger samples. These results indicate that accretion and disk winds coevolve and that, as inner disks clear out, wind emission arises further away from the star. Finally, our large spectral range coverage reveals that Cool stars have larger FWHMs normalized by stellar mass than Warm stars indicating that [O I]$λ$6300 emission arises closer in towards lower mass/lower luminosity stars.
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