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GIARPS High-resolution Observations of T Tauri stars (GHOsT)

机译：GIARPS T陶里星（GHOsT）高分辨率观测

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Context. The mechanism for jet formation in the disks of T Tauri stars remains poorly understood. Observational benchmarks to launching models can be provided by tracing the physical properties of the kinematic components of the wind and jet in the inner 100 au of the disk surface. Aims. In the framework of the GIARPS High-resolution Observations of T Tauri stars (GHOsT) project, we aim to perform a multi-line analysis of the velocity components of the gas in the jet acceleration zone. Methods. We analyzed the GIARPS-TNG spectra of six objects in the Taurus-Auriga complex (RY Tau, DG Tau, DL Tau, HN Tau, DO Tau, RW Aur A). Thanks to the combined high-spectral resolution ( ? = 5°0 000?115 000) and wide spectral coverage (~400?2400 nm) we observed several O?~(0), S?~(+), N?~(0), N?~(+), and Fe?~(+)forbidden lines spanning a large range of excitation and ionization conditions. In four objects (DG Tau, HN Tau, DO Tau, RW Aur A), temperature ( T _(e)), electron and total density ( n _(e), n _(H)), and fractional ionization ( x _(e)) were derived as a function of velocity through an excitation and ionization model. The abundance of gaseous iron, X(Fe), a probe of the dust content in the jet, was derived in selected velocity channels. Results. The physical parameters vary smoothly with velocity, suggesting a common origin for the different kinematic components. In DG Tau and HN Tau, T _(e), x _(e), and X(Fe) increase with velocity (roughly from 6000 K, 0.05, 10%X(Fe)_(⊙)to 15 000 K, 0.6, 90%X(Fe)_(⊙)). This trend is in agreement with disk–wind models in which the jet is launched from regions of the disk at different radii. In DO Tau and RW Aur A, we infer x _(e)< 0.1, n _(H)~ 10~(6?7)cm~(?3), and X(Fe) ? X(Fe)_(⊙)at all velocities. These findings are tentatively explained by the formation of these jets from dense regions inside the inner, gaseous disk, or as a consequence of their high degree of collimation.
机译：上下文。 T Tauri恒星盘中射流形成的机理仍然知之甚少。可以通过跟踪磁盘表面内部100 au中风和射流的运动学成分的物理属性来提供发射模型的观测基准。目的在GIARPS T Tauri恒星高分辨率观测（GHOsT）项目的框架内，我们旨在对射流加速区中气体的速度分量进行多线分析。方法。我们分析了Taurus-Auriga复杂区域（RY Tau，DG Tau，DL Tau，HN Tau，DO Tau，RW Aur A）中六个对象的GIARPS-TNG光谱。由于结合了高光谱分辨率（？= 5°000 000-11.5万）和宽光谱覆盖范围（〜400？2400 nm），我们观察到了几个O？〜（0），S？〜（+），N？〜 （0），N 2+（+）和Fe 2+（+）禁止线跨越大范围的激发和电离条件。在四个物体中（DG Tau，HN Tau，DO Tau，RW Aur A），温度（T _（e）），电子和总密度（n _（e），n _（H））和分数电离（x通过激发和电离模型得出_（e））作为速度的函数。在选定的速度通道中得出了丰富的气态铁X（Fe），它是射流中粉尘含量的探针。结果。物理参数随速度平稳变化，表明不同运动学成分的共同起源。在DG Tau和HN Tau中，T _（e），x _（e）和X（Fe）随速度增加（大约从6000 K，0.05，10％X（Fe）_（⊙）增加到15000 K， 0.6，90％X（Fe）_（⊙））。这种趋势与磁盘-风模型相吻合，在磁盘-风模型中，以不同半径从磁盘区域发射射流。在DO Tau和RW Aur A中，我们推断x _（e）<0.1，n _（H）〜10〜（6？7）cm〜（？3），X（Fe）？所有速度下的X（Fe）_（⊙）这些发现由内部气态盘内部密集区域形成的射流或由于其高度准直的结果而暂时解释。

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