标题： 利用1微米光谱探测T Tauri吸积和喷流 显示英文标题

标题： Probing T Tauri Accretion and Outflow with 1 Micron Spectroscopy

摘要： 在一项针对39颗经典T Tauri星的高色散1微米巡天中，检测到80%的恒星存在消光现象，97%的恒星出现He I 10830和Pgamma线发射。 平均而言，1微米的消光超过了之前已知的过量发射源所预期的水平，表明在恒星-盘界面区域存在额外的吸积光度贡献者。 这两条谱线的强度与消光现象相关联，在Pgamma处，随着消光现象的变化，谱线形态呈现出系统性的变化。 He I 10830对内风具有前所未有的敏感性，在71%的CTTS中显示出连续区以下的蓝移吸收，而在Pgamma处未发现任何蓝移吸收（0%）。 这条谱线同样对磁层吸积流敏感，在47%的CTTS中发现了连续区以下的红移吸收，而在Pgamma处这一比例仅为24%。 在10830处的蓝移吸收表现出其宽度和渗透深度进入连续区的显著多样性，这表明在吸积恒星中有多种内风条件存在。 我们将最宽且最深的蓝吸收解释为由流出气体对1微米连续区的散射形成，这些气体的完全加速区域包围着恒星，这表明恒星有径向外流。 相比之下，具有不同径向速度的窄蓝吸收更可能由内盘喷出的风对1微米连续区的散射产生。 由于这两种情况在非吸积WTTS中均未被观测到，因此恒星风和盘风都是由吸积驱动的。 在CTTS中，氦的强度与消光现象相关联。 显示英文摘要

摘要： In a high dispersion 1 micron survey of 39 classical T Tauri stars veiling is detected in 80%, and He I 10830 and Pgamma line emission in 97% of the stars. On average, the 1 micron veiling exceeds the level expected from previously identified sources of excess emission, suggesting the presence of an additional contributor to accretion luminosity in the star-disk interface region. Strengths of both lines correlate with veiling, and at Pgamma there is a systematic progression in profile morphology with veiling. He I 10830 has an unprecedented sensitivity to inner winds, showing blueshifted absorption below the continuum in 71% of the CTTS compared to 0% at pgamma. This line is also sensitive to magnetospheric accretion flows, with redshifted absorption below the continuum found in 47% of the CTTS compared to 24% at Pgamma. The blueshifted absorption at 10830 shows considerable diversity in its breadth and penetration depth into the continuum, indicating that a range of inner wind conditions exist in accreting stars. We interpret the broadest and deepest blue absorptions as formed from scattering of the 1 micron continuum by outflowing gas whose full acceleration region envelopes the star, suggesting radial outflow from the star. In contrast, narrow blue absorption with a range of radial velocities more likely arises via scattering of the 1 micron continuum by a wind emerging from the inner disk. Both stellar and disk winds are accretion powered since neither is seen in non-accreting WTTS and among the CTTS helium strength correlates with veiling.