HD 100546的高分辨率近红外光谱：I。非对称性滚转振动OH发射线的分析
High-Resolution Near Infrared Spectroscopy of HD 100546: I. Analysis of Asymmetric Ro-Vibrational OH Emission Lines
摘要：
我们目前的观测从赫比格Be星HD 100546的振转OH和CO的排放。这两个分子的发射都来自于从中心恒星延伸约13 AU的圆盘内部区域。OH线的速度分布比[O I] 6300埃线的速度分布窄，表明盘中的OH与O I不是共空间的。这表明，内部的光学薄区域的磁盘是在很大程度上缺乏分子气体。与振转CO发射线不同，OH线是高度不对称的。我们表明，平均CO和平均OH线的配置文件可以与一个模型的磁盘组成的偏心内壁和圆形外盘。在这个模型中，绝大多数的OH通量（75%）起源于内壁，而绝大多数的CO通量（65%）起源于半径大于13 AU的盘表面。偏心内盘的流体动力学模拟包含嵌入的巨行星的拱星盘预测。我们讨论了这样一个磁盘的几何形状的行星盘潮汐相互作用的模型光的影响，并提出了替代解释的起源的不对称性。
英文摘要：
We present observations of ro-vibrational OH and CO emission from the Herbig Be star HD 100546. The emission from both molecules arises from the inner region of the disk extending from approximately 13 AU from the central star. The velocity profiles of the OH lines are narrower than the velocity profile of the [O I] 6300 Angstrom line indicating that the OH in the disk is not cospatial with the O I. This suggests that the inner optically thin region of the disk is largely devoid of molecular gas. Unlike the ro-vibrational CO emission lines, the OH lines are highly asymmetric. We show that the average CO and average OH line profiles can be fit with a model of a disk comprised of an eccentric inner wall and a circular outer disk. In this model, the vast majority of the OH flux (75%) originates from the inner wall, while the vast majority of the CO flux (65%) originates on the surface of the disk at radii greater than 13 AU. Eccentric inner disks are predicted by hydrodynamic simulations of circumstellar disks containing an embedded giant planet. We discuss the implications of such a disk geometry in light of models of planet disk tidal interactions and propose alternate explanations for the origin of the asymmetry.
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