NIR SPECTROSCOPY OF THE HAeBe STAR HD 100546. III. FURTHER EVIDENCE OF AN ORBITING COMPANION?
NIR SPECTROSCOPY OF THE HAeBe STAR HD 100546. III. FURTHER EVIDENCE OF AN ORBITING COMPANION?
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HAeBe STAR HD 100546 的近红外光谱。 III。
DOI：
10.1088/0004-637x/791/2/136
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
M. Meyer
中科院分区：
文献类型：
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作者：
S. Brittain;J. Carr;J. Najita;S. Quanz;M. Meyer
我们报告了赫比格Be星星HD 100546的CO和OH发射的高分辨率近红外光谱。我们讨论了我们的结果如何与几个理论预测的巨行星形成的路标惊人的相似。CO和OH发射线的性质与我们先前的解释一致，这些诊断提供了一个伴星的间接证据，该星星靠近盘壁（在1013 Au）。OH谱线轮廓的不对称性和它们缺乏时间变化性与在惯性系中近似静止的盘壁处的偏心轨道中的气体的发射是一致的。CO v = 1-0发射线的时变光谱性质指向一个轨道源的CO发射与发射面积类似的预期为一个环行星盘（AU0.1 AU 2）假设CO发射是光学厚。我们还考虑了一个反假设，这种解释，即可变CO排放产生的亮点上的磁盘壁。最后，我们提出了一个简短的建议，进一步的工作，可以区分这些情况。
We report high-resolution NIR spectroscopy of CO and OH emission from the Herbig Be star HD 100546. We discuss how our results bear striking resemblance to several theoretically predicted signposts of giant planet formation. The properties of the CO and OH emission lines are consistent with our earlier interpretation that these diagnostics provide indirect evidence for a companion that orbits the star close to the disk wall (at ∼13 AU). The asymmetry of the OH spectral line profiles and their lack of time variability are consistent with emission from gas in an eccentric orbit at the disk wall that is approximately stationary in the inertial frame. The time variable spectroastrometric properties of the CO v = 1–0 emission line point to an orbiting source of CO emission with an emitting area similar to that expected for a circumplanetary disk (∼0.1 AU2) assuming the CO emission is optically thick. We also consider a counterhypothesis to this interpretation, namely that the variable CO emission arises from a bright spot on the disk wall. We conclude with a brief suggestion of further work that can distinguish between these scenarios.