Mira变星猎户座S的J，H，K光谱干涉测量
J, H, K spectro-interferometry of the Mira variable S Orionis
摘要：
目的：我们提出了J，H，K干涉光谱分辨率为35的Mira变量S Orionis。我们的目标是测量的直径变化作为波长的函数，预期由于分子层位于连续形成光球。研究方法：在相位0.78处，使用VLTI/AMBER仪器，使用条纹跟踪仪FINITO，在1.29和2.32 μ之间的29个光谱通道处获得了S Ori的可见度数据。计算每个光谱通道的表观均匀圆盘（UD）直径。此外，能见度数据直接与最近的自激动力学模型大气的预测进行了比较。结果如下：S Ori显示了可见度值作为光谱通道的函数的显著变化，其只能通过表观角度大小随波长的明显变化来描述。闭合相位值在所有光谱通道处接近于零，指示不存在不对称强度特征。表观UD角直径在约1.3和1.7 μ处最小，并且在约2.0 μ处增加约1.4倍。最小UD角直径为8.1 pm 0.5 mas，对应于~420 R_sun。S Ori能见度数据和明显的UD变化可以合理地解释了一个动态的大气模式，包括分子层。结论：测得的能见度和UD直径随波长的变化类似，并普遍证实了最近的动态模型大气的预测。[删节]
英文摘要：
Aims: We present J, H, K interferometry with a spectral resolution of 35 for the Mira variable S Orionis. We aim at measuring the diameter variation as a function of wavelength that is expected due to molecular layers lying above the continuum-forming photosphere. Methods: Visibility data of S Ori were obtained at phase 0.78 with the VLTI/AMBER instrument using the fringe tracker FINITO at 29 spectral channels between 1.29 and 2.32 mu. Apparent uniform disk (UD) diameters were computed for each spectral channel. In addition, the visibility data were directly compared to predictions by recent self-excited dynamic model atmospheres. Results: S Ori shows significant variations in the visibility values as a function of spectral channel that can only be described by a clear variation in the apparent angular size with wavelength. The closure phase values are close to zero at all spectral channels, indicating the absence of asymmetric intensity features. The apparent UD angular diameter is smallest at about 1.3 and 1.7 mu and increases by a factor of ~1.4 around 2.0 mu. The minimum UD angular diameter is 8.1 pm 0.5 mas, corresponding to ~420 R_sun. The S Ori visibility data and the apparent UD variations can be explained reasonably well by a dynamic atmosphere model that includes molecular layers. Conclusions: The measured visibility and UD diameter variations with wavelength resemble and generally confirm the predictions by recent dynamic model atmospheres. [abridged]
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