凯克孔径掩蔽实验：1.1 - 3.8微米3个Mira变星的光谱干涉测量
The Keck Aperture Masking Experiment: spectro-interferometry of 3 Mira Variables from 1.1 to 3.8 microns
摘要：
我们目前的结果从光谱干涉研究的Miras o Cet，R狮子座和W Hya获得的凯克孔径掩蔽实验从1998年9月至2002年7月。光谱分散的可见度数据允许拟合与圆对称的亮度分布，如一个简单的均匀的磁盘。本文给出了在1.1-3.8微米范围内的~ 450个光谱通道上获得的恒星角直径。使用一个简单的统一磁盘亮度模型，便于历元之间的比较，并与现有的数据和理论模型。强烈的尺寸变化与波长记录的所有恒星，探测区的H2O，CO，OH和尘埃的形成。从我们的数据中提取的同时代的光谱的比较表明，所观察到的角直径和通量之间的强反相关。这些变化巩固了一个复杂的恒星大气的概念，包括分子壳与时间相关的密度和温度。我们的研究结果与现有的数据和脉动模型进行了比较。发现模型很好地再现了波长与角直径曲线的函数形式，尽管在2.8-3.5微米范围内注意到一些偏离。
英文摘要：
We present results from a spectro-interferometric study of the Miras o Cet, R Leo and W Hya obtained with the Keck Aperture Masking Experiment from 1998 Sep to 2002 Jul. The spectrally dispersed visibility data permit fitting with circularly symmetric brightness profiles such as a simple uniform disk. The stellar angular diameter obtained over up to ~ 450 spectral channels spaning the region 1.1-3.8 microns is presented. Use of a simple uniform disk brightness model facilitates comparison between epochs and with existing data and theoretical models. Strong size variations with wavelength were recorded for all stars, probing zones of H2O, CO, OH, and dust formation. Comparison with contemporaneous spectra extracted from our data show a strong anti-correlation between the observed angular diameter and flux. These variations consolidate the notion of a complex stellar atmosphere consisting of molecular shells with time-dependent densities and temperatures. Our findings are compared with existing data and pulsation models. The models were found to reproduce the functional form of the wavelength vs. angular diameter curve well, although some departures are noted in the 2.8-3.5 micron range.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
