Analysis of visibility data from the University of California/Berkeley Infrared Spatial Interferometer: radiative transfer modeling and results on fifteen stars
Analysis of visibility data from the University of California/Berkeley Infrared Spatial Interferometer: radiative transfer modeling and results on fifteen stars
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加州大学/伯克利分校红外空间干涉仪的可见度数据分析：十五颗恒星的辐射传输模型和结果
DOI：
10.1117/12.177247
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发表时间：
1994
期刊：
影响因子：
--
通讯作者：
C. Townes
中科院分区：
文献类型：
--
作者：
W. Danchi;M. Bester;L. Greenhill;C. Degiacomi;C. Townes
本文讨论了15颗晚型星的可见度数据及其分析。C.伯克利红外空间干涉仪（ISI）。ISI是一种在9至12微米波长范围内工作的双元件外差干涉仪，位于Mt。威尔逊能见度曲线计算使用辐射传输模型，并与能见度数据从ISI进行比较。A（chi）2拟合程序已被用来估计的尘埃壳，在11微米的光学深度的内半径，和温度的内半径。对于尘埃完全分解的恒星，也可以估计恒星的直径和温度。我们提出了初步的能见度数据的恒星NML天鹅座和IRC +10420最近获得的使用10米基线。此外，我们提出了初步的最近的数据和分析的六颗恒星，阿尔法猎户座，omicron Cet，IRC +10216，R狮子座，VY CMA和R Aqr使用32米的基线。猎户座阿尔法星的可见度数据涵盖了足够的空间频率范围，可以确定其直径。在95%置信区间内，我们获得的直径为0”.053+/- 0”.003。对于其他恒星最近的32米基线数据与以前的模型进行了比较，并进一步约束他们的一些参数。
We discuss visibility data and its analysis for 15 late-type stars observed with the U. C. Berkeley Infrared Spatial Interferometer (ISI). The ISI is a two-element heterodyne interferometer operating in the 9- to 12-micrometers wavelength region and is located at Mt. Wilson. Visibility curves were calculated using a radiative transfer model and compared with the visibility data from the ISI. A (chi) 2 fitting procedure has been used to estimate the inner radii of the dust shells, optical depths at 11 micrometers , and the temperature at the inner radii. For stars in which the dust is completely resolved estimates of the stellar diameter and temperature can also be made. We present preliminary visibility data for the stars NML Cyg and IRC +10420 obtained recently using a 10-m baseline. In addition, we present preliminary recent data and analysis for the six stars, alpha Ori, omicron Cet, IRC +10216, R Leo, VY CMA, and R Aqr using a 32-m baseline. The visibility data for alpha Ori covers a sufficient range of spatial frequencies to make a determination of its diameter. Within a 95% confidence interval we obtain a diameter of 0".053+/- 0".003. For the other stars the recent 32-m baseline data are compared with previous models and further constrains some of their parameters.