Comparative modelling of the spectra of cool giants
Comparative modelling of the spectra of cool giants
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DOI：
10.1051/0004-6361/201219142
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发表时间：
2012-09
影响因子：
6.5
通讯作者：
T. Lebzelter;U. Heiter;C. Abia;Kjell Eriksson;Michael J. Ireland;Michael J. Ireland;H. Neilson;W. Nowotny;J. Maldonado;Thibault Merle;Robert W. Peterson;B. Plez;C. Short;G. Wahlgren;C. Worley;B. Aringer;S. Bladh;P. Laverny;A. Goswami;Alcione Mora;R. Norris;A. Recio-Blanco;Michael Scholz;Michael Scholz;F. Thévenin;T. Tsuji;G. Kordopatis;B. Montesinos;R. Wing
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文献类型：
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作者：
T. Lebzelter;U. Heiter;C. Abia;Kjell Eriksson;Michael J. Ireland;Michael J. Ireland;H. Neilson;W. Nowotny;J. Maldonado;Thibault Merle;Robert W. Peterson;B. Plez;C. Short;G. Wahlgren;C. Worley;B. Aringer;S. Bladh;P. Laverny;A. Goswami;Alcione Mora;R. Norris;A. Recio-Blanco;Michael Scholz;Michael Scholz;F. Thévenin;T. Tsuji;G. Kordopatis;B. Montesinos;R. Wing
上下文我们从恒星光谱中提取信息的能力取决于可靠的恒星大气模型和适当的光谱合成技术。目前已有各种用于分析恒星光谱的模型代码和策略。目标。我们的目的是比较使用不同的大气模型和不同的分析策略推导恒星参数的结果。重点是冷巨星的高分辨率光谱学。方法.代表四颗冷巨星的光谱提供给从事光谱合成领域工作的各种团体和个人，请他们从所提供的数据中推导出恒星参数。2010年在维也纳举行的一次研讨会上讨论了研究结果。目前天文学界用于分析恒星光谱的大多数主要代码都包括在这次实验中。结果我们提出的结果，从不同的群体，以及一个额外的实验比较合成光谱的各种代码为一组给定的恒星参数。对结果的异同进行了讨论。结论.几种有效的方法来分析一个星星的给定光谱的结果在相当广泛的解决方案。不同小组得出的参数差异的主要原因似乎在于实际输入数据和分析方法的细节。这清楚地表明，我们离确定的丰度分析还有多远。
Context. Our ability to extract information from the spectra of stars depends on reliable models of stellar atmospheres and appropriate techniques for spectral synthesis. Various model codes and strategies for the analysis of stellar spectra are available today. Aims. We aim to compare the results of deriving stellar parameters using different atmosphere models and different analysis strategies. The focus is set on high-resolution spectroscopy of cool giant stars. Methods. Spectra representing four cool giant stars were made available to various groups and individuals working in the area of spectral synthesis, asking them to derive stellar parameters from the data provided. The results were discussed at a workshop in Vienna in 2010. Most of the major codes currently used in the astronomical community for analyses of stellar spectra were included in this experiment. Results. We present the results from the different groups, as well as an additional experiment comparing the synthetic spectra produced by various codes for a given set of stellar parameters. Similarities and differences of the results are discussed. Conclusions. Several valid approaches to analyze a given spectrum of a star result in quite a wide range of solutions. The main causes for the differences in parameters derived by different groups seem to lie in the physical input data and in the details of the analysis method. This clearly shows how far from a definitive abundance analysis we still are.