旋转对织女星光谱的影响
The effect of rotation on the spectrum of Vega
摘要：
织女星是一颗快速旋转的极上星的发现，引发了许多关于这个基本标准的问题，包括它的组成，以及它的质量和年龄。我们在这里报告的织女星的组成重新分析。一个完整的光谱合成的基础上罗氏模型推导出较早的NPOI干涉测量。我们发现在织女星的光谱线的形状是更复杂的，而不仅仅是平底，这是以前报道的;配置文件的范围从轻微的自反转到简单的“V”形。一个高信噪比的光谱，从EQUIPDIE档案的叠加光谱，显示出良好的协议与计算，提供我们添加约10公里/秒的宏观湍流的预测光谱。从丰度分析中，我们发现织女星表现出了以前提出的\W牧夫座星的特殊丰度模式。我们调查的旋转推断丰度的影响，并表明，占主导地位的电离状态相比，使用非旋转模型的分析只有轻微的影响。我们认为，快速旋转需要的明星是完全混合。这种成分导致质量，特别是年龄与通常假设的情况相比有很大的不同。
英文摘要：
The discovery that Vega is a rapidly rotating pole-on star has raised a number of questions about this fundamental standard, including such issues as its composition, and in turn its mass and age. We report here a reanalysis of Vega's composition. A full spectral synthesis based on the Roche model derived earlier from NPOI interferometry is used. We find the line shapes in Vega's spectrum to be more complex than just flat-bottomed, which have been previously reported; profiles range from slightly self-reversed to simple ``V'' shapes. A high SNR spectrum, obtained by stacking spectra from the ELODIE archive, shows excellent agreement with the calculations, provided we add about 10 km/s of macroturbulence to the predicted spectra. From the abundance analysis, we find that Vega shows the peculiar abundance pattern of a \W Bootis star as previously suggested. We investigate the effects of rotation on the deduced abundances and show that the dominant ionization states are only slightly affected compared to analyses using non-rotating models. We argue that the rapid rotation requires the star be fully mixed. The composition leads to masses and particularly ages that are quite different compared to what are usually assumed.
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