FURTHER STUDIES OF STELLAR ROTATION FROM COPERNICUS SATELLITE DATA.
FURTHER STUDIES OF STELLAR ROTATION FROM COPERNICUS SATELLITE DATA.
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根据哥白尼卫星数据进一步研究恒星旋转。
DOI：
10.1086/130490
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发表时间：
1979
期刊：
影响因子：
--
通讯作者：
J. Cassidy
中科院分区：
文献类型：
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作者：
J. Hutchings;J. Nemec;J. Cassidy
旋转加宽的线宽是通过 26 颗 O 和 B 星的 lambda 光谱扫描来测量的。其中大约一半在可见光谱区域测量到类似的量。这些线宽的比率以及 V crit 和 V sin i 的值被导出并用于估计 24 颗星的 omega 和 i。讨论了 Hutchings (1976) 简单理论的适用性，并检查和讨论了来自本次和之前研究的 B 和 Be 星整个样本的 omega 和 i 的分布。特别令人感兴趣的是，Be 星不会以 V Crit' 旋转，并且旋转轴具有随机分布。
Rotationally broadened line widths are measured from lambda spectrum scans of 26 O and B stars. Similar quantities are measured in the visual spectral region for about half of them. The ratio of these line widths, and values for V crit and V sin i are derived and used to estimate omega and i for 24 stars. The applicability of the simple theory of Hutchings (1976) is discussed and the distributions of omega and i for the whole samples of B and Be stars from this and previous investigations are examined and discussed. Of particular interest is the indication that Be stars do not rotate at V crit' and have a random distribution of rotational axes.