Science. 1967 Dec 8;158(3806):1273-9. doi: 10.1126/science.158.3806.1273.
According to theories of model stellar atmospheres only stars of spectral types from O to about B3 may be expected to be bright in the ultraviolet-wavelength region. Observations of the strong resonance lines between 911.6 and 1900 A will yield new information permitting construction of better models for the outermost layers of OB stars. However, an adequate theory of line-formation, including non-l.t.e. effects, should be used if an accurate physical representation is to result. Already it has been demonstrated beyond doubt that O and B0 supergiants are surrounded by expanding atmospheres.
根据恒星模型理论，只有光谱类型从 O 到大约 B3 的恒星才可能在紫外线波长区域中发光。对 911.6 和 1900 A 之间的强共振线的观测将提供新的信息，允许为 OB 恒星的最外层构建更好的模型。然而，如果要得到准确的物理表示，就应该使用包括非局部热平衡效应在内的合适的谱线形成理论。已经毫无疑问地证明，O 和 B0 超巨星被膨胀的大气层所包围。
