Fig. B.2
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Some low-luminosity stars that may be classified as B8.5, compared to B8 V and B9 V standards. The earlier type of 21 Tau is confirmed by the presence of very weak He I 4009, 4713 Å lines, which cannot be seen in the spectra of the B8.5 V or B9 V stars. The weakening of He I 4026 Å is also obvious. ζ Peg would be close to the limit between the B8 and B8.5 subtypes.
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