Das Sternsystem: Erster Teil I by R. H. Curtiss (auth.), Fr. Becker, A. Brill, R. H. Curtiss,

By R. H. Curtiss (auth.), Fr. Becker, A. Brill, R. H. Curtiss, K. Lundmark (eds.)

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Identifications of single line criteria for which wave lengths are used will be found below in connection with the DRAPER Classification. Spectral regions used as criteria arc denoted hy wave lengths of their limits connected by hyphens. The mathematical symbols for "is greater than" and "is less than" arc used here in the sense, "is stronger than" and "is weaker than" respectively. Tht· other mathematical symbols will be readily understood. I{oman numerals always refer to spectral groups. Comparisons, such as weaker or stronger, always refer to the adjacent group to the left unless otherwise specified.

Criteria that carryover are repeated on each page so that the full description of each group can be readily Table 2. Miss MAURY'S Classification of Stellar Spectra. Criteria A. 4686 XXII IV v Rather narrow Difficult Not seen Rather narrow Difficult Not seen VI VII Strong E 1°,5 x 4026 1 Band , , 4543 4026 About 0,5 4089 Very strong (1) 4097 Strong 4116 Weak (2) 4070, 4073,4076 Weak (3) 4121 Weak 4200 4026 III II = > 4026, 4116 About same I> 1,2, 3,4' Rather narrow Absent >1 Rather narrow Narrow > I : At least 2xII Conspicuous 4472 4026 Much 1 (4) 4144 Not seen !

6826, RA. 19h42,1ID, Dec. C. 6326, RA. 17h12,9 ID, Dec. - 51 °40'. The chief nebular line, 5007,0, is the strongest line. The greater number of gaseous nebulae belong to this and the following class .. Class Pe. 7662, RA. 23 h21,1ID, Dec. 7009, RA. 20h58,7 ID, Dec. - 11 °46'. This class differs from class Pd in having line He II 4685,7 also present. 71 °32'. A bright Class Pf. 40, RA. Oh7,6 ID, Dec. band centered at 4650, probably due to carbon, is the most conspicuous feature of this spectrum and appears to ally it with spectra of Class O.

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