Part 3 — TABLE XXXIII

Atom Line Pup Note

C++ 4649 0.0 2.0 9.0 6.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 .. 1

N+ 3996.9 0.0 0.0 0.0 0.0 5.0 6.0 7.0 .. 9.0 .. .. 5.0 0.0 1

N++ 4515.0 .. 9.0 4.0 4.0 1.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 2

4097.5 .. 15.0 8.0 5.0 .. 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 3

O+ 4943.4 0.0 0.0 0.0 0.0 4.0 4.0 3.0 0.0 0.0 0.0 0.0 0.0 0.0 1

4941.2

4705.3 0.0 0.0 0.0 2.0 4.0 4.0 3.0 0.0 0.0 0.0 0.0 0.0 0.0 2

4699.2

4676.2 0.0 0.0 0.0 2.0 5.0 .. 7.0 0.0 0.0 0.0 0.0 0.0 0.0 3

4661.6 0.0 0.0 0.0 2.0 5.0 .. 7.0 0.0 0.0 0.0 0.0 0.0 0.0 4

4649.1 0.0 0.0 0.0 6.0 9.0 12.0 9.0 .. 4.0 0.0 0.0 0.0 0.0 5

4641.8 0.0 0.0 0.0 0.0 3.0 10.0 7.0 .. 0.0 0.0 0.0 0.0 0.0 6

4596.2 0.0 0.0 0.0 1.0 5.0 .. 6.0 .. 3.0 0.0 0.0 0.0 0.0 7

4591.0 0.0 0.0 0.0 1.0 5.0 .. 6.0 .. 3.0 0.0 0.0 0.0 0.0 8

4417.0 0.0 0.0 0.0 5.0 6.0 11.0 3.0 .. 2.0 0.0 0.0 0.0 0.0 9

4415.9 0.0 0.0 0.0 3.0 .. 2.0 0.0 0.0 0.0 0.0 10

4366.9 0.0 4.0 4.0 4.0 .. 6.0 6.0 .. 1.0 0.0 0.0 0.0 0.0 11

4075.9 0.0 3.0 0.0 2.0 6.0 8.0 6.0 0.0 0.0 0.0 0.0 0.0 0.0 12

4072.2 0.0 0.0 0.0 2.0 7.0 9.0 6.0 0.0 0.0 0.0 0.0 0.0 0.0 13

4069.9 0.0 0.0 0.0 4.0 6.0 8.0 6.0 0.0 0.0 0.0 0.0 0.0 0.0 14

S+ 4815 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 x 0.0 0.0 0.0 1

4174.5 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 3.0 0.0 0.0 0.0 2

4162.9 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 3.0 0.0 0.0 0.0 3

S++ 4295 0.0 0.0 0.0 0.0 0.0 1.0 0.0 0.0 0.0 0.0 0.0 0.0 0.0 4

4285.0 0.0 0.0 0.0 0.0 0.0 6.0 4.0 0.0 0.0 0.0 0.0 0.0 0.0 5

4253.8 0.0 0.0 0.0 0.0 6.2 6.8 6.0 0.0 0.0 0.0 0.0 0.0 0.0 6

NOTES TO TABLE XXXIII

Atom Note Maximum Remarks

C++ 1 Line blended, in stars cooler than , with V+ 4649.1. Attributed by Fowler and Milne, and by Hartree, to C+++

N+ 1 Unblended

N++ 2

3 Blended with the Si+++ line at 4096, which is probably effective throughout the whole range

O+ 1

2

3 ?

4 ?

5 Blended with C++ line at 4649, which preponderates in stars hotter than , and probably contributes largely in that class

6

7

8

9

10

11 ? Certainly another line is here involved, but it has not been identified

12

13

14

S+ 1 2 3 Lines recorded by Lockyer; not measured by the writer

S++ 4 Line recorded by Lockyer. Intensity from H.A., 28; not measured by the writer

5

6 Recorded by H. H. Plaskett in 10 Lacertae

V. MATERIAL BEARING ON THE CLASSIFICATION OF STARS, QUOTED IN CHAPTER XII

IN illustration of the problem of Class , observations of sixty-two stars are collected in the following table. Successive columns contain the H.D. number, the name of the star, the apparent magnitude, the reduced proper motion , and the spectral class. Then follow columns which indicate the presence () or absence of metallic lines, the quality of the lines (sharp lines being represented by the letter and hazy lines by the letter ), the presence of wings to the hydrogen lines, and the strength of the Sr+ line at 4077 and the Si+ lines at 4128, 4131.

The stars in each class are arranged in order of increasing strength of metallic lines, and it will be seen that this feature is correlated with the strength of the silicon and strontium lines, but not with the line quality or the hydrogen wings, nor with the reduced proper motion.