THE following tabulation shows the intensity changes of lines of unknown series relations that occur in the hotter stars. The arrangement follows that of [Table XIX]. Notes on the maxima and blends are appended.
[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