In addition to the comprehensive data just quoted, there have been numerous determinations of the temperatures of individual bright stars, chiefly by Abbot,[52] Coblentz,[53] Sampson,[54] and H. H. Plaskett.[55] In the main these values confirm the scale given in [Table V], but sometimes considerable differences occur in the values given for individual stars by different investigators. At the same time, each observer is usually reasonably self-consistent, and the deviations must therefore be ascribed to differences of method. Some of the results are reproduced, for illustration, in [Table VI].
[TABLE V]
| Class | Wilsing | Rosenberg | E.S. King Color Temperature | E.S. King Total Radiation |
|---|---|---|---|---|
| 12300° | 30000° | 22700° | 22700° | |
| 11450 | 18000 | 15200 | 14900 | |
| 10250 | 1200 | 11600 | 11300 | |
| 9000 | 9000 | 8800 | 8600 | |
| 7950 | 7850 | 7900 | 7700 | |
| 6880 | 6930 | 7000 | 6800 | |
| 5980 | 6000 | 6040 | 5870 | |
| 5250 | 5200 | 5090 | 4950 | |
| 4570 | 4570 | 4570 | 4440 | |
| 3860 | 3840 | 3640 | 3550 | |
| 3550 | 3580 | 3430 | 3340 |
It is seen that the effective temperatures of individual hotter stars vary widely among themselves. This is largely a result of the difficulty of making the appropriate correction for atmospheric extinction. It must, then, be supposed that the temperatures derived by spectrophotometric methods are not trustworthy for stars hotter than Class
. The values determined by the earlier observers for the
and
classes are almost certainly too low. Rosenberg’s value of 30,000° for