96 
DR. C. CHEEE; SOME PHENOMENA OF SUNSPOTS AND OF 
1892, 1893, and 1894, led to some very striking results, which are given in Table X. 
Use was made in the calculations of figures going one decimal place beyond the figures 
in Tables Y. and VII. 
Data in Table X., in the lines to which the letter A is attached, answer to the case 
where n is the representative day of largest sunspot area ; those in the lines to which 
B is attached answer to the case where n is the representative day of smallest spot 
area. By A —B is meant the algebraic excess of the A figures over the corresponding 
B figures. 
Table X.— Excess of Percentage Figure for Day n + s over That for Day n — s 
for Years 1892 to 1894 in Tables V. and YII. 
5. 
1. 
2. 
3. 
4. 
5. 
6. 
7. 
9. 
10. 
11. 
12. 
13. 
14. 
15. 
H 1 
[A. . 
+ 
18 
+ 28 
+ 38 
+ 36 
+ 40 
+ 33 
+ 21 
+ 
17 
+ 14 
+ 5 
- 5 
-12 
- 10 
-9 
-8 
ranges 
lb. . 
— 
8 
- 8 
- 12 
-14 
- 11 
- 12 
- 9 
— 
8 
- 9 
- 6 
- 3 
- 14 
- 11 
-5 
-6 
A- 
-B. . 
+ 
26 
+ 36 
+ 50 
+ 50 
+ 51 
+ 45 
+ 30 
+ 
25 
+ 23 
+ 11 
- 2 
+ 2 
+ 1 
-4 
-2 
Character 
fA. . 
+ 
25 
+ 42 
+ 49 
+ 44 
+ 41 
+ 38 
+ 27 
+ 
21 
+ 21 
+ 11 
+ 10 
- 3 
- 1 
+ 2 
-2 
figures 
LB. . 
20 
-20 
- 11 
- 19 
-13 
- 15 
- 11 
— 
17 
- 15 
-10 
-16 
-18' 
-11 
-6 
-3 
A- 
-B . . 
+ 
45 
+ 62 
+ 60 
+ 63 
+ 54 
+ 53 
+ 38 
+ 
38 
+ 36 
+ 21 
+ 26 
+ 15 
+ 10 
+ 8 
+ 1 
Every B figure in Table X. is negative. For values of s up to 9 this may reasonably 
be ascribed to the passage of the pulse of low sunspot area centering at day s = 0. 
But for higher values of s it seems to arise from a pulse of high values in both range 
and character figures having its crest about day 7i — V2 or li—11. This presumably is 
a more or less distinct phenomenon. 
The spot area at the crest of the pulse of large spot area for the years 1892 to 1894, 
now under consideration, was 98 per cent, in excess of the mean for the 31 days, while 
the spot area at the trough of the pulse of small spot area showed a deficiency of only 
67 per cent, from the 31-day mean. ■ One would thus have expected the A figures in 
Table X. to exceed the B figures numerically, but the excess shown is larger than 
would have been anticipated. Thus, in this instance, a deficiency of sunspots below 
the mean seems to have exerted a smaller influence than a corresponding excess. 
The large size of the percentage excesses in Table X., and the regularity in the 
figures for values of s up to 10, are phenomena of so striking a character that a 
warning seems desirable against attaching undue significance to them. From 1892 to 
1894 there must have been a very close parallelism between the variations of sunspot 
areas and H ranges, pulses in the latter quantity tending to follow those of the former 
after an interval averaging about 4 days; but in view of the differences between the 
