352 
THE REV. STEPHEN J. PERRY ON THE MAGNETIC 
Table XIV. (continued). 
Station. 
Date. 
Chronometer. 
Error at 
Noon. 
Daily 
Bate. 
Azimuthal 
distance of sun 
from mark. 
Azimuthal 
reading of 
magnet. 
Azimuthal 
reading of 
mark. 
1871. 
h m s 
m a 
o / // 
Sept. 6 
2 41 113 f.m. 
+31 12-63 
98 36 0 
2 46 41-8 
100 5 0 
2 52 1-6 
101 30 30 
2 57 20 1 
102 54 45 
O / // 
3 22 0 
125 17 57-5 
3 28 0 
125 18 16-9 
91 37 15 
7 
11 13 3S-6 a m. 
31 16-88 
96 9 45 
IMS 590 
97 56 30 
11 25 2-8 
99 59 0 
11 30 57-5 
102 0 30 
1 2 3 30 p m 
253 23 21 0 
12 •• 0 
253 23 1-5 
153 6 5 
9 
11 31 1-4 A.M. 
31 25-37 
28 50 30 
11 42 56 0 
24 46 30 
11 51 581 
21 39 30 
270 2 22-3 
12 13 0 
270 3 20 7 
122 5 30 
1 27 0 
269 53 23 0 
1 31 30 
269 52 44 0 
122 6 30 
„ 12 
8 58 23 - 4 a.m. 
31 38-10 
13 55 52 
9 3 53 1 
15 14 22 
9 10 5-6 
16 45 22 
9 15 59 0 
18 11 22 
9 58 0 
112 17 20-9 
10 2 30 
112 16 42 0 
237 37 15 
„ 14 
3 8 6-5 p.m. 
31 46-69 
19 17 45 
3 17 18 4 
21 34 0 
3 26 49-9 
23 52 0 
4 0 30 
186 1 46 6 
4 5 30 
186 1 40 1 
237 12 5 
16 
31 55 08 
58 44 30 
9 1 37-8 
60 10 15 
9 6 41 1 
61 23 30 
9 10 511 
62 24 0 
9 50 30 
192 31 21-4 
9 57 0 
192 30 24-2 
10 1 0 
192 31 42 1 
94 1 10 
Alost 
„ 19 
q 12 9- 1 
32 7-81 
24 10 30 
9 17 14 8 
22 52 45 
10 33 0 
251 28 6-7 
10 38 30 
251 28 52-2 
10 44 0 
251 29 24-6 
240 31 35 
Brussels, 131 rue Royale 
„ 20 
2 12 39 5 p.m. 
32 1206 
17 24 0 
2 21 46-5 
14 54 15 
2 57 30 
188 1.3 38-6 
3 3 O 
261 28 50 
Brussels Observatory ... 
22 
?» — 
9 55 45 -S a.m. 
32 20-55 
32 42 45 
10 0 56 0 
31 18 15 
10 51 30 
181 57 24-2 
10 58 30 
181 55 14 4 
192 25 0 
22 
11 13 44-4 
10 17 45 
11 19 11-5 
8 35 15 
11 49 30 
181 42 30-6 
1154 0 
181 40 46-8 
192 47 37-5 
To complete the determination of the Declination at the different stations, it is necessary 
to compute the azimuth of the sun at the times of observation. The mean result for each 
station is contained in the following Table, along with the Declination corrected for Scale- 
reading, as well as for Daily Range, and for any irregular perturbation that may have 
occurred at the moment of observation. Fortunately the magnet was always very quiet 
during the hours of observation, and hence the greater part of the correction in each 
case is due to Daily Range, which can be estimated more correctly than could the effect of 
any great disturbance. In order to calculate this correction, I have been obliged to make 
