IN PASSING THROUGH THE ATMOSPHERE. 263 
Brientz. 
First Series. 
Second Series. 
Hour. 
Log v. 
X. 
Hour. 
Log v. 
X. 
8± 
1-3579 
1952 
10 
1-4409 
1244 
9 
1-4065 
1529 
11 
1-4579 
1113 
3 
1-3838 
1529 
12 
1-4857 
1073 
4 
1-2989 
2184 
1 
1-5024 
1111 
4i 
1-2095 
2874 
2 
1-4409 
1242 
Sum. . . 
10068 
Sum. . . . 
. 7-3278 
5783 
Mean. . 
. . T3313 
2014 
Mean . . . 
. . 1-4656 
1157 
Taking V 
= 1 . M = 
•7602, m = -0001567 
V expressed in actinometric degrees (B. 2.) 
= 44-35. 
Faulhorn. 
First Series, 
Second Series. 
Hour. 
Log v. 
X. 
Hour. 
Log v. 
X. 
1\ 
1-2601 
2197 
10 
1-5250 
957 
8? 
1-3892 
1501 
11 
1-5866 
857 
9 
1-4639 
1176 
12 
1-5717 
827 
3 
1-4698 
1178 
1 
1-5353 
85 7 
4 
1-3802 
1683 
2 
1-5224 
958 
4* 
1-3304 
2214 
Sum. . . 
. . 8-2936 
9949 
Sum. . . . 
. 77410 
4456 
Mean . . 
. . 1-3823 
1658 
Mean . . . 
. 1-5482 
891 
V — 1, 
[ 0 ] = -6848, 
m = -0002163 
V expressed in actinometric degrees (B. 2.) = 55’0 7- 
102. We thus find that when the extreme observations of each series are employed, 
the Faulhorn observations give a greater intensity to the extra-atmospheric radiation, 
and consequently a greater coefficient of extinction to the atmosphere, because the part 
of Curve XV. corresponding to the least thickness rises proportionably faster than 
the other part. But both results give greatly inferior extra-atmospheric radiation 
than the corrected hypothesis we have assumed ; the first set gives 44°, the second 55°, 
the corrected hypothesis as much as 73° for the extra-atmospheric radiation. 
103. If we avoid extreme columns and arrange the observations in alternating 
series so as to present a feeble but w r ell-ascertained mean difference, we shall have 
results somewhat different, and more accordant at the two stations. These are con- 
tained in the following Tables, of which the first gives V = 42° nearly, the second 
47° nearly, the difference being in the same direction as before. 
