91 
Explanation of table I: 
In this table 6(0,/) calculated for the values of cosi is given in the first column 
for three different values of A by the aid of (3). In column 3 the found values of 
b(0,i) have been multiplied by a factor in order to render a comparison with 
ABBOT’s values, recorded in the fourth column, possible. 
By the aid of (3) and Asspot’s values, which | subjoin, Drerant 
tries to draw a conclusion on the effective temperature of the sun. 
Wavelength in « Rn ye cer Ben 
0.323 Wn 
0.386 338 | 
0.433 456 | 
0.456 515 
0.481 en 
0.501 ns 
0.534 ae 
0.604 a 
0.670 Poe 
0.699 so 
0.866 en 
1.031 111 
1.225 17.6 
1.655 39.5 
2.097 14.0 
(ABBOT’s values). 
His reasoning is as follows: 
For 2 = 0 we obtain (0,0) i.e. formula (3) then gives for every wave- 
length 2 the intensity of radiation passing out in the centre of the sun’s 
disc, when that of the area of the photosphere for this 4 is put equal 
to |. What we measure is, however, not the quantity 6(0,0), but 
the radiation 2%, actually passing out, which is in relation with 6(0,0) 
through the formula: 
U), 4) 
b(0,0) ( 
in which /; is the intensity of radiation in the spectrum of the 
photosphere (considered as absolutely black body) for the wavelength 2. 
By the aid of (3) and (4) and ABBotr's values the following table 
can, therefore, be calculated for /; (table II). According to our 
