MK. LOUIS VESSO'r KING ON THE SCATTERING AND 
4-22 
Table XIII.— Pohi)-izatim of Sb/ Bailiafion Calcvlafed from Mount irUson and JFashvngfon Ohservations. 
Numerical results on the polarization of sky radiation are calculated from the approximate formulse 
given in Section 6. In order to save space numerical values corresponding to the formulce given at the 
foot of the table are entered in the same order under each value of A. and 
The values of 
P(0,C) = Ce-^U{C(secC-l)} 
and 
Q(0,0 = |r/C..<i’(C, 0) 
are obtained from Tables VI. and VIII. 
The ratios of the intensities of zenith sky polarized in the principal 2 )lane and in a j^lane at right angles 
to it are calculated in the form 
Ti( 0,0 ^ i+Q(o,D/P(o, 0 
T.,(o,0 cos-^t+Q(0,D/P(0,0 
The results are shown graphically in Diagram XIV. 
The ratios Q(0, ()/P (0, 1) given in the jiresent table compare the contribution of self-illumination to the 
sky intensity of different wave-lengths with the effect of direct sunlight on sky radiation. 
The ratios 
Q(0, C)/P(0, D 
1+Q(0, 0/P(0,t) 
compare the residual intensity of sky radiation over the great circle of most complete polarization 90° from 
the sun to the intensity polarized in a plane at right angles. It will be noticed that this ratio remains 
nearly the same for all zenith distances, and is very small for long wave-lengths when the effect of self¬ 
illumination is small. 
