then we find 
3 
- 
pd zi -ompeley 
r B B, 
en 1 + DE P,(sin d) + Pi P,(sin d) + to 
The value of w is different for different latitudes. At the equator 
the period of rotation is nearly 
T= 9502. 
In higher latitudes in the northern hemisphere it is about 
P= 905506 
while in the southern hemisphere the average is 
7 == BoP. 
In the northern hemisphere 7, appears to increase somewhat from 
the equator to the pole, while in the southern hemisphere there seems 
to be a slight decrease '). These results are, however, still rather 
uncertain and it seems better to adopt a mean value. 
For 7, = 9507.5 we have 0, = 0.09017 
and. tor 7 == A09 Ie i, = yy AEL 
If now we write the equation (1) first for a point on the equator 
[r=6], and then for the pole |r=6(1—e,)|, taking both times g = 9,, 
we find the following condition determining «, 
1 B, 9473 3 B 53 
gek Reden NT [124] + $ De as]. 
where 
L 
,= 
= (ener 
I thus find 
e, = 0.06494 —1/,..,, 
From the eclipses of the satellites observed at Harvard College | 
derived ?): 
From satellite I e= 0.0604 + .00380 
3 vs II (0764-29715 
ys eed 0544 + 30 
7 sf [V ‚0649 + 10 
It is well known that also the values of ¢ derived by different 
observers from micrometrical measures of the diameters are very 
discordant. They range from about 0.055 to 0.075. The value derived 
1) Srantey Wittiams, Observatory 1913, page 465. 
*) Monthly Notices LXXI. page 96. 
