38 W. A. Norton on the Variations of the Declination 
law of variation of the individual currents with the distance from 
the points at which they originate, and on the position of t 
diurnal circle traced by the zenith among the ecliptic currents, 0 
on the sun’s distance from the zenith at noon. ‘The previous 
cussion has not revealed these laws, it has only served to confir 
the natural supposition that the intensity of each individual cul 
rent decreases in both directions from the point of original excit 
ment, aud made known the comparative intensities of the cu 
_ rents which pass through the zenith at noon in the differen 
months of the year. Avoiding, for the present, all speculation 
at an ticular instant the current which is at any given d 
tance fror int underneath the sun has the same intens 
as the current which passes through the zenith on that day 
which the zenith is at the same given distance from the point 
of a current depends 
of the point at which i gina 
phere which has the sun in its zeni 
should be the case unless there are inequa 
Adopting this supposition, then, we ma fror 
given in the Table on p. 34 that, beginning at a po 
from the sun, the ecliptic currents gradually increase in intens 
until we reach the distance of about 45°, but that from this po 
to 67° they retain pretty nearly the same intensity. Beyond 67° 
toward the horizon, we must conclude that the currents in ques 
tion, if they have their origin in any direct solar action, in all 
probability diminish in intensity. Whatever may be the law 
distribution of the ecliptic currents over the photosphere, at a 
moment, it is important to remark that, except as there may 
inequalities in the photosphere, it should be the same at alls 
sons; and therefore that the ads 
very i 
] 9 
nstance, entirely on the distane 
s 
“a 
hemispheres (e. g. at Hobarton as at Toronto), f 
the above conclusions ‘are correct then the difference of in 
tensity of currents on opposite sides of the zenith must beg 
at 6 a. mM. or 6 p.m. than at noon, and hence there should be a 
dency to a diminution of the vertical force from 6 a. m. to nooD 
aud to an augmentation from noon to 6 p.m. But if the eclip 
eurrents after their excitation subside gradually, from hour t 
honr, we shall have in action at noon the differences of all t 
residual currents consequent upon the forenoon excitation, and ai 
p.m. the differenves of all the residual currents result 
from the sin’s action during the whole day. The tendency 
these residual currents will be to make the vertical foree gr 
