( <fr4 ) 
ration of the Declination of Stars of different Luflre * 
for that is not fenfibly different in fuch Stars as feem 
near together, though they appear of very different 
Magnitudes. And whatever their Situations are (if I 
proceed according to the foregoing Hypothefis) I find 
the fame Velocity of Light from my Obfervations of 
fmall Stars of the fifth or fixth, as from thofe of the 
fecond and third Magnitude, which in all Probability 
are placed at very different Diftances from us. The 
fmall Star,for Example, before fpoken of, that is altnoft 
oppofite to y 'Draconis (being the 3 5th Camelopard. 
Hevelii in Mr. Flamfleed’s Catalogue) was 19" more 
Northerly about the Beginning of March than in Sep - 
tember . Whence I conclude, according to my Hypo- 
thefis, that the Diameter of the little Circle deferibed 
by a'Star in the Pole of the Ecliptic): would be 40", 2. 
The laft Star of the great Bear’s-tail of the 2d 
Magnitude (marked yi by Bayer) was 36" more South- 
erly about the Middle of January than in July. 
Hence the Maximum , or greateft Alteration of Decli- 
nation of a Star in the Pole of the Ecliptick would be 
4c", 4, exaftly the fame as was before found from the 
Obfervations of y c Draconis. 
TheStar of the 5-th magnitude in the Head of Ter feus 
marked r by Bayer, was 25" more Northerly about 
the End of T)ec ember than on the 29th of July fol- 
lowing. Hence the Maximum would be 41". 'This 
Star is not bright enough to be feen as it pafles over my 
Zenith about the End of June , when it fhould be ac- 
cording to the Hypothefis fartheft South. But becaufe 
I can more certainly depend upon the greateft Alterati- 
on of Declination of thofe Stars, which I have frequent- 
ly obferved about the Times when they become ftatio- 
a nary, 
