north polar distances of the principal fixed stars. 69 
ern motion relatively to v\ Ursas Majoris, viz. at the rate of 
i",9 in ten years, at 1818 greater than at 1784. 
(I. ) Capella and v\ Ursas Majoris observed at Paris. 
Z. D. Jan. 1, 1740. 
Capella .... 3 0 8' 2 .%" ,6 S. » Ursae Maj. i°47' 7",7. N. 
Sol. and lunar nut. — 5 ,7 — 7 ,6 
3 8 22 ,9 1 47 o ,1 N. 
3 8 22 ,9 S. 
Diff. decl. 4 55 23 ,0* 
Greenwich, 
1755, decl. 
Palermo, 
3 800 decl. 
Dublin, 
1823, N.P.D. 
Capella . 
00 
0 
45° 46' 37">S 
44 0 11' 36",2 
yi Ursae Maj. 
50 32 39 ,0 
50 18 59 ,2 
39 47 59 >9 
Diff. 
4 49 34 ,2 
4 3 2 21 >7 
4 2 3 36 ,3 
Paris, 1740 
4 55 23 ,0 
4 49 34 > 2 
4 3 2 21 >7 
(15 years) 
5 48 ,8 
(45 y.) 17 12 ,5 
(23 y.) 8 45 ,4 
The secular variation of annual precession in diff. of decli- 
nation for these two stars is +, 622 + ,153 = -f- ,67 5. Vide 
Table III. 
Hence, 
Rate at 1747 1 f 3' 5 2", 5 ] f 3' 50", 3 
at 1777 >in ten years •< 3 49 ,4 > reduced to I78 o< 3 49 ,2 
at 1812 J 1 3 4 8 >4J l 3 5° >5 
* The result from the observations at Bourges is 4 0 55' 22",8. This close agree- 
ment must be accidental. But the observations in general may be considered as 
exact. It is worth while mentioning here the latitude of the Royal Observatory, 
at Paris, as deduced by comparing the Dublin north polar distances 1823, with 
the zenith distances of three stars observed at Paris, 1739 and 1740, 
Capella gives lat. = 48° 50' i4",o 
n Ursae Maj. - - --13,1 
7 Draconis - - - - - 17, 4 
Mean 48 50 14 ,8 
This differs so little from 48° 50' 14", the lat. according to the latest determina- 
tion, that it shows also we can calculate the motions of these stars pretty exactly 
for eighty years. 
