18 
a second from the truth; and therefore it may fairly be concluded, 
that the errors of p and z are not much greater. 
The values obtained from the three equations deduced by sup- 
posing the solar nutation known are probably more exact. These 
equations are 
1. 199¢e+48,762—28,90p—5,77=0 
2. 48,76e+82,58022 + 35,8977p + 23,9894—0 
3. -28,90e + 35,89772 + 101,6388p + 18,6693—0 
The solution gives 
p= —0",0332 
x= —0,3395 or const. of aberration=19”",91 
e= +0,1074 or mean N. P. D. Jan. 1, 1819=38° 29’ 7”,52. 
The small negative value of p, arising from the unavoidable 
effect of the errors of observation, seems to shew, that the value of p 
does not amount to a of a second; and therefore, that this star is ten 
times more remote than a Lyre. 
Iam aware, that to many it will appear almost absurd to rely 
on these small fractions of a second—I hope they will not adhere to 
this opinion without carefully examining the steps, by which these 
conclusions have been obtained. 
Observations of 1» Urse Majoris. 
For this star the mean zenith distance Jan. 1, 1819, has been sup- 
posed = 3°. 10’. 0”, 60—e 
The four resulting equations that have been deduced as before, 
from 144 observations, are 
1. 144e+15,632—6,99p+64,56:—1 9,07 =0 
2. 15,63¢+-42,21152+25,5393p—8,2082z—13,1740—0 
3. -6,99e+25,53932+71,0775p—9,4177z—13,4576=0 
4.  64,56e—8,208272—9,4177p+60,8238z:—19,8381=0 
