in the relative Situation of double Stars. 375 
with great difficulty. The object is uncommonly beautiful ; but 
it requires a most ‘excellent telescope to see it well, and the 
focus ought to be adjusted upon e of the same constellation, so 
as to make that perfectly round. The appearance of the two stars 
is much like that of a planet with a large satellite or small com- 
panion, and strongly suggests the idea of a connection between 
the two bodies, especially as they are much insulated. The 
change of the angle of position, might be explained by a paral- 
lactic motion of. the large star; but the observations on the 
distance of the two stars, can hardly agree with an increase of 
it, which would have been the consequence of that motion. 
North-preceding FL 29 Capricorni. I, 47.' 
The position, July 23, 1783, was 84° 48' north -preceding. 
Sept. 1, 1802, it was 66° 50'. This gives a change of 17 0 58', in 
19 years and 40 days. The effect of a parallactic motion would 
fall chiefly on the distance ; it will, however, account for the 
change of the angle. 
Near FI. 3 Pegasi. II, 62. 
The position, May 3, 1783, was 88° 24' north-preceding. 
August 31, 1802, it was 7 g° 38' south-following. The change 
is 8° 46', in 19 years and 120 days. The stars are so nearly 
equal, that in 1783 I supposed the preceding one to be the 
smallest, and in 1802 the following one; which occasions the 
different denomination of the angles of position. If the distance 
of the preceding star should be much greater than that of the 
following one, a parallactic motion would explain the change of 
the angle, but not otherwise. 
3c 
MDCCCIV. 
