384 Mr. Herschei/s and Mr. South's observations of the apparent 
£ Aquarii continued. 
The various measures of this star are, 
1 779 * 9 ° 5 Position 7 1° 5' nf ; ^ 
1781.73 ; 7 1 39 nf; (.Distance 4".j6 ; H. Cat. of 1782 and “ Account of 
178247; 72 7 nf; J Changes,” &c. 
1802.01; 78 3 nf; (air too tremulous for measures); H. Account, &c, 
1819.64; 88 o np ; Struve, Additamenta. p. 198. 
1820.92; 88 18 np; 1 
„ . >Dist. = 4 400; Struve, vide Zach viii, 524, &c. 
1821.76; 88 12 np; ) 
1822.27 > 89 2 9 sp or nf; Distance 4" .989 ; H. and S. ut supra. 
The motion first noticed by Sir W. Herschel in his paper 
of 1804 is therefore clearly confirmed. It is remarkable 
that M. Struve uniformly places the smaller star in the 72-pre- 
ceding quadrant, while our observations as regularly make 
it sp or nf, but the position is so nearly in the meridian that 
it is scarcely possible to perceive a bias one way or the other ; 
and perhaps qo° n or s may be taken as the present situation 
without sensible error. In 42.37 years therefore the angle 
described is 19 0 , giving an average annual motion of o°-4484 
in the direction npsf or retrograde. 
As the proper motion of £ Aquarii (according to Piazzi) 
amounts to o". 1 73 or 7". 2 66 in 42 years, and yet the stars of 
which it consists still retain the same distance and nearly the 
same relative situation with respect to each other ; this cir- 
cumstance alone amounts to a proof of their mutual connec- 
tion, which their equal size corroborates, and renders it ex- 
ceedingly probable that they form a binary system. 
