212 Mr. Herschel’s and Mr. South’s observations of the apparent 
£ Bootis continued. 
if the stars form a binary system, the present angular velocity 
of about a degree per annum, will continue for some time 
nearly uniform, and in 15 or 20 years the limit of 50° np will 
be attained or passed. 
If we give up the observations of 1802, 1804, and suppose 
the position to have been exactly north at the epoch 1792.8, 
the observations, both of angle and distance, will be nearly 
represented by a circular orbit, described with a mean motion 
of i°.8 per annum, and inclined at an angle of 13 0 34,' to the 
visual ray, supposing the intersection with the plane of pro- 
jection to lie in the np and s/" quadrants, at an angle of 70° 
with the parallel ; but the data are too precarious to rely 
much on this conclusion. 
There is a small star at about if- or 2 minutes distance, 
and at about 82° np, which is not to be suspected with the 
seven -feet reflector (aperture 6 inches) and can barely be 
discerned by rare glimpses (knowing its place) in the ten 
(aperture 9 inches) but with the twenty-feet it is very con- 
spicuous. This was observed by Sir W. Herschel, in 1792, 
to be in the same line with the two stars of J, or rather, ac- 
cording to a diagram made at the time of observation, a little 
more ( 3 0 by measurement of the diagram) to the preceding 
side of that line. It became interesting to re-observe this 
star, as a verification of the motion of J. Accordingly, in 
the month of July last, the twenty-feet reflector (aperture 18 
inches) being directed on it, £ and the neighbouring small 
stars were seen as in fig. 2, Plate IV. The small star in 
question is 6, and is now decidedly on the following side of 
the line of junction of the two stars of £, and that by a 
