338 Mr. South’s re-examination of the apparent distances 
No. XVI. R. A. i4 h 43™ ; Decl. 19 0 51' N. 
| Bootis ; II. 18 ; H. and S. 187. 
Double ; 6th and 8th magnitudes. 
Passy ; April 3 , 1825 ; Seven-feet Equatorial. 
Position zz 66° 22' np I 7 Obs. 
Distance zz 7". 668 | 6 Obs. 
Diff. zz i° 56' } ,, 
Diff. — o".jzi | Very unsteady. 
Observed when 40 minutes east of the meridian. 
Passy ; May 27 , 1825 ; Seven-feet Equatorial. 
7 th and 10th magnitudes. 
Position z: 68° 16' np I 7 Obs. Diff. — i° 54' ? TT . . 
Distance = 7 ".8 i 4 | 5 Obs. Diff. zz o".6 7S 5 Unstead 7 - 
Observed on the meridian ; but the night is unfavourable. 
Passy ; May 31 , 1825 ; Seven-feet Equatorial. 
6 th and 8th magnitudes. 
Position zz 67° 3 ' np 
Distance zz 7". 9 49 
Observed on the meridian. 
5 Obs! | Difflrz: o". 4 8i } Ver X unstead 7 - 
Passy ; June 1 , 1825 ; Seven-feet Equatorial. 
6 | and Qth magnitudes. 
Position zz 66° i6' np 
Distance zz 7" .672 
7 Obs. 1 
5 Obs. I 
Diff. zz 2 0 3' 
Diff. zz o".889 
| Unsteady. 
Observed with 181 ; stars on the meridian, and at times well defined; a power of 
413 showed the larger of the two stars as round as possible. 
Mean Result. 
Position 67 0 o' np ; Distance 7". 7 76 ; Epoch 1825.37. 
In the former communication (Phil. Tran. 1824. III.) it 
is remarked that the continuance or decrease of the then 
angular velocity of about i° per annum for a few years, 
would decide the question of rectilinear or orbitual motion. 
The present observations, then, go a great way towards de- 
ciding this interesting question, as, so far from indicating 
any retardation, their tendency lies the other way. In fact, 
(supposing them free from error), no less than — 3 0 54' have 
been described in 2.74 years, being at the rate of — i°.42o 
per annum. This star therefore merits peculiar attention, as 
the great variation of its distance gives reason to suppose a 
great ellipticity, or considerable inclination of its orbit. (H.) 
