338 Mr. South's re-examination of the apparent distances 



No. XVI. R. A. 14^ 43™ ; Decl. 19° 51' N. 

 I Bootis ; II. 18 ; H. and S. 187. 

 Double ; 6th and 8th magnitudes. 



Passy ; April 3, 1825 ; Seven-feet Equatorial. 



Position = 66° 22' np 

 Distance = 7".668 



7 Obs. 

 6 0bs. 



'. — d'.jzi ] ^^^ unsteady. 



DifF. = I 

 DifF. 



Observed when 40 minutes east of the meridian. 



Passy ; May 27, 1825 ; Seven-feet Equatorial. 



7th and 10th magnitudes. 

 Position =: 68° i6' n/) I 7 Obs. 

 Distances 7*.8 1 4 | 5 Obs. 



Observed on the meridian ; but the night is unfavourable. 



DifF.= i°54' Kt ^ J 

 DifF. = o".673|U"^teady. 



Passy ; May 31, 1825 ; Seven-feet Equatorial. 



6th and 8th magnitudes. 



5 Obs! I Diff:= o''.48i } Very unsteady. 



Position = 67° z' np 

 Distance = 7"-949 



Observed on the meridian. 



Passy ; June 1, 1825 ; Seven-feet Equatorial. 



6\ and 9th magnitudes. 

 Position = 66° ib' np\j Obs. I Diff. = 2° 3' ) ^t <■ a 

 Distance = 7".672 | 5 Obs. | DifF. = o".889 ] "^nsteaay. 



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° o' np\ Distance 7^.776; 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 1° 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 hes the other way. In fact, 

 (supposing them free from error), no less than — 3° 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 eUipticity, or considerable inclination of its orbit. (H.) 



