326 Mr. South's re'examination of the apparent distances 



No. VIII. R. A. 8^^ 2"» ; Dec!. 18** ii' N. 



f Cancri ; I. 24 and III. 19 ; H. and S. 90. 



continued. 



Eassyi Agril 4, 1825 ; Seven-feet Equatorial. 



■7th and 8th magnitudes. 

 Position = 6j° 14' sf \ 7 Obs. | Diff. = 1® 30'. Very difficult. 

 Observed with 413, when a few minutes west of the meridian; but the unstea- 

 diness of the stars renders it impossible to procure any observations of distance. 



Passy ; April 5, 1825 ; Seven-feet Equatorial. 



7th and 8th magnitudes. 



Position = 68° 49' sf 7 Obs. DifF. = 1° 27' 7 ^ . ,. 

 Distance = s".6i6 5 Obs. DifF. = o".673 j ^^^^ ^^ 



Observed a few minutes west of the meridian with 41 3 ; stars well defined, but very 



unsteady, 



• ' ■ Mean Result. 



bf A^B.^1*o'sM6nS'^*io'w/(430bs.); Distance i".o86(i50bs); 



of AC. — 67° 55' 5/ (2 7 Obs.); 5".436(iiObs.); 



Epoch 1825.27. 



Note. The observations of A C, when the star A was only 



seen as a single star, are rejected. 



This star presents the hitherto unique combination of three 

 individuals, forming, if not a system connected by the agency 

 of attractive forces, at least one in which all the parts are in 

 a state of relative motion. To begin with the two nearer 

 stars A and B. Sir W. Herschel's measure of their posi- 

 tion Nov. 28, 1781 (1781.90) was 86° 32'^/. and it will be 

 remarked, that a position so nearly perpendicular to the diur- 

 nal motion carries in some measure its own verification with 

 it, as not liable to gross error. This differs no less than 

 54° 22' from the present angle in the same quadrant, giving 

 a meaniannual motion of + 1^.254 or direct {nfsp). The 

 distance remains as it was, so close as to be barely separable. 

 In 1802 it was so also ; but at that time, though observed by 



