334 Mr. South's re-examination of the apparent distances 
No. XIII. R. A. I2 h 32 m ; Decl. o° 27' S. 
7 Virginis ; III. 18 ; H. and S. 150. 
Double ; 8th and 8 \ magnitudes. 
Passy ; April 3 , 1825 ; Seven-feet Equatorial. 
Position = 7 0 22 ' sf 7 Obs. I Diff. 
Distance = 3".287 5 Obs. | Diff. 
o°.3i 2 } Unstead y- 
The angles were observed with 413 ; but the distances with 181 only, in conse- 
quence of the unsteadiness of the stars, which were at the time of observation a few 
minutes west of the meridian. 
Passy ; April 4 , 1825 ; Seven-feet Equatorial. 
Position = 6° 42' np 5 Obs. 
Distance = 3". 152 5 Obs. 
Diff. = 2 0 20' ) -* T , 
Diff. = o".6oi ) Ver y unsteady. 
The stars are of the 8th and 8j magnitudes. I tried to use a higher power than 
1 8 1, but could not do it advantageously. 
Passy ; May 14 , 1825 ; Seven-feet Equatorial, 
8th and 8g magnitudes. 
Position r= 6° 55' np I 7 Obs. 1 Diff. = i° 9' ) 
Distances: 3"»325 J 5 Obs. j Diff. ~ ’ 
Observed when on the meridian ; stars tolerably well defined, but unsteady. 
Passy; May 31 , 1825 ; Seven-feet Equatorial. 
8 1 and 9th magnitudes. 
Diff. =o° ci' ) ,, . , 
Diff. zz o".4.8 i j ^ er y unsteady. 
Stars one hour west of the meridian ; at times tolerably well defined. 
Mean Result. 
Position 6° 53' np (28 Obs.) ; Distance 3". 2 63 (20 Obs.); 
Epoch 1825.32. 
These observations confirm the motion attributed to the 
stars of y Virginis, and point out an acceleration in it, even 
more strongly than has been insisted upon in a former paper. 
This will appear by assembling all the observations with 
their epochs, as follows : 
Position “ 6° 34' np 7 Obs. 
Distance = 3".28o 5 Obs. 
