1838.] Motion of the Solar System in Space, 



397 



General P. M, 

 A. R. in Declination. 



Cord. Gen. P. M. 

 in Declination. 



h. m. 



No. 1. 



No. 2. 



0 



30 s 



+ 



,0079 X 



,891 X 



I. 



30 



+ 



,0172 X 



,923 

 ,793 



11. 



30 



+ 



,0032 + 



III. 



30 



+ 



,0099 X 



,608 



IV. 



30 



+ 



,0072 X 



,382 



V. 



30 



+ 



,0146 X 



,130 



VI. 



30 



+ 



,0216 - 



,130 



VII. 



30 



+ 



,0139 ~ 



,382 



VIII. 



30 



+ ,0037 - 



,608 



IX. 



30 



+ 



,0073 - 



,793 



X. 



30 





,0121 - 



,923 





^rt 

 ou 





,0171 - 



,JO 1 



XII. 



30 





,0037 - 



,991 



XIII. 



30 





,0009 _ 



,923 



XIV. 



30 





,0111 _ 



,793 



XV. 



30 





,0043 _ 



,608 



XVI. 



30 





,0142 _ 



,382 



XVII. 



30 





,0134 - 



,130 



XVIIl. 



30 





,0190 + 



,130 

 ,382 



XIX. 



30 





,0160 + 



XX. 



30 





,0090 + 



,608 



XXI. 



30 





,0094 + 



,793 



XXII. 



30 



+ 



,0019 + 



,923 



XXIII. 



30 



+ 



,0108 + 



,991 



O;^ a 

 3 o 



s - ,0071 

 + ,0038 



- ,0083 

 + ,0009 

 + ,0015 

 +.,0127 

 + ,0235 

 + ,0196 

 + ,0127 

 -f ,0188 

 + ,0013 



- ,0023 

 + ,0111 

 + ,0126 

 + ,0004 

 + ,0047 



- ,0085 

 ,0115 



- ,0211 



- ,0217 



- ,0180 

 ~ ,0209 



,0115 

 ,0041 



Inspecting No. 1, we find a pretty regular determination to + and 

 — , which cannot possibly arise from accident ; we notice, that any 

 small correction for error of precession, such as found at page 312, 

 since it interferes in no respect with the general tendency of the num- 

 bers in the table No. 1, may be applied, or not, at pleasure ; to be con- 

 sistent, however, it will be proper to apply this correction, and adopt 

 the results contained in No. 2. 



If we now divide the line A B fig. 2 into 24 equal parts, 

 to represent hours of A. R. and making use of any convenient scale, 

 set off opposite to OA. 30m. \h. 30m. and the perpendiculars a \, a 2 

 &c. corresponding to the values given in the table at page 312, and 

 perform the same fig. 3, for the above table; we get two series of 

 lines 1,2, 3, and 1, 2, 3, exhibiting, in the first instance, the observed 

 variation of the A. R, of a star supposed to be situated at Ok. 30m. 



