SECT. 1.] 



THREE COMPLETE OBSERVATIONS. 



225 



Accordingly, the data of the problem, after heing freed from parallax and 

 aberration, and after the times have been reduced to the meridian of Paris, are as 

 follows : 



From these right ascensions and declinations have been deduced the longi 

 tudes and latitudes, using for the obliquity of the ecliptic 23 27 55&quot;.90, 23 27 

 54&quot;.59, 23 27 53&quot;.27 ; the longitudes have been afterwards freed from nutation, 

 which was for the respective times -j- 17&quot;.31, -f- 17&quot;.88, -|- 18&quot;.00, and next re 

 duced to the beginning of the year 1806, by applying the precession -\- 15&quot;.98, 

 2&quot;.39, 19&quot;.6S. Lastly, the places of the sun for the reduced times have 

 been taken from the tables, in which the nutation has been omitted in the longi 

 tudes, but the precession has been added in the same way as to the longitudes of 

 Ceres. The latitude of the sun has been wholly neglected. In this manner have 

 resulted the following numbers to be used in the calculation: 



Times, 1805, September 



a, a, a 



5.51336 



95 32 18&quot;.56 



59 34 .06 



342 54 56 .00 



0.0031514 



i, i , i&quot; ...... 



log R, log K, log R . 



The preliminary computations explained in articles 136-140 furnish the fol- 



139.42711 



99 49 5&quot;.87 

 + 7 16 36 .80 

 117 12 43 .25 

 9.9929861 



265.39813 

 118 5 2S&quot;.85 

 7 38 49 .39 

 241 58 50 .71 



0.0056974 



lowing : 



AD, AD , AD&quot; . 

 A D, A&quot;D , A D&quot;. 



35855 28&quot;.09 

 112 37 9 .66 



15 32 41 .40 

 138 45 4 .60 



29 18 8 .21 



29 



156 52 11&quot;.49 



18 48 39 .81 



252 42 19 .14 



6 26 41 .10 



170 32 59 .08 



17048 44&quot;.79 

 123 32 52 .13 

 136 2 22 .38 

 358 5 57 .00 

 156 6 25 .25 



