216 



DETERMINATION OF AN ORBIT FROM 



[BOOK II. 



156. 



We shall take the second example from Pallas, the following observations of 

 which, made at Milan, we take from VON ZACH S Monatliche Corrcsporidmz, Vol. 

 XIV., p. 90. 



We Avill here take the equator as the fundamental plane instead of the 

 ecliptic, and we will make the computation as if the orbit were still wholly un 

 known. In the first place we take from the tables of the sun the following data 

 for the given dates : 



We reduce the longitudes of the sun, the precessions -j-7&quot;.59, -|-3&quot;.36, 2&quot;.ll, 

 being added, to the beginning of the year 1806, and thence we afterwards derive 

 the right ascensions and declinations, using the mean obliquity 23 27 53&quot;.53 and 

 taking account of the latitudes. In this way we find 



