SECT. 1.] 



THREE COMPLETE OBSERVATIONS. 



205 



150. 



We proceed now to the illustration of this method by some examples fully 

 explained, which will show, in the plainest manner, how generally it applies, and 

 how conveniently and expeditiously it leads to the desired result* 



The new planet Juno will furnish us the first example, for which purpose we 

 select the following observations made at Greenwich and communicated to us by 

 the distinguished MASKELYNE. 



From the solar tables for the same times is found 



We will conduct the calculation as if the orbit were wholly unknown : for 

 which reason, it will not be permitted to free the places of Juno from parallax, 

 but it will be necessary to transfer the latter to the places of the earth. Accord 

 ingly we first reduce the observed places from the equatoi to the ecliptic, the 

 apparent obliquity being employed, whence results, 



* It is incorrect to call one method more or less exact than another. That method alone can be con 

 sidered to have solved the problem, by which any degree of precision whatever is, at least, attainable. 

 Wherefore, one method excels another in this respect only, that the same degree of precision may be 

 reached by one more quickly, and with less labor, than by the other. 



