( 666 ) 



ill (li'ttiil in these Proceedings (March J 906). The values found for 

 V; and Fio were very nearly equal to those found previously. The 

 correction to x' was very small, viz. -. 



ox' = -t- 0.0026 ± .0058. 

 The masses now become 



y.' = 4- 0.0276 i\ = + 0.050 j 



.... (5) 

 ri = — 0.360 r, = +0.01-5) 



The motions of the nodes were no^v made to correspond with 

 these masses, the values found for 7/ , Ho , .r„ and y„ were introduced 

 into the equations of condition, and residuals Ay/ and .sm y, A T/ were 

 formed. From these latter I then derived for each satellite separately 

 a correction to the motion of the node. These corrections are gixen 

 below sub I. The values of the nodes in 1750.0 were next computed 

 and compared with those determined by Dklambre. This comparison 

 o-ave the corrections II to the motions of the nodes. 



('orieciion 



to the 

 motion of 



I 



{modern) 



II 



f DK.I.AMIUtK.) 



Ado/iteo 



e^ 4- 0°.0094 ±.0029 



S^ —0 .00001 ± 00009 — 0°.00042±°.00020 — 0°.00010±. 00008 



0^ _0 .00048± 23 - .00034± 20 -0.00041± 15 



0^ _0.00013± 11 -f0,00008± 50 — O.OOOlOi 10 



These corrections have been used as the right-hand members of 

 equations of condition, from which, together with those derived from 

 the other subordinate investigations, corrections to the values {B) of 

 the masses have been determined. These eqnations will be given further 

 on. It will be seen that the adopted values agree within the probable 

 errors with those derived from the modern observations alone. If 

 thus these latter were adopted, the luial results could only be 

 altered within their probable errors. The tinally adopted masses are: 



(O 



These were now introduced into tiie quantities (jy and ;// and a 

 new solution was made (Sol. IXj, in which the motions of the nodes 

 corresponding to the masses (C) were adopted, and accordingly tfx' 

 was not introduced as unknown. The result is : 



