( B68 ) 



Sol nl ion IX. 



6^^ 60!2 ± t'Io — |o!i3614 ±!o0100|^ 

 ^, = 293.18 ± 0.19 — |0. 032335 ± .000240| < 

 6, — 319.73 ± 0.52 — (0.006854 ± .000180| t 

 6, — 11.98 =h 0.67 - {0.001772 ± .000030| < 



The time t is counted in days from 1900 Jan. O, mean Greenwich 

 noon. The nodes are reckoned from the first point of Aries. Tlie motions 

 contain the precession, for wiiich Nkwcomb's value was adopted. 

 The probable errors of the motions of the nodes were computed 

 from those of the masses (C). For tlie position of the mean equator 

 referred to Lfaekkier's plane of Ju])iter's orbit for J 900.0 I find 



(o= 3?1153 ± 0°00I4 



^ = 315.800 ±0.025 (1900 Jan. 0.0) 



Table I contains the observed corrections to Souillart's theory, 

 their probable errors derived from the discussion of each series 

 separately, and the residuals which remain after the subtitulion of 

 the final values of yi. Si, to and 8. 



The probable error of ^veig•ht unity, determined from these resi- 

 duals is 



± 0°,0097. 



Weights had oi-iginally been assigned, corresponding to a probable 

 error of weight unity of 



± 0°.0100. 



Comparing each residual with its probable error, we find the 

 following distribution 



Remembering that the corrections ^pi and Lqi are for each epoch 

 the results of a series of observations, made for the different epochs 

 by different obser\ ers and different instruments, and reduced absolutely 

 independently of each other, we must consider this excellent agree- 

 ment of the actual distribution with the ideal one according to the 

 law of errors as a strong proof of the freedom of the observations 

 from systematic errors. Accordingly the probable errors of the resul- 



