95 
mes uncertain by the method used. It is necessary, therefore, to 
consider the results according to the methods A and E separately. 
For_this purpose I calculated, from the values of the 6 coefficients, 
after correction for the subsidiary terms, the components X, Y, Z 
of the solar motion for the A and E groups of each of the catalo- 
gues separately, and combined these results with the previously adopted 
weights. 
In this way | found adopting the system of Auwers’s N. F. K. 
Bec) BES. |e ER FE 
| | 
x +014 | +0742 | +062 | +0734 
Y (R. A) Sea? 7) 1746 e) A 0 
Y (Decl.) ASA (17 32) 6B 2 BB: | 2217 
Y (mean; weights 2and1) | —3.13 —2.05 —2.04 —1.58 
Z 42.13. | +1.70 | +2.89 | +42.29 
and for the further constants derived from these 
BA BEM’: PEA FE 
|| 28303 281°6 286°9 282°1 
(18h 53m 18h 46m 1gh 8m 18h 48m 
VX? | 3722 2”09 2/13 1/62 
D 4 3394 +3991- | _ +53°6 15497 
VX2+Y212Z2 | 3/86 2710 | 3/59 280 
It may be regarded as.a satisfactory result of the last calculation 
that the coordinates of the apex, gained by the A and / methods, 
do not differ greatly, and also differ only slightly from my previous 
results. On the other hand, the result that the Z-component is found 
larger for the faint than for the bright stars, becomes even more 
striking, now that it proves to hold good for the results deduced 
separately by the A and £ method. was to be 
expected from former results, the amount of the parall. motion 
gained by the two methods differs considerably, which again shows 
that the parall. motion increases greatly with the total P. M. The 
Further, as 
