94 
from various researches for stars 8™.5 with small P.M.: 279° 
and + 45°. 
My results, which apply to méan magnitudes (photom. magnitudes 
of Kiisrner), of 77.25 for the bright group and of 9".19,for the fainter 
group, remain almost the same, whether we take Auwers’s system 
or Nrwcoms’s as. basis. Comparing them with the above, it is seen 
that my values for A belong to the greatest so far obtained, while 
those for D for my bright group agree very well with those from 
the Brap.ey stars and the results for my faint group do not differ 
much from the corresponding ones of Boss. The large difference 
between the value for D in my two groups, which is the result of 
the abnormal relation of the two values found for the Zcomponent, 
is a striking result, to which I shall return further on. 
In the second place, my results for the amount of the paral- 
lactic motion must be further considered, both those for the projec- 
tion of this motion upon the plane of the equator and those for the 
total motion. We observe first that, for both motions, the reduction 
to Newcome’s system gives somewhat larger values than that to 
Auwers’s system. Naturally both for the bright and for the faint 
group. 
For the equatorial motion the ratio of group B to group F is 
according to the two systems 1:0.71 and 1: 0.73, while the ratio 
between the mean distances of the groups, according to the later 
researches (Comp. Kapreyn and Weersma Publ. Gron. 24, 15), should 
be 1 :0.63. Here the agreement is, therefore, fairly good, but the 
result is totally different, if we consider the total motion. For this 
we find for the faint group results which are only 3° , smaller than 
those for the bright group. 
However, before endeavouring to draw any conclusion from this, 
we must consider the significance of my results, in connection with 
the methods used concerning the exclusion of stars of large proper 
motion. As mentioned above I made one set of solutions (method A) 
in which practically only the double stars were excluded (besides 
the double stars for the four catalogues together only 21 stars) and 
another set (method E) in which a considerable number of stars 
with a somewhat large P.M. were excluded. Finally the mean results 
from these methods were accepted as the final result. 
This method was certainly justifiable, where a determination of 
the precessional motion was aimed at, and perhaps is so still, when 
we only desire to derive the coordinates of the apex of the paral- 
lactic motion. If we wish, however, to determine the amount of 
this motion, it will be seen that the significance of the results beco- 
