93 
In the second place we will discuss the results obtained for the 
parallactie motion, if -we successively adopt the two systems. 
For the components of the parallactic motion the following values 
are found : 
In AUWERS’s system: In NEwcomps’s system: 
_ Groups B Groups F_ | Groups B Groups F 
Sse. 1-050 0/52 0/55 +049 
Y —2.59 el 28719 = 2001 
Z BIg? ah. 2:50 SE U OE Er Py (1 
From the values in this table I deduce the following values for 
the coordinates of the apex, A and D, and for the total solar motion 
and its projection upon the plane of the equator. 
In AUWERS’S system: IS In NEWCOMB’S ne 
| Groups B ie Cone F | Wenne B Groups F A 
| 28205 =} 286% 28191 =| 28307 
6 {1h 50m 19h 4m | 18h 44m | 1h 55m 
XY? 2/65 ves | oe | 2°07 
D | 4.3509 45499 | 43595 | 4.5205 
VK NVZ? 3728 | 320 | 349 | 3/40 
Let us first consider the results obtained for the R.A. and Decl. 
of the apex. It is not possible here to institute a critical comparison 
of my results with those of others which would in itself form a 
research. For the sake of orientation in the problem I will merely 
quote some results obtained by previous investigators along the same 
lines. 
The results deduced for A and D from the Bradley stars by 
Newcoms and corrected for the systematic difference of distance, 
according to the research published in these Proceedings, by — 1° 
and + 2° respectively were 273° and + 33°; in the same way the 
results of L. Srruvr (corrected by Newcoms) become 272° and + 37°. 
From the comparison of the whole material of his Albany-zone with 
LALANDE and Bresser, Boss found for stars of a mean magnitude 
8™.7: 264° and + 54°'), while later on?) he accepted as final result 
A.J. 9, 28 
2) A. J. 31, 168. 
