22 



Walter Gillenberg 



TABLE V. 



Comparison with the values of the constant K obtained 

 by Campbell (for each spectral class). 



Spectral class 



K (Gyllenberg) 



K (Campbell) 



B 



+ 0.91 + 0.11 



|+ 0.832 

 1 + 0.859 



A 



+ 0.03 + 0.18 



+ 0.201 



F 



+ 0.05 + 0.23 



+ 0.013 



G 



— 0.17 i 0.28 



j — 0.042 

 1+0.046 



K 



+ 0.75 + 0.19 



)+ 0.403 

 1+0.595 



M 



+ 1.11 ± 0.45 



)+ 0.830 

 1 + 0.969 



Campbell it seems probable that tbe stars of type B — Bö have a larger value of 

 K than stars of type BS— Bd. It would thus be possible from a smoothed curve 

 to interpolate the value of K for the subdivisions of the spectral classes. From a 

 preliminary computation of the constant K within class B stars (page 24) nothing 

 seems however to indicate a continuous variation when passing from class B0 to 

 class 59. 



18. In his paper »On the Motion of the brighter class B stars», Campbell 

 has tested the value of this constant in zones at different angular distances from 

 the apex. No variation was however observed. In order to test the value of K at 

 different distances from the vertex and furthermore in the plane of the Milky Way, 

 I have in the figures 2 — 8, representing the galactic plane, illustrated the value 

 of K. The numbers denote the galactic longitudes and are computed from the 

 vertex (closer defined in the following Chapter III) a = 274°.6 S = — 12°.o. From 

 the dotted line the values of K are marked out, positive values in the direction 

 from, and negative values in the direction of the centre. The values were com- 

 puted by subtracting the solar velocity components from the mean displacements 

 in the squares. 



The variation of K seems quite irregular with the exception of the types B 

 and M, where a distinct relation with angular distance from the vertices, situated 

 at 0° and 180° seems to exist. The mean velocity of the class B stars being small 

 and consequently also the mean error of K in the squares, the numerical value of 

 this constant seems to be in some way dependent on the position of the stars in 

 relation to the vertex. In the same manner the stars of type M show an identical 

 relation. It is true that the mean error here is large and the number of stars small, 

 but the difference in the means of K from stars in a zone surrounding tbe vertices 

 and in a zone at angular distance of 90° gives evidence of a large variation. 



