Summary. 



1. The magnitude of the sun's relative velocity seems to he highly dependent 

 on the spectral class, and shows very high values for the spectral classes B and M. 

 In the same manner the constant K is a function of spectral class, and the numeri- 

 cal value of this constant seems to be closely correlated with the solar velocity. 



As for the radial velocity observations used here, the value of K seems, espe- 

 cially for stars of types B and M, in some way to be dependent on the angular 

 distances of the stars from the principal vertex a = 274°,6, 3 = — 12°,o and the anti- 

 vertex. In these regions the value of K is larger than for other parts of the sky. 



2. As for the velocity distribution, the generalized ellipsoidal hypothesis was 

 applied. It was then found that, when the stars were divided into three groups 

 according to their spectral classes, as well as when all stars were treated together, 

 the velocity surfaces were represented by three axial ellipsoids with distinct exten- 

 sion in the direction of the principal vertex, but flattened perpendicular to the plane 

 of the Milky Way. The excentricity of the ellipsoid was found to he largest for 

 stars of the so called earlier types and smallest for stars of the so called later types. 

 For the group containing stars of magn < 4,9, the position of the ellipsoid was 

 closely correlated with the galactic system. 



A second solution, where the spectral classes B, A, F, G, K, M were treated 

 separately, led to the following results: 



In contradistinction to the other stars, the class B stars have their velocity 

 distribution represented by an ellipsoid of revolution flattened in the plane of the 

 Milky Way. No principal vertex direction seems to exist for these stars. 



For the stars of class A the principal vertex direction is very distinct ; further 

 the velocity ellipsoid is flattened perpendicular to the plane of the Milky Way. 

 Indeed the class A stars show, compared with the other spectral classes, the most 

 excentric velocity surface. 



The other spectral class stars have their velocity distribution represented by 

 three axial ellipsoids with the same position as for the class A stars. Excepting 

 the class B stars, the mean velocity of the stars in the direction of the principal 

 vertex seems to be almost constant, while the mean velocities in the other direc- 

 tions are slowly increasing when passing from the class A to the class M. For stars 

 of this latter class the velocity distribution seems to be quite spherical. 



