24 Walter Gyllenberg 



Fig. 8. 

 Stars of magn. 4.9. 



Assuming however the stars of types BO to B2 to have their constant K larger 

 than the other class B stars, the variation of K in galactic longitude might be 

 caused by a clustering of these stars about the vertices. 



The stars used were however distributed in the following way: 





BO— Bl 



B2 



B3 



Bb 



B8—BQ 



No. of stars in the M. W. 



37 



24 



72 



42 



41 



No. of stars surrounding 















12 



6 



12 



to 



11 



The values of K for the subdivisions of the class B stars were obtained from 

 the numerical mean value of the peculiar velocities, the relative velocity of the sun 

 being taken from table IV a. The computation led to the following values of K: 



Bo—Bl 



m 



Bi 



B5 

 B8—Bd 

 all stars 



K (magn. ^ 4.9) 



K (all magn.) 



+ 1.22 + 0.14 

 + 0.84 + 0.13 

 + 1.10 + 0.15 

 + 1.18 + 0.14 

 + 0.10 + 0.18 

 + 0.92 + 0.07 



H 

 - 



-l.oo 4- 0.15 



- 0.77 + 0.12 



- 0.89 + 0.12 



- 1.29 + 0.12 



- 0.26 + 0.14 



- 0.87 + 0.06 



There is a remarkable difference in the value of K for stars of type BS — 59 

 and for the other class B stars. However this circumstance and the relative distri- 

 bution of the class B stars seem insufficient to explain the variation of K in terms 

 of galactic longitudes. 



19. Concerning the origin of this remarkable constant, Campbell says that a 

 personal equation in the measurement of the spectrogram, systematically positive 

 amounting to 5 km per second cannot be regarded as possible, while observations 



