Walter Gyllenberg 



On the other hand the value of K seems to be strongly correlated with the 

 relative solar velocity. 



In fig. 9 I have made a graphical comparison between the relative velocity of 

 the sun and the value of K; the agreement is very striking. It is, besides, in- 

 teresting, that the values of the distances of the stars of different spectral classes 

 will, drawn as a curve, have the same form, when the parallaxes are computed 

 from a comparison between proper motion and radial velocity. The mean parallaxes 

 are indeed influenced by the assumed value of the solar velocity. This will however 

 not change the mutual relations. 



The mean errors in the solar velocity determinations. 



21. In the linear equations in U 0 ", V 0 ", W 0 " and K, the mean error in one 

 unknown quantity — R — is expressed through 



where p B denotes the weight of R obtained in the usual manner. Further s is the mean 

 error in one single observation and was put equal to a (see table X page 30). The 

 stars in the squares taken in groups, the mean error of a single observation is equal 

 to the mean error in the mean or 



s = 9 : V ni. 



The number n was put equal to the mean number of stars in the squares. 



The following table gives the mean errors computed in this way. In order 

 to determine the mean error in the apex direction it was assumed that 



<U 0 ") = b(V 0 ")^^W 0 ") = b(S). 



TABLE VI. 



The mean errors in the coordinates of the apex, the solar velocity and the constant K. 



Type 



<U 0 ") 



< v 0 ") 





<S) 



z{D) 



in degrees 



<A) 



<A) 

 in degrees 



B 



0.218 



0.170 



0.178 



0.190 



0.041 



2°.4 



0.052 



2°.9 



A 



0.301 



0.290 



0.321 



0.305 



0.060 



3°.4 



0.084 



4°.8 



F 



0.450 



0.401 



0412 



0.421 



0.100 



5°.7 



0.116 



6°.6 



G 



0.498 



0.455 



0.479 



0.474 



0.113 



6°.5 



0.130 



7°.4 



K 



0.346 



0 325 



0.313 



0.328 



0.078 



4°.5 



0.090 



5°.2 



M 



0.772 



0.831 



0.763 



0.789 



0.188 



10°.8 



0.216 



12°.4 



m <^ 4.9 









0.182 



0.043 



2°.5 



0.050 



2°.9 



m > 5.0 



0.348 



0.324 



0.294 



0.322 



0.077 



4°.4 



0.089 



5°.l 



ail stars 









O.160 



0.038 



2°. 2 



0.044 



2°.5 



