The general Characteristics of the frequencyfunction of stellar movements 45 



The Apex of the solar motion referred to the stars here used has been com- 

 puted by Charlier. A recompilation performed by me of course gave the same 

 result. It is : 



Solar motion and Apex. 9^ S= 1.0275 = 0."05138 

 A = 272.°? 

 D = 31.°6. 



Taking for the value of S the solar velocity found by Gyllenberg from 1114 

 radial velocities, or 



S = 19.4 km. per sec. 



we obtain 



(1) \ = 0.0529, 



which value is to be used to get our attributes of motion expressed in the km. per 

 sec. as unity. 



Generally it will be more adequate in discussing stellar movements, to use 

 as unity of length and time the Siriometer = 10 6 times the mean distance of the 

 Sun and the SteUttr year = 10 6 years*. Thus the velocity one Siriometer per stellar 

 year is the same as one mean distance of the Sun per year. 



In those units we have 



S = 4.103, 



and obtain 



(2) & t = 0.2504. 



Multiplying with the classbreadth we find the mean parallax of the stars 

 brighter than (ï.o 



rt 1 = 0."01252. 



Using the value (1) of we get the table VIII for the axes. In this table 

 also the excentricities are contained. Thus e 12 is the excentricity in the plane 



VJII. 



i' 



o, km 



o 2 km 



a, km 



e 12 



e,3 



1.0000 



34.88 



23.93 



19.29 



0.73 



0.83 



0.8422 



31.57 



21.36 



17.44 



0.74 



0.83 



0.6205 



26.36 



17.15 



14.18 



0.75 



0.83 



0.4500 



21.77 



13.60 



9.75 



0.78 



0.89 



of o 1 and a 2 , a. s. f. Of course the excentricities are independent of d- v but we 

 here see also, that they are practically independent of q' . Thus we may state 

 that the form of tJie ellipsoid is the same whatever (in any way plausible) values 



* Those units have been adopted by Charlier in bis lectures on stellar statistics. 



