Stellar velocity distribution 



111 



TABLE XX. 



The moments of the second order of the observed proper motions and radial velocities. 



Square 



V 200 



V 020 



V 002 



v nn 



Aj 



-f- 0.00609 



-j- 0.01391 



-f- 11 .07 



+ 0.00701 



A 



-j- 0.00305 



-j- 0.0051'. 1 



-j- 13.59 



— 0. 00006 



Bi 



+ 0.01164 



-j- 0.00449 



1 



-f- t .98 



-\- O.00377 



B. 2 



-\- 0.00543 



4" 0.00437 



-j- 6.86 



4" 0.00338 



B a 



4- 0.001! 10 



4- 0.00827 



-|- 12.49 



— 0.00130 





-j- 0.01484 



4- 0.00723 



-j- 12.97 



-4- 0.00574 



B s 



4" O.O0915 



4- 0.00401 



-f- 11.64 



— 0.00163 



B a 



4" 0.01187 



4- 0.00957 



-j- 5.08 



-j- 0.00152 



B, 



4" 0.01450 



4- 0.01809 



-j- 10.12 



-j- 0.00215 



B s 



4- 0.00427 



4- 0.00585 



+ 14.65 



+ 0.00038 



A, 



4" 0.00277 



4" 0.00563 



+ 7.47 



+ 0.00271 



B l0 



4" 0.00652 



4" 0.00513 



+ (5.48 



+ 0.00089 



c l 



+ 0. 00920 



+ 0.002!>8 



+ 9.53 



+ 0.00130 





4- 0.01157 



4" 0.01378 



+ 15.85 



+ 0.00295 



c\ 



4- 0.00734 



4- 0.00265 



+ 13.38 



+ 0.00017 





4- 0.00180 



-j- 0.00727 



+ 20.15 



-j- 0 00059 



a 



4-0 00451; 



+ 0.00208 



+ 13.27 



— O.O0O57 





-j- 0.02937 



4- 0.00380 



+ 15.48 



— 0.0020O 



% 



4- 0.02384 



4- 0.00877 



4- 9.1c, 



— 0.00240 





4- 0.01013 



4- 0.00405 



-f- 21-.49 



— 0.00039 





-j- 0.00649 



4- 0.00767 



4- 14.22 



+ 0.00320 





-j- 0.00318 



-j- 0.00811 



4- 12.76 



— 0.00115 



k 



4- 0.00596 



+ 0.00605 



4- 10 31 



— 0.00315 



c„ 



-1- 0 01703 



4- 0.020C4 



+ 11.51 



— 0.00555 



57. If we use the form (51) for the linear moments in a certain square, it is 

 easily found from the usual transformation of coordinates that the expression for 

 the linear moments in another system, say the galactic system — G — , will have 

 the same form as (51) so that in this system 



(52) 



00 a' — 0 — 2') £i> 2 

 W-0 -<z')V 

 ; o2 2' — i ] — q) c,. s 



.-lo 



and L denote the 



and similar equations for the correlation moments. Here £„ 

 components of the sun's relative velocity in the system G. 



The moments v,^ are the » apparent moments» in relation to the same system 

 and may be computed from the apparent moments in the squares. 



From the solution of the velocity ellipsoid of the apparent proper motions, 

 the following three axes and directions were found : 



