The Motion and Distribution of tlie Sun-spots 



31 



area A (or better, according to log A), the positive excess nevertheless remains un- 

 diminished. This may, to some extent, be owing to the fact of the class-interval 

 in oi being too broad. But if this should be the explanation of the remaining great 

 positive excess, this excess should have somewhat smaller vakies within tliese 

 different groups than when all the spots are combined. 



In examining the latitude motions of the spots, we shall be in a position to 

 discuss the problem of the positive excess, by a comparison with the observations 

 used by Dyson and Madnder in their paper on the position of the sun's axis. 



TABLE XII. 



Correlation between AX cos ß(= x) and log A(= m). 



1898-1909. — lOM ^ ß ^ — 12°.b . 



















Pr 





ory 



Mean i 



n oj 



= 1.900. 





Class-in 



terval in 



(0=0 



















Pro vis 





Mean i 



n X 



= - 



-0'.5. 



CI a 



5S-inter\ 



al in 



x = l' 





-Î) 



-8 





-6 



-> 



4 



-3 





-1 



0 



+ 1 



+ 2 



+ 3 



+ J 



+ 5 



+ 6 



+ 7 



+ 8 





+ 10 





+ 8 























2 























+ 7 

 +6 















1 





1 



1 





3 

 4 



1 

 1 

















11 



+ 5 





















6 



12 



9 





1 















31 



+ 4 











1 







4 



1 



lU 



20 



11 



6 



3 



1 













63 



+ 3 











J 



2 







4 



14 



27 



14 



10 





2 













78 



+ 2 















1 



.'i 





18 



14 



10 



8 



4 



1 



2 













+ 1 















2 







11 



18 



14 



8 



4 



3 





1 









74 



0 















2 



2 



8 



12 



16 



13 



9 



4 





1 











70 













1 







6 



11 



17 



9 



8 



3 





5 



1 



1 









62 













1 





1 



] 



C 



8 





8 



6 



3 





4 





2 







53 



-3 







1 



1 







1 



4 





5 



6 



7 



8 



3 



4 





1 





1 





.51 



-4 











1 



1 





8 



2 



4 



5 



6 



8 





4 



1 





1 







39 





1 







1 





1 





1 



2 





2 



5 





1 





1 











21 



-6 

 -7 

 -8 













1 





2 



1 

 1 



1 



1 





2 

 1 



1 









1 







11 

 1 



Totals 



1 





1 



2 



5 







38 



64 



117 



144 



112 



68 



29 



28 



12 



3 



4 







646 



In order to get a more accurate idea of the distribution of the longitude 

 motions of the sun-spots, 1 have given in fig. 2 a graphical representation of tliis 

 distribution in the zones and , compared with the normal distribution. The 

 observations of both periods are taken together. The distribution is in the figure 

 indicated with small circles. To be able to compare the distribution of the motions 

 with a normal distribution, I have used the normal co-ordinates introduced by 

 Charlier, 



