62 



O. A. Åkesson 



AAAAAA Î s 



AAAAAA i 3 



05 to ^3 .t5 "o 



■g "§ g 8 § g 



371 

 658 

 883 

 1108 

 819 

 190 





1 Northern Hemisphere 



First Period (1886—1897) 



2'.813 

 3.226 

 2.473 

 2.048 

 1.785 

 1.841 





l'.523 

 1.495 

 1.214 

 1.053 

 0.932 

 0.852 





to CO za CO n- 



g 00 to g o CÇ 





Southern Hemisphere 



2.926 



2.439 

 1.890 

 1.661 

 1.694 





l!426 

 1.403 

 1.204 

 0.959 

 0.894 

 0.948 









1 Northern Hemisphere 



Second Period (1898—1909) 



3^168 • 

 2.976 

 2.570 

 1 875 

 1.869 

 1.489 





1.626 

 1.604 

 1.318 

 1.090 

 1.063 

 1.130 





5 to S o œ *^ 

 ►t- ht- -a cr. o LO 





Southern Hemisphere 



3.123 

 2.838 

 2.609 

 1 887 

 1.632 

 1.738 





l!530 

 1.486 

 1.30G 

 1.058 

 1.011 

 0.892 



1554 

 2861 

 3550 

 4424 

 2899 

 865 





T 



2^999 

 2.997 

 2.519 

 1.927 

 1.727 

 1.696 





l'.518 

 1.490 

 1.259 

 1.036 

 0.967 

 0.958 





0.506 

 0 501 

 0.500 

 0.538 

 0.560 

 0.565 





columns. From these values the intimate 

 connection between the dispersion and spot- 

 area is still more obvious. 



Since Oj; is about double the size of a,, , 

 we see that tlie dispersions in longitude, 

 as well as in latitude, are approximately 

 the same function of the spot-area. In fig. 

 7 the values of the dispersions, computed 

 from the entire material of observation, are 

 graphically represented. 



Computing the quotient a,, : for the 

 different spot- sizes, we obtain the values given 

 in the last column of table XXIX. It seems as 

 jf this quotient for the larger spots should 

 have a greater value than for the smaller 

 ones. Since the dispersion for spots of a certain 

 size may be i-egarded as a measure of the 

 currents in the photosphere, one might 

 possibly infer that the quotient between the 

 sizes of the currents perpendicular and 

 parallel to the equator, is greater for the 

 larger than for the smaller spots. This 

 might be supposed to be due to 0^:0^-, as 

 well as the spot-area, varying with the lati- 

 tude, or one might also suppose that the 

 larger and smaller spots generally occur 

 at different depths of the photosphere. As 

 far as J can find, nothing seems to prevent 

 the state of the currents possibly being 

 different at different depths. We saw, how- 

 ever, page 49, that there did not exist any 

 marked connection between the quotient 

 cs,j : a,, and the latitude, wherefore the first 

 assumption does not seem very probable. 

 Should it, however, be the case that the 

 larger spots generally occur at higlier level 

 than the smaller, this might possibly explain 

 the fact, stated on page 43, that the larger 

 spots givie a shorter rotation period than 

 the smaller ones, which fact would thus indi- 

 cate a greater angular velocity of the outer 

 layers of the sun than that of the lower. 



