The Motion and Distribution of the Sun-spots 



a supposition. And I consider it the more essential that this supposition of 

 Carrington should not be adopted without further investigations, as it might 

 easily lead theoretical researches on the conditions of the solar atmosphere to 

 erroneous results. 



TABLE XXI. 

 Characteristics of the Motions in Latitude. 



Latitude- 







First Period (18 



6—1897) 







Second 



Pe 



riod (1898 — 1909) 





























N, 



20 





- 0.075 





h 1.426 







11 



+ 0.M5 





- 0.690 











176 





- 0.076 





- 1.236 



+ 0.124 



+ O.ICO 



48 



— 0.136 





- 1.047 









N. 



562 





- 0.012 





- 1.434 



+ 0.052 



+ 0.169 



373 



— 0.012 





- 1.358 



+ 0.230 



+ 0.213 



K 



1081 





- 0.036 





- 1.185 



— 0.100 



-j- 0.205 



644 



+ 0.106 





- 1.364 



— 0.092 



+ 0149 





1285 





- 0.062 





-1.118 



— 0.013 



+ 0.264 



1239 



+ 0.096 





- 1.306 



— 0.070 





- 0.180 



^2 



709 





- 0.039 





- 1 .194 



+ 0.106 



4- 0.136 



1139 



4- 0.050 





- 1.290 



+ 0.078 





- 0.219 





314 





L- 0.052 





- 1.212 



— 0.101 



+ 0.176 



267 



+ 0.218 





- 1.25? 



4- 0.012 



_ 



- 0.389 



^1 



391 



H 



- 0.004 





- 0.977 



+ 0.068 



+ 0.078 



264 



+ 0.097 





- 1.206 



+ 0.112 



- 



- 0.255 



Si 



1108 





- 0.011 





- 1.122 



-f 0.173 



4- 0.2;to 



888 



4- 0.108 





- 1.212 



— 0.029 





- 0.2 19 





1367 





- 0.008 





- 1 .176 



— 0.054 



+ 0.274 



1J81 



4- 0.052 





- 1.252 



+ 0.035 





- 0 .170 





1234 



+ 0.024 





- 1.150 



+ 0.069 



4- 0.231 



956 



4- 0.026 





- 1.298 



-|- 0 200 





- 0.186 



s. 



621 





- 0.018 





- 1.264 



4- 0.118 



-f 0.229 



445 



4- 0.030 





- 1.815 



— 0.025 





- 0.139 



s„ 



274 



+ 0.070 





- 1.827 



+ 0.074 



4- 0.062 



50 



-|- 0.320 





- 1.559 









s. 



77 



+ 0.114 





- 1.172 







15 



+ 0.616 





- 1.335 









The dispersions of the latitude 

 motions prove, on the whole, to be 

 about half the size of the dispersions 

 in longitude. This fact seeuis to in- 

 dicate that the currents in the solar 

 atmosphere parallel to the equator are 

 greater than those in a direction per- 

 pendicular to the equator. Table XXII 

 gives the quotient between o,, and a^. . 

 As is evident from the table this 

 quotient does not vary with the lati- 

 tude. Hence we may infer that the 

 relation between the sizes of the cur- 

 rents parallel and perpendicular to 

 the equator is the same at all lati- 

 tudes within the spot-zones. 



As regards the sTcewness, it proves 

 to be alternatively positive and nega- 

 tive. One might perhaps say that a positive skewness is predominant. If, however, 

 we take into consideration the mean error of the skewness, which is very great — 



Lunds Universitets Årsskrift. N. F. Afd. 2. Bd 10. 7 



TABLE XXir. 

 The Values of o,^ : at different Latitudes. 





First 



Period 



Seconc 



Period 



Latitnde- 



(1886 



-1897) 



(1808 



—1909) 















20 



0.475 



11 



0.255 





176 



0.474 



48 



0.440 



N. 



562 



0.587 



373 



0.552 



K 



1081 



0.485 



644 



0.518 





1285 



0.504 



1239 



0.534 





709 



0.448 



1139 



Ü.5C6 



^\ 



314 



0.496 



267 



0.560 



Sr 



391 





264 



0.577 





1108 



0.512 



888 



0.522 



Si 



1367 



0.497 



1181 



0.503 



S, 



1234 



0.493 



956 



0.531 



S. 



621 



0.495 



445 



0.542 



s. 



274 



0.556 



50 



0.587 



s, 





0.559 



15 



0.394 



