188 9. J Variability in condensing Swarms of Meteorites. 419 



Spectra. 



Rrj. 



Ej. 



Jr. 



Jjr. 





— 



2 



10 



— 





— 



— 



15 



— . 





3 



5 



9 



— 



2 — 8 bands moderately wide and dark, 2 and 3 













— 



5 



36 



4 





— 



— 



3 



2 



2 — 9 bands moderately wide and dark, 2 and 3 













— 



4 



6 



— " 



1 — 9 bands moderately wide and dark, 2 and 3 













— 



1 



2 







1 — 10 bands wide and moderately dark, red strongest 



— ■ 



— 



1 



— { 





3 



5 



— 



— 





— 



1 



1 







— 



5 



4 



— 





1 



5 



4 



1 





1 



5 



21 



— 





— 



3 



— 



— 





4 



13 



5 



— 



2 — 8 ivide and dark, blue strongest 



— 



1 



— 



1 





5 



10 



6 



1 





— 



6 



20 



1 







1 



1 







— 





5 



~~ | 







2 



6 





O Q K h Q 







Z 



1 1 







1 



6 









3 



3 



± J 





3 



8 



10 





20 



86 



176 



12 ! 



preddish-yellow, 

 | yellowish-red, 

 Group II. . . . <J red, 



yellowish-red, 

 ^reddish-yellow. 



Hence no definite conclusion as to temperature of Group II stars can 

 be arrived at by colour observations alone, since stars cooler than the 

 mean, as well as hotter, give the same colour. 



The Cause of the Relation between Colour and Period. 



On reference to the tables of variables, it will be seen that there are 

 none less condensed than Species 7. This means that the sparsest 

 swarms either exhibit no variability at all, or their variability is of such 

 a character as to escape notice. The reason for this is not far to seek. 

 Firstly, if there be any revolving swarms with small orbits, they will 

 never be entirely out of the central swarm, and their effect will 

 simply be to produce a general increase of brightness of the swarm. 



