EVOLUTION IN THE SUNS 55 



tion an opportunity which would be totally 

 unrealizable on earth of observing the effects 

 of high temperatures and the results upon the 

 constitution of matter. The nebulae have been 

 similarly studied and chemically classified. 

 At these spots in the universe temperatures 

 exist far exceeding such as are producable 

 upon earth by artificial means, and cosmic 

 history may be studied from which lessons 

 may be derived as to what happened millions 

 of years ago in the history of our earth, and 

 how the elements and substances found to-day 

 upon the earth's crust gradually came to be 

 formed. It is only by supplying this chapter 

 that the mind can be brought into proper 

 training for understanding how life arose, 

 much as one movement in a symphony pre- 

 pares the mind and senses for, and leads on 

 to another. 



In the solar and stellar spectra as photo- 

 graphed and charted by the use of the most 

 powerful telescopes and delicate spectroscopic 

 apparatus, many thousands of lines are visible 

 in definite positions. Some of these lines are 

 very strong and visible with ease through a 

 pocket spectroscope, such, for example, as 

 the double line or D line of sodium, used as 

 an illustration in the description above. 

 Such principal lines starting from the red 



