126 



INORGANIC EVOLUTION. 



[CHAT. 



The following table will show the gradual increase in the number 

 of stars from the pole to the plane, as seen by the Herschels with a 

 reflecting telescope of 18 inches aperture and 20 feet focal length : * 



A consideration of the distribution of stars in right ascension 

 between declinations 15 N: aud 15 S., led Struve to the conclusion 

 that there are well marked maxima in K.A. 6 hrs. 40 mins. and 18 hrs. 

 40 mins., and minima in E.A. 1 hr. 30 mins. and 13 hrs. 30 mins.; 

 he remarks that the maxima fall exactly on the position of the Milky 

 Way in the equator, and further states that " the appearance of the 

 close assemblage of stars or condensation is closely connected with the 

 nature of the Milky Way, or that this condensation, and the appear- 

 ance of the Milky Way, are identical phenomena." 



Although the Milky Way dominates the distribution of stars, and 

 especially of the fainter stars, it does not appear to be the only ring 

 of stars with which we have to do. Sir John Herschel traced a zone 

 of bright stars in the southern hemisphere, which he thought to be the 

 projection of a subordinate shoot or stratum. That was the first 

 glimpse of a new discovery, which was subsequently established by 

 Dr. Gould in' his work in the southern hemisphere at. Cordova. He 

 found that there was a stream of bright stars to be traced through the 

 entire circuit of the heavens, forming a great circle as well defined as 

 that of the galaxy itself, which it crossed at an angle of about 25. 



Gould, while in the southern hemisphere, had no difficulty in 

 observing that along this circle, which we may call the Star Way, in 

 opposition to the Milky Way, most of the brighter stars in the southeni 

 heavens lie. 



When he subsequuently came home he made it a point of study to 

 see whether he could continue this line of bright stars completely 

 through the northern hemisphere, and he found no difficulty. So that 



*' Outlines of Astronomy, Herschel, pp. 535, 536. 



