jSee — Temperature of the Sun and Ages of Stars and Nebulae. 29 



^ = 1. The value r = 0, or c = 0, corresponds to the value 



(IT drj 



a = 0, and hence by (48) -^ =0, or ^ = 0. Finally, 



T= Tq,ovv = l,fore=0. 



If now we seek to find the law, according to which ^ and ij 

 change, and represent the result by a curve which is corrected 

 by successive approximations till it satisfies the above differ- 

 ential equation in all its points, we shall have the following 

 numerical values, computed by Ritter : — 



0. 

 The constants v = 2.4, and ^ = 23. 



(T 



By means of these results and equations (51) and (48) we 

 derive the curves which — > and a represent geometrically. 







In this way we find the numbers given in the following table : 



-^=0 0.1 0.2 0.3 0.4 0.5 



0.6 0.7 0.8 0.9 1.0 



- = 1 0.88 0.64 0.39 0.20 0.10 



" 0.040 0.015 0.0038 0.00054 



a = 2.1 3.5 3.9 3.6 3.2 



2.5 2 1.6 1.2 



(B) 



In the case of the Sun, where the central density is, on the 

 gaseous theory, 23 times the mean value, we have the density 

 in units of the mean density and of water respectively : — 



1.0 



r 



a 



2.30 0.90 0.345 0.0874 0.01242 0. 



Spec.gr. = 32.2 28.34 20.61 12.56 6.44 



3.22 1.29 0.483 0.12236 0.017388 0. 



