﻿Electric Source, and Line Spectra. 



Table II. 

 7 = -3660 6 ; & =3-5345; «=-4-0819. 



713 



i. 



i calc. 



X obs. 



A 



3 



•4338! 



•4340 7 H y 



-2-6 



4 



•4102 3 



•4102 3 8 



00 



5 



•3970 2 



•3970 2 e 



00 



6 



•3888 9 



•3889 2 i 



-0-3 



7 



•3835 5 



•3835 6 , 



-0-1 



8 



•3798 G 



•3798! o 



+05 



9 



•3772 3 



•3770 8 , 



+1-5 



10 



•3752 7 



•3750 2 K 



+25 



11 



•3737 



•3731 5 x 



+34 



]2 



•3726 2 



'3722 M 



+4-2 



13 



•3717 3 



•3712, „ 



+5-2 



14 



•3709 7 



•3704 ^ 



+ 57 



00 



•3660 



•3661 2 H 31 



-0-6 







■8646 a =X B 





becomes, after z = 13 or 14, ambiguous. There are again 

 superabundant lines, owing to the smallness of the interval 

 Xoo~ H 31 . Compare the remarks made above. To prevent 

 the premature crowding of the theoretical lines and to take 

 in, at the same time, the hitherto ignored lines H a , H^, the 

 convergence-point \ cc =y is pushed back, nearly as far as 

 Balmer's limit. Some of the results of the corresponding- 

 calculation, which is just started and is being assiduously 

 retouched (with regard to the values of a, / ), are collected 

 in Table III. Its chief purpose here is to show that the 

 enormous value of A for H a can well be reduced, although 

 at the price of spoiling to a certain extent the successive 

 lines, and that the superfluous theoretical lines can be entirely 

 abolished. It will be enough to give here the wave-lengths 

 to four figures only. 



The numbers (1), (2), etc. inserted in the third column 

 stand for " first, second, etc." observed line of the hydrogen 

 series; they mny facilitate the testing of coordination. It 

 is quite possible that the simplest dispersion formula (3a) 

 will turn out to be too narrow for the purpose of red 



lucmsr 



