,,K. U. M. HICKS: A CRITICAL STUDY OF SPKITUAL SERIES. 



Tin- >////'. S. r i,--iiinM. As the values of the satellite differences are practically 

 Jndewodanl <-!' ih.- exact value of D(), their consideration may be taken up at 

 ,,. ..,,! th-- details of the calculations respecting the tables postponed until the 

 consideration of the older differences. An examination of the tables will show 

 ,,,,,,.hisiv,-ly that these differences are multiples of the "oun." Dealing first with 

 tli,- differences for the first lines, the following figures, contained implicitly in th.- 

 tables, will show how closely this is the case. The nearest multiples of the oun are 

 appended, as calculated from the first approximations of Table I. The possible errors 

 are those of the D,, lines (except Zn). 



Cs. 



Cu 



&g 



Ca. 



Sr. 

 Ba. 



Zn. 



7394 228 46*, = 7340 



7 94 43 22*, = 804 

 2424 19 23*, = 2422 



f 7468 51*, = 741 



'1 45025 31*, = 451 



j"36207 52*, = 3596 



\2170? 31*, = 2154 



. . Not observed, as deduced 



below (p. 388), 15*, 9*, 



or 60*,, 36*, 



T 52577 IS*, = 581 

 ' 'I 369 28 9*, = 350 



The only case of " failure " is the first difference for Sr in which the estimated 

 possible error is extremely small. If the possible error be the sum of those of each 

 line, the value is 15 in place of 7, and if *, be calculated from the most probable 

 value of the oun it should be about i D greater, i.e., 52*, = 3600. It will be noted 

 that where triplets enter, the two satellite differences, and consequently the two 

 satellite separations, are extremely close to the ratio 5 : 3. This ratio seems to 

 persist also in Hg where the separations are in reverse ordtir, and we find a ratio of 

 3 : 5 in place of 5:3. The law for this ratio is in fact much more closely obeyed 

 than the corresponding one for the ratio 2:1 for the triplet separations. It is 

 therefore of great assistance in searching for the lines of F series whose limits are 

 VI ) ('!}, and which consequently possess constant triplet separations in this ratio. Its 

 explanation should be expected to throw some valuable light 011 the constitution of 

 tin- atom. The general dependence of the differences on the small "oun" J, should 

 also be noted. 



Passing now to the consideration of the satellite differences for orders beyond the 

 first (m>'J), it is seen that they still depend on multiples of the oun, but different 

 from those of the first order. In a large number of cases the multiples are the same 



