210 
SIR NORMAN LOCKYER AND MR. F. E. BAXANDALL 
Comparison ol Groups of Chromosplieric Lines belonging to Various Metals M’ith 
Liveing and Dewar’s Gaseous Lines. 
Chromosphere 
(Humphreys). 
X. 
Origin. 
Atmospheric Gases 
(Liveixg and Dewar). 
Humphreys. 
Kensington. 
Most volatile. 
Xenon. 
Krypton. 
f3829-5 
Mg 
Mg 
3830 
3829 
3832-5 
Mg 
Mg 
— 
_ 
— 
[3838-4 
Mg 
Mg 
— 
— 
— 
/ 3944-0 
A1 
A1 
3944-0 
13961-6 
A1 
AI 
— 
— 
— 
14046-0 
Fe 
Fe 
4047 
4045 
4063 - 7 
Fe 
Fe 
_ 
_ 
L4071-9 
Fe 
Fe 
— 
— 
— 
14077-9 
Sr 
p Sr 
14215-7 
Sr 
p Sr 
— 
4215 
— 
14254-5 
Cr 
Cr 
4274-9 
Cr 
Cr 
_ 
_ 
_ 
1 
[4289-9 
Cr 
Cr 
4290 
— 
— 
14383-6 
Fe 
Fe 
4404-9 
Fe 
Fe 
_ 
_ 
_ 
[4415-2 
Fe 
Fe 
4415 
— 
— 
14508-5 
Fe ? 
p Fe 
4508 
J 
4515-5 
— 
p Fe 
_ 
- 
_ 
S 
4520-7 
Fe ^ 
p Fe 
_ 
■ ■ ■ 
. 
[4522-9 
Ti 
p Fe 
4523 
— 
— 
From this comjiarison it would appear that Professoi' Dewar claims for xenon, one 
member of tlie magnesium trijilet (W 3829‘5-3838’4), one component of the aluminium 
double (XX 3944‘0, 3961‘6) and one member of the strontium pair (XX4077‘9, 4215‘7); 
for krypton one member of the iron triplet (XX 4046"0-4071‘9); and for the most 
volatile gases, one member of tlie magnesinm ti'iplet, one of each of two iron triplets, 
one of a chromium trijilet, and two members of the enhanced iron t|uartette 
(XX 4508‘5-4522‘9). It is, of course, quite possible that some of these gaseous lines 
may account for the coronal lines ; but that the chromospheric lines ai'e, in the main, 
produced by metallic vajjoui’s, there can be no doubt. 
Comparison of y Cygni and a Cygni. 
It will be seen that there is a much greatei' number of lines in the spectrum of 
y Cygni than in that of a Cygni. The lines occnrring solely in y CVgni Avhich have 
been traced to any terrestrial origin are found to be attributable to the ordinary 
