G84 
DR, W. HUGGINS ON THE PHOTOGRAPHIC SPECTRA OF STARS. 
Lines. 
H 
4340 
OL 
3887-5 
4137-5 
thin. 
9 
3834 
4120 
thin. 
3816-1 
h 
4101 
7 
3795 
4022-5 
thin. 
C 
3767-5 
4004-5 
thin. 
€ 
3745-5 
3968 
? 
3730 
3944-5 
thin. 
V 
3717-5 
K 
3933 
probably present as a thin line. 
e \ 
3920 
thin. 
11 
thin 
doubtful 
§ XIII. a Aquilce. 
All the lines are narrower than in Vega, and are well-defined at the edges. In 
this spectrum we have numerous lines, besides the twelve strong lines, and the 
spectrum may be regarded as changed considerably in the direction of stars of the 
solar type. The line K is now strong, though still inferior to H. Six lines have 
been measured in the spectrum beyond i, and possibly there may be lines still more 
refrangible. In addition to these, seventeen fine lines have been measured between 
the strong typical lines. 
Lines. 
H 
h 
4230 
4172-5 
4131 
4120 
4101 
4072 
4022-5 
pair of lines. 
4000 1 . 
3997 } pair - 
H x 3968 
K 3933 
3915 
« 3887 5 
3862-5 
3854 
/3 3834 
ft 3816 
3807-5 
7 3795 
a 3767-5 
3757-5 
6 3745-5 
f 3730 
r, 3717-5 
e 3707-5 
< 3698 
3690 
3677-5 
3656 
3654 
3637-5 
§ XIV. a Cygni. 
If we consider only the breadth of K and the narrowness and defined character of 
the lines, this spectrum is much altered in the direction of the solar type. On the 
other hand, few lines beyond the typical ones are present. The photograph is not 
strong, and I have not been able to measure the two most refrangible of the typical 
lines 9 and i, 
