190 
SIE NORMAN LOCKYER AND OTHERS ON THE 
About 2 minutes after totality. —“F” long and bright. 
Magnesium (“ h ”) short and bright. 
Call 3 minutes after totality. —Only continuous spectrum udth Fraunhofer lines. 
Call 5 minutes after totality. —Ordinary continuous spectrum, with dark lines 
“ F” again coming in brightly for a short time. 
Call 7 minutes after totality. —“ F ” bright but faint, and very short. 
No other bright lines. 
Only ordinary continuous spectrum with Fraunhofer lines. 
iSiote. —The portion of the spectrum observed was from “F” to just beyond 
“ 1474 K.” 
It will therefore be seen that in the s})ectrum of the corona the arc lines of iron 
were seen, and also magnesium and hydrogen, together with the coronal hne 1474 K, 
all of tliem bright. On the other hand, I was unable to rej^eat the observations made 
by Sir Norman Lockyer in the eclipse of 1882. A further point which may be 
noticed is that I was able to observe distinctly the coronal line 1474 K bright beyond 
the cusp of the sun one minute after totality. No carbon bands could be detected at 
any time. 
Remarlcs on the Observations. 
The preceding obsei'vations of bright lines may be conveniently summarised as 
follows :— 
F. 
F, 
r 10 miii.-l min. 
At cusp before tot.Mity s 4 mm.-2 min. . . 
b 2 min.-l min. 
Cliromosjmere . . . Beginning of totality. 
Inner corona (3' from f About 120-97 secs, calls 
eastern limb) f time keeper. 
Signal. 
Outer corona (IG' from f 97-G7. 
eastern limb) LG7-47. 
Inner corona (3' from 132-17. 
eastern limb) Ll7-. 
[ 0 min.-l min. . 
I 1 min.-2 min. . 
Cusp after totality . . 
[ 2 niin.-3 min. . . . 
. F, h, Fe arc quartette. 
8 or 9 bright lines benveen F and h. 
by F, 1474 K, and 4 or 5 feeble lines, 
possibly identical with iron quartette. 
F, 1474 K, trace of . 
No lines seen. 
F, 1474 K. 
F, 1474 K, no Fe lines. 
F, h. 
F, h, 1474 K, three members of iron 
quartette. 
F, 
As regards the attempt to repeat the observations ot 1882, it may be remarked 
tliat the want of complete success was probably due to faintness of the spectrum as 
seen with a grating, and the difficulty of observing the shorter lines in consequence of 
tlie small size of the image projected on the slit. So far as they go, however, the 
