330 
CAPTAIN L. DARWIN, DR. A. SCHUSTER, AND MR. E. W. MAUNDER 
Bj holrling, the photograpli against a bright sky, and examining it with a lens of 
about half an inch focal length, I can see what I have tried to represent in the 
drawing. But I could only carry on the work about an hour at the time, and it 
was always followed by strong pain and neuralgia in the eye, lasting sometimes for 
several days. I am sorry, therefore, not to be able to accompany this report wuth a 
complete set of drawings. The two specimens which 1 can give will, however, give a 
fair idea of the appearance of the lines on the photograph. The band reaching from a 
wave-length 4318'4 to a wave-length 4323'7 has a curious shape. It is broad near 
the centre of the field, where it is widest, and there nearly covers the bright space 
on the least refrangible side of the G band, which comes out so strongly in photo¬ 
graphs taken on a small scale. If it was of equal width throughout, I should have 
taken it for that band, coming out by contrast between the Fraunhofer line G and 
the group of lines at 4324. But the manner in wdiicli the line becomes thinner 
towards the outer parts of the corona shows that it must be a real band. 
As we go from this band towards the less refrangible side, we come to very compli¬ 
cated markings until we reach the Hy prominence. These markings I believe to be 
due to an overlapping of Fraunhofer lines and corona lines ; whether the difference in 
the appearance on the northern or southerji side is real or not I cannot be certain. 
The line at 4378’1 is the most conspicuous one in this part of the spectrum. By its 
side we can trace the Fraunhofer line 4383. The series of lines here seem to widen 
at the base of each bright band of the corona, and they are weak on the northern 
side. 
I have not been able to trace with certainty a difference in the lines of the spectrum 
of different parts of the corona, except that already mentioned of the calcium and 
hydrogen lines. The group of lines at 4076 (fig. 3, Plate 9) at first sight looks as if 
there was such a difference ; but we have here possibly only one broad band, and the 
lighter appearance in the centre may be a defect in the photograph, or it may be due 
to a Fmunhofer absorption line, which ought to be here, or, finally, to a reversal of a 
corona line against a hotter background. 
The results obtained with Spectroscope I. are much less satisfactory. The plate had 
a very narrow escape during development. Owing to the hot damp weather the films 
were often found to detach themselves from the glass in the develop)ing bath ; but we 
had not found any difiiculty when the bath was kept cool by ice, and when the film 
wus soaked with alum. Captain Darwin had kindly offered to do the whole of the 
photographic part of the work for me, and for this, as well as for continuous assistance 
in other ways, I have to offer my sincere thanks. The plate in question was developed 
during the afternoon of the eclipse. For some time nothing appeared, and when at 
last the image showed itself the plate at once began to frill at the edges. It was 
only by j-epeated treatment with ice and alum that Captain Darwin saved the plate, 
but the image is very faint. What this is due to, I cannot say with certainty. The 
plate was one of Captain Abney’s red end plates, and probably was less sensitive in 
