TOTAL ECLIPSE OF THE SUN, JANUARY 22, 1898. 
175 
“No bright arcs were observed before or after totality. 
“ The records of the other four observers are similar, though somewliat less com¬ 
plete. The appearance of dark Fraunhofer arcs as the crescent became thinner, their 
replacement by light arcs at the commencement of totality, the change of the arcs 
from the east to the west side, and the reappearance of dark arcs was noted by all. 
“ The half-jilate camera, with diffraction grating, was manipulated by G. Gray, 
chief stoker. It was supported on a stand near the finder of the 6 -inch prismatic 
camera, a portion of the light from the siderostat of that instrument being intercepted 
and reflected into the lens of the camera by a right-angle prism. A photographic 
diffraction grating was fitted to the front of . the Cooke lens of the camera, and the 
whole was so arranged as to show three orders of the spectrum above and one below 
the image of the sun. Ordinary plates were used, as isochromatic ones of the proper 
size were not available. The exposures were made liy means of a sliding shutter 
fitted in front of the grating. Four plates were exposed, with varying exposures, 
namely, 10 secs., 65 secs., 15 secs., about 5 sec. For all the exposures F/A = 6'5.” 
lhmarl:s hij Sir Norman Lockyer. 
In discussing tliese observations, it is important to distinguish lietween rings 
produced by the light of the corona and tliose produced by the succession of promi¬ 
nences which surround the dark moon. An examination of the photographs taken 
with the prismatic cameras shows that the conditions with regard to tlie visibility of 
the chromosphere and prominences were as follows :—■ 
During first 30 seconds of totality. . CTromospheric arcs in N.E., jirominences 
in S.E., N.W., and W. 
During next 60 seconds.No chromospheric ai'cs visible, hut the 
succession of prominences appear as 
dotted rings. 
During last 30 seconds of totality . . Chromospheric arcs in S.W., prominences 
in S.E., N.W., N., and E. 
The green ring of the corona was visible tliroughout totality, and must have lieen 
visible to all the ohseiwers. Its variation from the fragmentary rings, due to chroino- 
sphere and prominences, however, appears to have almost escaped notice. None of 
the observations suggest the presence of a red coronal ring, so that there was no 
indication of hydrogen in the corona. 
The flashing out of bright lines at the commencement and end of totality was 
observed, and also the spectrum of tlie chromosphere and of the largest prominence. 
The lines seen in the latter were probably as follows :— 
