174 
SIR NORMAN LOCKYER AND OTHERS ON THE 
consisted of a patchy arc, extending over about 150° of the sun’s circumference, 
on the N.E. Nearly continuous, hut varying in height from about 1' to 
broken near the equator, continued on the S.E., where there was a peculiar whorl¬ 
shaped prominence about 2 feet in height. This was shown complete in two red, 
one orange, and three yellowish-green images (close together). In two greenish- 
blue images and one blue one, patches only of these arcs were observed, very 
disconnected in the north-east, and only slightly more continuous in the south-east, 
where the arcs were broadest, thus aj^pearing to consist of the bases of the greater 
projections. The yellowish-green arcs were very bright, the red somewhat less so, 
the remainder being relatively faint. The red arcs appeared to be the most com¬ 
plete, the yellow-green slightly less so, the orange still less continuous, the blue 
and others very Incomplete. 
“ At about G5 seconds after the commencement of totality, rings were observed, 
discontinuous, but extending round the whole of the sun’s circumference, of the same 
general character as the arcs before mentioned, but slightly larger in diameter. Two 
rings in the red appeared broader and more regular than the rest; three in the 
yellowish-green, very close together, were brighter, Imt not so extended as the first ; 
and one in the orange was much less complete and fainter, but similar in shape to the_ 
red and yellow-green. These rings were represented in the greenish-blue and blue 
by only a few isolated patches, principally in the north-east. 
“Seventy seconds after the commencement of totality, these rings had disappeared 
on the east side, leaving arcs surrounding the west side, similar in appearance, 
omitting the whorl-shaped prominence, to those first observed. These arcs gradually 
became broader and more connected, the blue and green-blue becoming nearly 
continuous. 
“ Two minutes after commencement these rings were all much more connected and 
broader, while preserving their relative breadth and brightness. 
“About 125 seconds after commencement a number of bright arcs suddenly 
a])j)eared, covering the structure of the arcs previously described. The number seen 
might be estimated at about twenty, but this is not considered reliable, as the arcs 
rapidly laded ; in about one second they were obscured by bright continuous 
spectrum. 
“In half a minute two dark lines appeared in the red, one in the orange, a broad 
one in the yellowish-green, one in the green-blue, and one in the blue, gradually 
becoming broader and losing definition until five minutes after totality, when they 
were not distinguishable. 
“ During tlie whole period of totality, a continuous spectrum was observed, faint 
at the ends, but increasing in brightness about the 3 mllow and green, where it was 
nearly half as bright as the bright arcs observed in that part of the spectrum. No 
detads of structure were observed in this spectrum, but its width was about twice 
the apparent diameter of the sun. 
