580 
MR. J. NORMAN LOCKYER ON THE 
and the continuous spectrum at these points is most intense, whilst a prominence 
occurring at any part of the sun’s limb does not appear to alter the intensity of 
the coronal ring at the corresponding part. Besides this principal ring we should 
expect to see some of the fainter ones shown on the African negatives, if their 
presence was not masked by the intense continuous spectrum, but there are indica¬ 
tions of others in less actinic parts of the spectrum, which are not shown on the 
African plates. 
Photographs about End of Totality. 
The chromosphere begins to put in appearance again, but only feebly, in Photograph 
1 6 ; between this and the next plate a change of slides was made, and a considerable 
time elapsed. In consequence of this rather large interval between the lGth and 17th 
exposures it is slightly difficult to estimate more than approximately the length of 
time the chromosphere was visible, but probably corresponds very nearly to that at 
the beginning of the eclipse. Photograph No. 18 was the last exposed during totality; 
the sun reappearing between exposing this plate and No. 19, the spectrum of the 
chromosphere is shown by long arcs corresponding to Hg, H y , H s , H^, H,,, H„, some 
of the principal Oa and Sr lines and some He lines. The spectrum of the corona is 
represented by the continuous spectrum, intensified in the two strong bands at the 
top and bottom of the spectrum for reasons explained previously. 
Photographs Out of Totality. 
The first photo, out of totality was No. 1 : it was given an instantaneous exposure, 
and a narrow band of continuous spectrum extends from one end of the plate to the 
other ; besides this there seems to be no indications of any arcs from the prominences 
except those corresponding to H^, H y , H 6 , H e , and K. 
In this respect it is very similar to Photograph No. 22, taken at the African station. 
The first photo, after totality, No. 19, was exposed for 5 seconds, probably com¬ 
mencing about two seconds after the sun broke out. During this time the sun was 
sufficiently uncovered to present a thin crescent, and the photograph show's a Fraun¬ 
hofer spectrum with arcs in place of the lines observed in the ordinary way. 
In consequence of the long exposure the Fraunhofer spectrum is solarised, and out¬ 
side this the plate is much fogged with stray light, which was then becoming strong, 
but here and there, where a prominence was unusually high to show" beyond the edge 
of the moon, and bright enough to be seen above the stray light, are a few" dots from 
the top of a prominence, in positions corresponding to the h}'drogen lines. The 
remaining five plates are very similar to the one described above, except that as the 
crescent of the sun became broader, the Fraunhofer spectrum is more ill defined. 
