576 
MR. J. NORMAN LOCKTER ON THE 
Photographs taken near the end of Totality. 
Two photographs, Nos. 20 and 21, were taken during the visibility of the chromo¬ 
sphere in the south-west quadrant just before the end of totality. No. 21, taken 
with an instantaneous exposure affiout 10 seconds before the end of totality, is 
reproduced in Plate 11, and it will be seen that the appearances are very similar to 
those photograjffied near the beginning of totality. The spectrum of a long arc of 
chromosphere and of numerous prominences are very strongly marked, and the full 
dimensions of the large group of prominences near the sun’s south pole are at the 
same time revealed. This group was large enough to be visible throughout the whole 
of totality, but others are only visible in the photographs near the beginning and end. 
The spectra of the prominences are again of various degrees of complexity. 
The corona is represented chiefly by continuous spectrum, but faint arcs representing 
coronal radiations can also be distinguished in the negatives; one, a little less 
refrangible than H, is sufficiently bright and defined to be seen in the reproduction of 
Photograph No. 21. The continuous spectrum of the corona in these photographs is 
brightest on the western (lower) edge, for the reason that at that part of the sun’s 
limb the moon’s edge was nearer to the photosphere than at the opposite limb, so that 
a brighter part of the corona was exposed. 
The coronal ring corresponding to 1474 K is not seen in either No. 20 or 21, as the 
plates were not isochromatic. 
Unfortunately, the attempt to make an exposure at the moment of third contact 
was not successful, for the reason already stated. 
Photographs taken out of Totality. 
Six photographs (Nos. 1-6) were taken before totality, and nine (Nos. 22-30) after 
totality. 
The first five show nothing but a curved Fraunhofer spectrum, the visible 
crescent acting as a curved slit. No. 6 shows a similar spectrum with the addition 
of five short bright arcs at the cusp nearest to the north point in continuation of the 
dark arcs due to Ip, H y , Ip, and H and K ; it also shows faint impressions in H and 
K radiations of the prominences in the region of the sun’s south pole. Photographs 
27 to 30 inclusive also give nothing but a Fraunhofer spectrum, the curves being 
diametrically opposed to those appearing in the photographs taken before totality. 
Photographs Nos. 25 and 26 show in addition bright projecting arcs at H and K, H y , 
H s , and H f . 
The most valuable photographs taken out of totality are Nos. 22, 23, and 24, 
all taken within about 12 seconds from the end of totality. During this interval 
the photospheric light was sufficiently reduced to exhibit the radiation spectra of the 
surrounding vapours. 
