262 
MU. J. XORMAN LOCKrER O:^' THE RESE^LTS OBTAINED IX 
No. 11 is oil a scale of 2’1 times that of the original negative, being exposed for a 
period of 40 seconds, beginning at 39 seconds from the commencement of totality, 
so that it records the spectrum near mid-totality. The two overlapjiing disconnected 
rings to the left are the Images of the prominences round the sun’s limb represented 
in the H and K light, the other discontinuous rings to the right are the images in 
Hg, and radiations respectively, the ring further to the right, which is of 
more continuous structure than the others is the 1474 K ring of the corona spectrum. 
There are other fiiinter rings, both of the prominences and the corona, which are 
well seen on the original negative, but it is too much to hope that these will be seen 
in the Plate, being lost in the process of reproduction. 
F\s 1. 
1474 K ring. 
Corona. 
Fig. 1 shows an enlargement of the 1474 K ring compared with an oriented 
photograph of the lower corona. It will be seen that the prismatic camera has 
picked out the brightest parts of the corona, and where it is strongest the spectrum 
ring and the continuous spectrum at those points are most intense, whilst a pro¬ 
minence occurring at any point of the sun’s limb does not alter the intensity of the 
ring at the corresponding part. 
The wave-lengths of the lines in Photo No. 11 have been measured by Dr. W. J. S. 
Lockyer, and a j^reliminary comparison of the results obtained in 1893 and 1896 
has shown many points of difference ; it also indicates that the photograph of the 
flash so happily caught by Mr. Shackletox, and the cusp photograph secured by 
Mr. Fowler, in 1893, both represent the spectrum of the chromosphere. 
Except in the case of the lines visible in the spectrum of hydrogen, and the 
cleveite gases and the longest lines in the spectra of some of the metallic elements, 
notablv calcium and strontium, there is little or no relation between the intensities 
of the lines visible in the chromosphere and Fraunhofer spectrum. 
There is already evidence that the photographs which we owe to the public spirit 
of Sir Georoe Baden-Powell and the energy and skill displayed by IMr. Shackle- 
ton will considerably widen our knowledge of solar physics and chemistry. 
