608 
MR. J. NORMAN LOCKYER ON THE 
eclipse phenomena have been found to be as bizarre, in relation to the non-dissociation 
hypothesis, as those which I have already discussed in relation to observation of 
sun spots and of the chromosphere and prominences without an eclipse. 
The view I expressed in 1879,* and to which I adhere, is therefore strengthened 
by the eclipse work. I then wrote: “The discrepancy which I pointed out, six 
years ago, between the solar and terrestrial spectra of calcium is not an exceptional, 
but truly a typical, case. Variations of the same kind stare us in the face when the 
minute anatomy of the spectrum of almost every one of the so-called elements is 
studied. If, therefore, the arguments for the existence of our terrestrial elements in 
extra-terrestrial bodies, including the sun, is to depend upon the perfect matching of 
the wave-lengths and intensities of the metallic and Fraunhofer lines, then we are 
driven to the conclusion that the elements with which we are acquainted here do not 
exist in the sun.” 
XII. General Conclusions. 
(1.) With the prismatic camera photographs may be obtained with short exposures, 
so that the phenomena can be recorded at short intervals during the eclipse. 
(2.) The most intense images of the prominences are produced by the H and K 
radiations of calcium. Those depicted by the rays of hydrogen and helium are less 
intense and do not reach to so great a height. 
(3.) The forms of the prominences photographed in monochromatic light (H and K) 
during the eclipse of 1893, do not differ sensibly from those photographed at the 
same time with the coronagraph. 
(4.) The undoubted spectrum of the corona, in 1893, consisted of seven rings 
besides that due to 1474 K. 
The evidence that these belong to the corona is absolutely conclusive. It is 
probable that they are only represented by feeble lines in the Fraunhofer spectrum, 
if present at all. 
(5.) All the coronal rings recorded were most intense in the brightest Coronal 
regions near the sun’s equator as depicted by the coronagraph. 
(6.) The strongest coronal line, 1474 K, is not represented in the spectrum of the 
chromosphere and prominences, while H and K do not appear in the spectrum of the 
corona, although they are the most intense radiations in the prominences. 
(7.) A comparison of the results with those obtained in previous eclipses confirms 
the idea that 1474 K is brighter at the maximum than at the minimum sun-spot 
period. 
(8.) Hydrogen rings were not photographed in the coronal spectrum of 1893. 
(9.) Do was absent from the coronal spectrum of 1893, and reasons are given which 
suggest that its recorded appearance in 1882 was simply a photographic effect due to 
the unequal sensitiveness of the isochromatic plate employed. 
* ‘ Roy. Soc. Proc.,’ 1879, vol. 28, p. 13. 
