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PROFESSOR J. N. LOCKYER 0^1 THE PHOTOGRAPHIC 
similar to those used in the case of iron for corresponding regions, the first two 
sections being taken on the ordinary “ Mawson and Swan Castle Plates,” and the 
third on plates which had been stained with a solution of erythrosin. 
In the present paper, the first three series of photographs are discussed, the 
consideration of the composite meteorite spectra being reserved for a subsequent 
communication. 
The lines in the spectrum due to iron were found to agree so closely with those in 
the photographic arc spectrum of Electrolytic Iron, on which a paper was communi¬ 
cated to.the Poyal Society, in October 27, 1893, that all lines due to iron have been 
omitted from the tables, and only the lines due to other metals dealt with. The 
results are given in the appended table. The first column gives the wave-length of 
all the lines, other than those due to iron, which appear in the spectra, while the 
second and third indicate the approximate intensities of the lines in the Obern- 
kirchen and Nejed meteorites respectively. The scale of intensities is such that 
1 represents the strongest, and 6 the weakest lines. 
In the fourth column are given the probable origins of the lines. The evidence for 
the origins of some of the lines rests on the new map of the spectra of the elements 
which is in progress at Kensington. 
The last column is reserved for occasional remarks. 
General Conclusions. 
1. The spectra of the two meteorites agree very closely both as regards the 
number and intensities of the lines. The slight difference in the number of lines 
seen in the two spectra may be in all probability due to the difference in exposures of 
the plates. In the first section of the spectrum (A 390-421) the lines correspond 
exactly in number; in the next section (X 420-470) the spectrum of the Obern- 
kirchen meteorite was evidently under-exposed in relation to the other, so that it 
contains fewer lines; in the third section, the Nejed spectrum was relatively under 
exposed, and all the lines which are not common to the two in this region are absent 
from the spectrum of the Nejed. 
2. There is a very considerable similarity between the spectrum of the meteorites 
and that of the sun. The iron lines in the meteorites have the same relative 
intensity as those in the solar spectrum, and this is an indication that the tempera¬ 
ture of the iron vapour, in the most valid iron vapour absorbing region of the sun, is 
about the same as that of the electric arc. 
3. The results of tbe enquiry into the origins of the lines, in addition to those of 
iron, may be thus summarised :— 
