714 
PROFESSOR J. N. LOCKYER ON RESULTS OBTAINED WITH THE 
No. 7 (Plate 9) was taken very shortly after the commencement of totality, the 
exjiosure being “instantaneous.” At this phase of the eclipse a considerable arc of 
the chromosphere was visible, and its spectrum is therefore shown in addition to the 
si^ectrum of the higher reaches of some of the large prominences extending beyond 
the moon’s limb. It will be seen that at H and K there are almost complete circles 
of chromosphere and jorominences, the absent portions being of course obscured by 
the moon. One very small prominence is especially rich in lines, including some of 
iron and manganese. 
No. 9 (Plate 10) was taken about 8 seconds later with an exposure of 5 seconds. 
Practically all the chromosphere is now covered by the moon so that only the spectra 
of prominences and corona are visible. With the increased exposure the ultra-violet 
spectrum is considerably extended, and the spectrum of one of the prominences 
reaches as far as h in the green. The continuous spectrum of the corona is also more 
strongly represented in this photograph. In this photograph the spectrum trailed 
slightly at right angles to its length owing to a defect in the driving screw of the 
telescope. 
Nos. 12 and 16 (Plate 9) were taken at later stages with instantaneous exposures. 
They differ from the others only in point of phase. 
No. 17 (Plate 10) was taken on an isochromatic plate with an exposure of 
40 seconds. The spectrum extends from the ultra-violet to the less refrangible side 
of D, Dg being a well-marked line. The characteristic coronal radiation at X 531 5’95 
(1474 K) is represented by portions of a well-defined ring at that wave-length. 
No. 21 (Plate 9) was taken shortly before the end of totality, a portion of the 
chromosphere being again visible in addition to numerous prominences. It will be 
seen that one of the smallest prominences is rich in lines and closely resembles that 
which appears in No. 7. 
No. 22 (Plate 10) was taken immediately after totality, the exposure being about 
5 seconds. 
Six of the photographs taken out of totality show bright lines in the same way, 
but the remainder show only the Fraunhofer lines, the thin crescent of the sun then 
visible acting as a curved slit. The latter plates will be of value, however, as 
comparison spectra for the final reductions. 
A word of caution is necessary with regard to the ill-defined broad ring, a little 
more refrangible than I), which is seen in photograph No. 17. Experiments made 
since the eclipse indicate that this particular ring, and possibly other less distinct 
ones which are more refrangible, may be produced by a purely continuous spectrum. 
The isochromatic plates employed have two well-marked maxima of photographic 
action, one at a point a little more refrangible than D, and another about G ; this 
appears to explain the origin of the rings in question. 
