( 200 ) 
Hence I have repeatedly sought for dark cores in the chromospheric 
ares on photographs taken during former eclipses, and have indeed 
found several indications of them; but a plate where this peculiarity 
was the rule, where all the chromosphere lines were double, has 
certainly never before been obtained, for if so, the phenomenon could 
not have escaped notice. 
The Dutch expedition had the fortune. to get the first plates 
which quite clearly show all the chromosphere and flash lines, visible 
on them, to be double lines. 
This important result is in the first place due to the great care 
with which the whole plan of observation with the beautiful prismatic 
camera of COOKE was designed and elaborated by Prof. NyLAND, and 
not less to the extraordinary exactness, with which both before and 
during the eclipse he has performed all necessary manipulations. 
But besides, it is not impossible that the result was favourably 
influenced by the in other respects very unfortunate cloudiness of 
the sky. For if the light had not been considerably weakened, the 
chromosphere lines would have been found on the plate both broader 
and in greater number, and the doubling would have been perhaps 
as little marked as on the plates, obtained on former occasions. 
Shortly after the second contact five exposures were made on one 
plate, each of them during about 3/, sec. They show each only 9 
lines, all double. On the four plates, prepared for the corona spec- 
trum, some of the stronger chromospheric lines are represented by 
often interrupted arcs. The light of these evidently comes from 
prominences which project rather far beyond the photosphere. Here 
it appears not so easy to distinguish the duplication, just as we 
might expect by our theory; but still it is visible at many places. 
On the sixth plate another set of five exposures, of %/, sec. each, 
were taken a little after the third contact. In the first of the spectra 
thus obtained (reaching from 4 3880 to 4 5000) 150 double chro- 
mosphere lines can be counted between A 3889 and A 4600, these 
being also visible in the other four spectra, as far as the increasing 
scattered light permits !). 
A little below the continuous spectrum, due to the just appearing 
edge of the sun, the double lines are most conspicuous. We find there, 
parallel to the spectrum, a bright narrow streak which appears broader 
1) On the original negatives the duplication can only be distinguished with a 
magnifying glass. Enlargements (which were shown in the meeting) will soon be 
reproduced and published. 
