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The sky has continually been for the greater part overcast by 
alto-cumuli, and only now and then the sun was uncovered during 
some moments. During totality the sun was uninterruptedly behind 
the clouds which only towards the end became thinner. 
This was the cause that, after the considerable dispersion it had 
to undergo in the great spectrograph, the light of the corona was 
too faint to make a perceptible impression on the photographic 
plate, and hence, contrary to what we first inferred from the telegrams, 
the very important observations with this instrument, from which 
we hoped to derive data on the mode of rotation of the corona, 
have entirely failed. 
Some results are obtained with the small spectrograph and with 
the prismatic camera, even though they have suffered much from the 
unfavourable circumstances. The object of these two instruments was 
to obtain images of the whole spectrum of the corona, and of that 
of the ,flash’’ at the beginning and the end of totality. This purpose 
has been attained reasonably well with regard to the second flash 
and perhaps also to some extent with the corona-spectrum. More- 
over the flash has been observed in the visual slit-spectroscope. 
The images of the corona have better succeeded than the spec- 
tral-plates. The 6 plates exposed in the focus of the 40-feet-lens 
are all satisfactory and 3 of them are even good. 
Six photographs have been made with the telescope of 10 inches 
aperture without using the BURCKHALTER-apparatus, of which 3 have 
succeeded. During the three exposures with that apparatus the images 
have been slightly displaced, yet they can partly be used. Of the 
6 photegraphs made with each of the smaller telescopes and came- 
ra’s, among which DALLMEYER’s telescope, half can probably be used. 
The latter result may relatively speaking be called satisfactory ; 
the very unfavourable condition of the weather appears among others 
from the fact that on one of the plates exposed in the focus of the 
portrait-lens nothing but clouds are seen and no trace of the corona 
is visible. 
Observations with the polarimeter were made before, during and 
after totality. The observations during the partial phases at a distance 
from the sun equal to the sun’s diameter gave no polarisation. 
During totality the light near the sun was distinctly partly polarised, 
and this was strongest at some distance from the sun; it may be 
however that the clouds have had a perceptible disturbing influence 
on this result. 
With Prof. Junius’ apparatus for the measurement of the radia- 
tion of heat observations were made from the moment of the first 
