SCIENTIFIC SUMMARY. 
93 
sun be the plane of condensation of gaseous matter, this plane may be found 
to be subject to periodical elevations and depressions in the solar atmosphere. 
It may be that at the epoch of minimum spot-frequency this plane is up- 
lifted very high in the solar atmosphere, so that there is comparatively little 
cold absorbing atmosphere above it, and therefore great difficulty in forming 
a spot. If this were the case, we might expect a less atmospheric effect or 
gradation of luminosity from the centre, to the circumference at the epoch of 
minimum than at that of maximum spot-frequency.” 
The important observation made by Lockyer, above referred to, has 
been confirmed by Secchi and Brodie, whose paper, printed in the last 
number of the “ Monthly Notices,” describes an almost identical phenomenon. 
We think, therefore, that it is not premature to look upon the down-rush 
and consequent melting of masses of photospheric matter into a spot as 
established ; with this a most important point is gained. Here we have 
a field of observation opened out to those who have large telescopes sur- 
passing immeasurably in interest anything belonging to the willow-leaf 
controversy. 
We must now refer to other solar observations made in the southern 
hemisphere. 
The Bulletin International for Dec. 12 and 13 contains a communication 
from Father Secchi, detailing the observations made by Father Cappelletti 
at La Conception, on the total eclipse of April 15 of the present year. 
Following the example set by Mr. De La Rue in the famous Spanish 
eclipse, Father Cappelletti set himself the task of photographing the red 
protuberances. Unfortunately, however, a mist rendered these attempts 
unsuccessful ; but the eye observations were of the greatest interest. The 
first appearance observed after the commencement of the totality was that 
of an immense fiery mountain, of a rose colour, in shape like a horn. This 
prominence was observable for 2 min. 22 sec. Almost diametrically opposite 
to this there was a smaller one, similar in form, but clearer in colour. The 
former was estimated at 2 min. 40 sec. and the latter 2 min. in height. After 
38 seconds there appeared a series of rose-coloured flames, as if the sun were 
on fire, and which fired in succession like a train of powder. The light of 
these was very vivid. 
A rainbow in form of a crescent, some 30 deg. from the sun, its extremities 
resting on a tangent to the lower limb of the sun, was also observed. 
When the sun was obscured, three faculae of light were observed in a 
direction normal to the edge of the moon. One of them was so bright, that 
the eye could scarcely bear to look upon it in the telescope. 
We now know, thanks to Mr. De La Rue’s photographs, and the investi- 
gations of the Astronomer Royal, that the words “ apparent diameter of the 
moon ” mean very much more than is ordinarily assigned to them. Time out 
of mind, the “ new 5 moon,” which carries the “ old moon ” in its arms, has 
been looked upon as a larger fellow, but it did not strike us that this effect 
of irradiation would be perpetuated in our telescopes. This, however, is the 
case, as has been recently proved by measuring the dark moon — a feat of 
observation rendered possible, we may remind the reader, in solar eclipses 
and occultations of stars at the dark limb. 
