M iscellaneous. 331 
On further scrutiny, with the aid of an opera-glass, two sharply cut and 
very narrow dark channels, bounding the principal ray, could be traced 
for ten or fifteen degrees from the nucleus; while outside of them, on 
either side, were two additional faint rays. The whole issue of nebulous 
matter, from the nucleus far into the tail, was curiously grooved and 
striated. It was noticed that both the principal ray and the dark chan- 
nels penetrated within the outline of the curved tail, the latter being clearly 
separated from the principal ray, even to the naked eye, by a dark cleft 
just above their intersection. The well-defined margin of the principal 
ray admitted of a very exact delineation, even as far as « Ophiuchi, 100° 
from its origin. 
On the 3d, the bright rays and dark channels were traced to a dis- 
tance of 40° from the nucleus, the principal ray to nearly 100°. Five or 
six alternations were distinguished, besides the hazy filaments consti- 
tuting the curved tail. Some of the streaks could be traced quite up to 
the nucleus. The rays were not only separated by the dark channel par- 
 rallel to their axes, but they were disconnected at intervals in the direc- 
tion of their length. 
On the 4th, there were two or more regions of contrary flexure on 
the north following margin of the ray, which, in a theoretical point of 
view, are of very great interest when taken in connection with the direc- 
tion of the ray almost precisely in a great circle from the sun continued 
through the nucleus. This peculiarity presented itself still more deci- 
seus on the 5th, when the tortuous path of the ray could not be over- 
looked. 
The very singular aspect of the northern edge of the principal ray for 
the first thirty or forty degrees of its course attracted particular atten- 
tion, and the charts were revised with all possible care. The sky was 
perfectly clear, and the outlines so distinct that there could be no room for 
doubt as to the reality of the reflexure of the curve. Subsequently, on 
projecting an arc of a great circle from the sun through the nucleus, it 
- was found to he clearly within the margin of the ray as far as a distance 
of thirty degrees (30°) from the nucleus, and there was still haziness be- 
yond it, almost to the distance of sixty degrees (60°). The charts on 
other dates indicate similar results, but the data cannot be properly dis- 
- eussed without requiring more labour than be at present devoted to 
them. 
Within the last few days the principal ray in the part near the nucleus, 
has assumed a more regular sweep in the direction opposed to that 
of the diffuse tail,,which now reaches nearly to the centre of Corona 
Borealis, scarcely changing the course of its southern limit between x 
and ; Bootis and ¢ Corone Borealis from night to night. 
The telescope phenomena, though interesting, have not presented equally 
strongly defined features with those which characterised the great comet 
of 1858. We should perhaps except from this remark their structure for 
a day or two after their first emission from the nucleus. In this stage 
they were intersected by jets of luminous matter projected from the nu- 
cleus, and these limits were clearly outlined. 
On the 2d, portions of three were visible; the inner one showing a 
variety of details. In its outline and general aspect it was, like others 
which followed it, almost a fac simile on an enlarged scale of some of 
those exhibited by the great comet of 1858. They rapidly faded, or were 
lost in the surrounding haze, and their places were filled with new ones. 
Latterly, two, at most, could be seen at one time. It is quite important 
to remark that the successive envelopes resembled their predecessors not 
only in their general aspect but quite closely in the details of their struc- 
ture; the luminous jets not issuing at random from all points alike of the 
