34 
which subsequently occurred. The question of identity 
may be definitely settled if any observations of the 
spot during the interval from January 13 to 27 are 
forthcoming from foreign observatories. In this part of 
England the sky was densely overcast at night during 
the whole of that time. If Prof. Hough at Chicago or 
some other systematic student of the planet can supply 
the missing links for the period referred to, it will be 
most important to ascertain how far they corroborate the 
assumed identity of the markings in question. 
These white spots are liable to great variations in 
apparent brilliancy at short intervals ; so that, unless an 
obseryer is very careful to discriminate between objects 
approximately situated, he is certain to introduce compli- 
cations into his results. But, in regard to the conspicuous 
white spot which has been the ‘subject of so much com- 
ment during the last few years, I have never found much 
difficulty in following it, because of its special character. 
Occasionally smaller spots slightly nearer the equator are 
seen on each side of it, but the leading spot of the trio is 
so bright and almost invariably shows a bright trail 
running from its north-east side towards the equator, that 
it may be readily identified. During the observations 
between October 4, 1884, and January 13, 1885, of the 
present opposition the extreme brilliancy of the spot was 
very noticeable, and the observations were pursued with- 
out any liability to error. I fear, however, that, morning 
observations being rendered necessary by the position of 
the planet in November and December will have enabled 
the singular vagaries of the white spot to have generally 
eluded notice. 
It is curious that since the end of January this white 
spot has maintained a rate very nearly conformable to the 
first meridian of gh. 50m. 12°25s., computed by Mr. Marth 
from the observations between 1882 and 1884; but there 
occurred a sudden deviation between March 14 and 18, 
amounting to some 8°. These singular displacements 
cannot be induced by changes in the form of the object, 
and they are far too considerable to be referred to errors 
of observation. Between February 9 and 16, 1882, Prof. 
Hough noticed an acceleration of 63°. 
The verification and true cause of these variations can 
only be efficiently sought out by frequent and very accu- 
rate observation. Our own climate is very ill-adapted to 
an investigation of this kind where the most essential 
point consists in closely consecutive results. What we 
need is an almost unbroken series. It is to be earnestly 
hoped that some attention will be devoted to this impor- 
tant work at the Lick Observatory, where “the elevation 
is 4200 feet above the sea, and for six or seven months of 
the year every night is clear! The position thus com- 
mands natural advantages (in this work of far more im- 
portance than instrumental advantages) which would 
enable it to obtain some most valuable evidence bearing 
on the question of the remarkable variations affecting the 
white spots on Jupiter. Near the time of opposition they 
might be observed every night, and it is this consecutive, 
close treatment that is required before the phenomena will 
really admit of satisfactory discussion. 
The question arises whether the whole southern belt 
partakes in these erratic and apparently frequent varia- 
tions of speed, or whether they are confined to proper 
motions affecting the individual spots at different times. 
If several markings were made the subject of contempo- 
rary study it might soon be determined whether they 
exhibited uniform displacements, and, if so, it would 
have to be admitted that the whole equatorial atmospheric 
current is subject to the singular onrushes and alternating 
lulls which our recent observations have demonstrated. 
Of the new features presented during the last few 
months the most striking are :— 
(1) The appearance of large, bright spots indenting the 
north edge of the great northern equatorial belt. A pecu- 
liarity of these objects is that lines of light flowing from 
NATURE 
[Way 14, 1885 
their west sides divide the dark belt and finally emerge 
near the equator, where they became indefinite. These 
spots show a rotation period only a few seconds less than 
the red spot. 
(2) The outbreak of dark, reddish spots, elongated in 
longitude, upon the narrow belt which became visible 
in 1882, immediately outlying the great belt. The de- 
pression north of the red spot was formed by the ends of 
this belt suddenly dipping northwards before reaching the 
spot where they became blended with the old belt. The 
spots now visible here are very plain and will probably 
increase until finally their material is dispersed around 
the planet and the belt becomes much darker than before. 
The individual spots should be carefully watched to 
ascertain whether this is their ultimate development. The 
rotation period they have hitherto shown is precisely the 
same as that of the red spot. One of the most con- 
spicuous of these new spots is about 10,000 miles long ; it 
follows the red spot th. 48m., so that its longitude is 66° 
east. 
(3) The fading away of the west shoulder of the de- 
pression north of the red spot. This is now very obvious, 
and extends along the narrow belt far to the west of the 
red spot. It remains to be seen whether this decadence 
will continue now that various other regions of the belt 
exhibit a confluent eruption of dark spots. 
The several features referred to are of extreme interest, 
as suggestive of peculiar forms of atmospberic disturb- 
ance and as affording fresh materials for students of 
Jovian phenomena. It will be necessary to follow each 
of these special features during the two ensuing months, 
and to recover them, if still visible, when the planet re- 
appears in the morning sky towards the end of October 
next. W. F. DENNING 
NOTES 
AT the conversazione of the Royal Society on Wednesday 
evening last week, the Fellows, we are sure, were all glad to see 
their President back again, in renewed health, after his long 
absence. Prof. Huxley had to welcometa very large number of 
guests, and some of the objects exhibited were of much interest. 
Prof. H. N. Moseley exhibited a collection of Pueblo Indian 
pottery, charms, prayer-sticks, &c., from Zini, New Mexico ; 
Gen. Strachey, an instrument for drawing curves of sines adapted 
to graphical representation of the harmonic components of 
periodical phenomena; Mr. W. T. Thiselton Dyer lent some 
beautiful flowering specimens of Himalayan rhododendrons (the 
small, rosy-pink RX. g/aucum and the large, velvety-white #. 
nuttalli), a fruiting branch of coffee, and the various vessels and 
implements used in the collection and preparation of Para india- 
rubber ; iridio-platinum weights, with a density of 21°5660, 
absolutely adjusted, and a piece of platinum wire ‘00075 of an 
inch, prepared by drawing, &c., were exhibited by Mr, G. 
Matthey ; the Linnean Society lent aremarkable set of drawings 
from the collection of Lady Impey, at Calcutta, painted by a 
native of Patna towards the end of the last century, and still in 
perfect preservation ; the Anthropological Institute contributed 
ethnographic photographs of various races; and there were 
many highly interesting philosophical instruments shown. 
THE Council of the British Association have nominated Prof. 
J. Struthers, M.D., as a Vice-President of the Association for 
the Aberdeen meeting, and have added the name of Prof. J. 
Stirling, M.D., D.Sc. (Aberdeen) to the list of those nominated 
for the Vice-Presidency of Section D. 
AT the invitation of Prof. Flower, a meeting of the Essex 
Field Club will be held on Saturday afternoon, May 16, at 3.30, 
in the Lecture Room at the Zoological Gardens, when the Pro- 
fessor will speak of the principal objects of interest in the 
