. 
NATGR LE 
465 
THURSDAY, SEPTEMBER 1885 
17, 
THE NEW STAR IN ANDROMEDA 
E have received the following important communi- 
cations from Lord Rosse and Dr. Huggins 
relating to the new star. Whether the star be connected 
with the nebula or not, during the last week evidence has 
been brought forward that it has changed both its 
brilliancy and position with regard to the nucleus. This 
question of change of position is of the highest import- 
ance, for arguments were advanced in this journal 
(NATURE, vol. xvi. p. 413) on the occasion of the out- 
burst of the stella nova in 1866, which suggested that a body 
which reduced its lustre so rapidly could have no very great 
“mass, and that therefore it might not be so very remote. 
Dr. Huggins is able to decide between the different 
statements which have been publishedas to the spectrum 
of the star: he has little doubt as to the existence of 
bright lines between D and % This endorses Lord 
Rosse’s observation which we printed last week. 
SINCE my communication of September 8 our books have 
been searched for information on the past history of the nucleus 
of the Andromeda nebula. I subjoin in full the entries bearing 
upon the question whether the ‘‘new star” is now seen for the 
first time, or is a variable now shining out with abnormal 
brilliancy. The latter would appear to be the case. The nebula 
was frequently observed in past years with the 6-foot reflector 
and measures made. These measures being too few in number 
for a proper survey of the nebula, publication was postponed in 
1878, and the details of configuration of the nebulosity have not 
appeared such as to merit a monograph. ROSsE 
September 12 
The Great Nebulain Andromeda as observed at Birr Castle with 
the 6-foot Reflector 
1848, December 13.—Three new stars seen near nucleus. 
Others stars at moments suspected in large nucleus. 
1848, December 15.—Confirmed previous night’s observations 
about the three stars 7 2 fof nucleus. 
1851, October 25.—[On a rough sketch accompanying micro- 
metrical measurements the nucleus is indicated by a point]. 
1852, September 16.—Nucleus looked very sharp. Had sus- 
picion of a point in centre of nucleus of large nebula which 
formed one angle of a quadrilateral of which the other three are 
small stars to the left. 
1855, October 15.—With higher power several stars become 
visible about the nucleus. Nucleus itself suspected at moments 
to be resolvable. 
1856, October 28.—I observed the nucleus attentively for a 
long time, and I thought I could at times see stars along its 
north edge, but I am not very confident about it. 
1857, October 16.—The higher power of single lens brings 
out a great many very faint stars around the nucleus. a seen 
steadily, 8 seen by glimpses and I suspect a star in the neigh- 
bourhood of y. 
The sketch represents the central portion of the 
nebula. 
[A point is indicated in the centre of the nucleus. ] 
VoL. Xxx11.—No. 829 
1860, October 19.—I 
accompanying sketch. 
think the nucleus is extended as in 
1860, November 13.—[A sketch was carefully made, which is 
almost identical with the sketch of 1860, October 19, showing 
the extension of the nucleus very plainly. No point is indicated 
in the centre of the nucleus. ] 
[In 1861 and 1862 numerous micrometrical measures were 
taken, accompanied by rough sketches, showing the nucleus as a 
diffused nebulous patch, either round or slightly extended as on 
1860, October 19. ] 
1871, October 7.—A rough sketch was made [showing the 
nucleus round and rather distinct. ] 
1872, August 7.—Nucleus very distinct on ground of nebula. 
1877, November 2.—Nucleus extends in same direction as 
nebula ; immediately following the nucleus the nebulosity de- 
creases quickly in brightness, more so than on preceding side. 
THE star was observed here first on the night of the 3rd inst. 
It presented the appearance of an orange-coloured star of from 
the 8th to the 9th magnitude. With a spectroscope of low 
dispersive power a continuous spectrum was seen from about 
C in the red to a little beyond F. There was an apparent con- 
densation of light from about D to 4, which might be due to 
bright lines in that part of the spectrum. This supposition was 
strengthened by the employment of a more powerful spectroscope, 
but I was not able to be certain on this point. 
On the oth the star, which was then distinctly on one side of 
the principal point of condensation in the nebula, appeared to 
me to have a less decided orange tint. It presented an appear- 
ance in the spectroscope similar to that which it had on the 3rd, 
with the exception that the light was less strong about D. I 
was so far confirmed in my suspicion of bright lines that I have 
little doubt that from three to five bright lines were present 
between D and 4. 
On the 3rd inst. the star did not appear clearly defined in 
the refractor of 15 inches aperture, but the state of the sky was 
not good enough to enable me to be sure that the star was truly 
nebulous. On the oth the star was certainly free from 
nebulosity. WILLIAM HuGGINS 
Upper Tulse Hill, S.W. 
On September 8 the new star in the nebula (Messier 31) in 
Andromeda was examined in my Io-inch reflector. The nova 
shines with a yellowish tint and looks like an ordinary star 
of about 7} mag., being a perfectly sharp and well-defined 
x 
