248 NEW STARS IN ANDROMEDA AND ORION. 
method has been found to yield satisfactory determina- 
tions even when bearing comparison with the more exact 
instrumental methods, such as by wedge photometer and 
meridian photometer. During the period of my ob- 
servation the Andromeda star fell with considerable 
regularity from the 8.4 to the 9.6 magnitude. On com- 
paring my estimates with those published in the Astvo- 
nomical Nachrichten, 1 found I had placed the magni- 
tude somewhat larger throughout. This arose, doubt- 
less, from my fear lest I should underrate it on account 
of its nebulous surrounding. It was noticed at Dum 
Echt that low powers showed the star relatively brighter 
than the large telescope, probably because low powers 
did not separate the star altogether from the surround- 
ing nebulosity. 
A few observers believed that they perceived a 
noticeable diminution of the brightness of the nebula 
during the maximum of the Nova, among them Hart- 
wig. The majority of astronomers, however, do not 
agree with his conclusion. They attribute any sup- 
posed change in brightness and extension to the un- 
usual illumination produced by the new star. 
On December 13, 1885, Mr. Gore, of Beltra, Ireland, 
observed a star of about the sixth magnitude following 
xX’ Orionts by 1" 25° and about 6” north or ieee 
Orionis is a fifth magnitude star in the club of Orion. 
He could not find it in any of the catalogues and sus- 
pected it to be a temporary. It was soon acknowledged 
by all astronomers to be a new body. It lost light from 
the time of its discovery and early in July, 1886, it be- 
came invisible even in telescopes of moderate size. But 
in August it again became visible and increased slowly 
in brilliancy. 
This speedy return to visibility and continuous varia- 
bility indicate that the star is not a temporary, but a 
hitherto unknown variable. Its maximum magnitude 
1382 
