REPORTS FROM THE SECTIONS. 231 
giving a difference of 166 millions of miles. This difference cer- 
ble part of its orbit for telescopic observation, and this favourable 
combination of circumstances will increase till 1882, after which it 
inish. 
Another result of the conditions I have thuspointed out is the fact 
that the planet is becoming more distinct to the naked eye at each 
successive opposition. It can, even now that several weeks have 
elapsed since its re dea be distinctly seen without a telescope. 
At the ap reant Sane ab > early on the same meridian of righ 
ascensio 1 
of that Mais Bowe stars ieee embraced within the field of the 
of v Leonis, so that Urarius may ai be Sokided as a ae 
star of the sixth magnitude. My attention was not directed to 
the planet at the time of its maximum brilliancy in February last. 
In February, 1869, I observed the planet on the meridian with 
the transit instrument, and found it to be very nearly fifteen seconds 
of time west of the place assigned to it by the old Tables of Bouvard, 
which have been employed in the computations of the Nautical 
nac down to the end of 1876. Observations taken last even- 
ing, however, showed it to be almost t precisely in the place deduced 
from Professor Newcomb’s new Tables since employed for the 
Toles meris in the Nautical Almanac. 
Observatory, Windsor, 25 Ape 1878. 
