The star [alpha] (_Betelgeuse_) is an interesting object, on account of
its colour and brilliance, and as one of the most remarkable variables
in the heavens. It was first observed to be variable by Sir John
Herschel in 1836. At this period its variations were "most marked and
striking." This continued until 1840, when the changes became "much less
conspicuous. In January, 1849, they had recommenced, and on December
5th, 1852, Mr. Fletcher observed [alpha] Orionis brighter than Capella,
and actually the largest star in the northern hemisphere." That a star
so conspicuous, and presumably so large, should present such remarkable
variations, is a circumstance which adds an additional interest to the
results which have rewarded the spectrum-analysis of this star by Mr.
Huggins and Professor Miller. It appears that there is decisive evidence
of the presence in this luminary of many elements known to exist in our
own sun; amongst others are found sodium, magnesium, calcium, iron, and
bismuth. Hydrogen appears to be absent, or, more correctly, there are no
lines in the star's spectrum corresponding to those of hydrogen in the
solar spectrum. Secchi considers that there is evidence of an actual
change in the spectrum of the star, an opinion in which Mr. Huggins does
not coincide. In the telescope Betelgeuse appears as "a rich and
brilliant gem," says Lassell, "a rich topaz, in hue and brilliancy
differing from any that I have seen."

Turn next to [beta] (Rigel), the brightest star below the belt. This is
a very noted double, and will severely test our observer's telescope, if
small. The components are well separated (see Plate 3), compared with
many easier doubles; the secondary is also of the seventh magnitude, so
that neither as respects closeness nor smallness of the secondary, is
Rigel a difficult object. It is the combination of the two features
which makes it a test-object. Kitchener says a 1-3/4-inch object-glass