more athwart that line, and as this occurs the spectral
lines will gradually assume their normal position and appear single.
This is the sequence of phenomena in beta Aurigae. And the same sequence
is found in Capella and in several other more or less conspicuous stars
in various parts of the heavens.

Such facts, like those connecting rows and groups of stars with masses
and spiral lines of nebula are obscure signboards, indicating the
opening of a way which, starting in an unexpected direction, leads deep
into the mysteries of the universe.

Southward from beta we find the star theta, which is a beautiful
quadruple. We shall do best with our five-inch here, although in a fine
condition of the atmosphere the four-inch might suffice. The primary is
of the third magnitude; the first companion is of magnitude seven and a
half, distance 2", p. 5 deg.; the second, of the tenth magnitude, distance
45", p. 292 deg.; and the third, of the tenth magnitude, distance 125", p.
350 deg..

We should look at the double Sigma 616 with one of our larger apertures
in order to determine for ourselves what the colors of the components
are. There is considerable diversity of opinion on this point. Some say
the larger star is pale red and the smaller light blue; others consider
the color of the larger star to be greenish, and some have even called
it white. The magnitudes are five and nine, distance 6", p. 350 deg..

Auriga contains several noteworthy clusters which will be found on the
map. The most beautiful of these is 1295, in which about five hundred
stars have been counted.

The position of the new star of 1892, known as Nova Aurigae, is also
indicated on the map. While this never made a brilliant appearance, it
gave rise to a greater variety of speculative theories than any previous
phenomenon of the kind. Although not recognized until January 24, 1892,
this star, as photographic records prove, was in existence on December
9, 1891. At its brightest it barely exceeded magnitude four and a half,
and its maximum occurred within ten days after its first recognition.
When discovered it was of the fifth magnitude. It was last seen in its
original form with the Lick telescope on April 26th, when it had sunk to
the lowest limit of visibility. To everybody's astonishment it
reappeared in the following August, and on the 17th of that month was
seen shining with the light of a tenth-magnitude star, _but presenting
the spectrum of a nebula