rs the orbit will be very nearly a circle.

Now, from what was stated in Art. 106, we know that the moon's orbit
will be nearly a circular orbit when the earth is farthest from the sun,
and that then its orbital velocity is at a minimum.

In order for this result to be produced, the earth must reach that part
of its orbit known as aphelion, where the distance from its controlling
centre is greatest, so that the eccentricity of the moon's orbit is
always an indication of the position of the earth in its relation to the
sun. When the eccentricity of the moon's orbit is decreasing, the
earth's distance from the sun is increasing, but when the eccentricity
of the moon's orbit is increasing, then the earth's distance from the
sun is decreasing.

Now if we apply this analogy to the eccentricity of the earth's orbit,
we shall be able to obtain some idea of the relation of the sun to its
central body. We find then that the eccentricity of the earth's orbit is
decreasing, therefore, arguing from analogy, we arrive at the conclusion
that the sun's distance from its controlling centre is increasing, and
that its orbital velocity is decreasing.

If it be true that in 24,000 years the earth's orbit will be nearly
circular, then it follows that in 24,000 years the sun will be at that
part of its orbit corresponding to the aphelion of the orbit of the
earth, that is, its distance from its controlling centre will then be at
a maximum. After that the eccentricity of the earth's orbit will begin
to increase, and will continue to increase for about 40,000 years,
according to some scientists, which implies that the sun will then have
started from its aphelion point, so to speak, and will begin its return
journey towards its central body, gradually getting nearer and nearer.
As it gets nearer its orbital velocity will be proportionately
increased, with the result that the eccentricity of the earth's orbit
will increase also. From a consideration of the movement of the major
axis of the earth's orbit, which is moving forward at the rate of
11 deg. per year, we are told that a whole revolution will be made in
108,000 years.

We have here, then, an indication of the time that the sun takes to
revolve round its central body, because the time of the whole revolution
of the eccentricity of the orbit should correspond with one complete
revolution of the sun around its central body. So that from a
consideration of the eccentricity of the earth