But the seasons of Venus present the greatest anomaly, if its assigned inclination of axis (75 deg.) can be relied on as correct, which is doubtful.  Its tropic zone extends nearly to the pole, and at the same time the winter at the other pole reaches the equator.  The short period of this planet causes it to present the south pole to the sun only one hundred and twelve days after it has been scorching the one at the north.  This gives two winters, springs, summers, and autumns to the equator in two hundred and twenty-five days.

If each whirling world should leave behind it a trail of light to mark its orbit, and our perceptions of form were sufficiently acute, we should see that these curves of light are not exact circles, but a little flattened into an ellipse, with the sun always in one of the foci.  Hence each planet is nearer to the sun at one part of its orbit than another; that point is called the perihelion, and the farthest point aphelion.  This eccentricity of orbit, or distance of the sun from the centre, is very small. [Page 106] In the case of Venus it is only .007 of the whole, and in no instance is it more than .2, viz., that of Mercury.  This makes the sun appear twice as large, bright, and hot as seen and felt on Mercury at its perihelion than at its aphelion.  The earth is 3,236,000 miles nearer to the sun in our winter than summer.  Hence the summer in the southern hemisphere is more intolerable than in the northern.  But this eccentricity is steadily diminishing at a uniform rate, by reason of the perturbing influence of the other planets.  In the case of some other planets it is steadily increasing, and, if it were to go on a sufficient time, might cause frightful extremes of temperature; but Lalande has shown that there are limits at which it is said, “Thus far shalt thou go, and no farther.”  Then a compensative diminution will follow.

Conceive a large globe, to represent the sun, floating in a round pond.  The axis will be inclined 7-1/2 deg. to the surface of the water, one side of the equator be 7-1/2 deg. below the surface, and the other side the same distance above.  Let the half-submerged earth sail around the sun in an appropriate orbit.  The surface of the water will be the plane of the orbit, and the water that reaches out to the shore, where the stars would be set, will be the plane of the ecliptic.  It is the plane of the earth’s orbit extended to the stars.

The orbits of all the planets do not lie in the same plane, but are differently inclined to the plane of the ecliptic, or the plane of the earth’s orbit.  Going out from the sun’s equator, so as to see all the orbits of the planets on the edge, we should see them inclined to that of the earth, as in Fig. 40.

[Illustration:  Fig. 40.—­Inclination of the Planes of Orbits.]

If the earth, and Saturn, and Pallas were lying in [Page 107] the same direction from the sun, and the outer bodies were to start in a direct line for the sun, they would not collide with the earth on their way; but Saturn would pass 4,000,000 and Pallas 50,000,000 miles over our heads.  From this same cause we do not see Venus and Mercury make a transit across the disk of the sun at every revolution.