Wolfram Demonstrations Project

Kepler's laws of planetary motion in the 17th century superseded the Ptolemaic system of epicycles to account for the detailed motions of the planets. Generalizations of epicycloids, called epitroichoids, still do occur, however, in the description of relative planet-moon motions as their barycenters (centers of gravity) follow Keplerian orbits around the Sun.

We consider a simplified idealized case, which is justified in the Details: a moon (red point

) with mass

is in a circular orbit about its planet (blue point

) with mass

, with the moon-planet distance equal to

, where

and

are the respective distances of the moon and planet from their barycenter. The barycenter of this pair is in a circular orbit of radius

about the Sun. With the Sun at the origin, the parametric equations for

and

can be written

where

equals the number of lunar cycles per revolution about the Sun. (For the Sun-Earth-Moon system,

.) These represent parametric equations for epitroichoids, which reduce to the more familiar epicycloids when

and

in the first and second set of equations, respectively. In most cases these curves exhibit a looped or cuspoid structure as they traverse the larger circle. All rotations and revolutions shown are counterclockwise.

This brings us to the remarkable fact that the Moon's orbit around the Sun is a convex curve. This can be explained by the following physical argument. The gravitational force of the Sun on the Moon is always more than twice the gravitational force of the Earth on the Moon:

. Thus the net force on the Moon is always directed toward the Sun. But, by Newton's second law, this force is proportional to the second derivative of

with respect to time, hence the radial curvature of the orbit is always positive. This implies that the Moon’s orbit is always convex with respect to the Sun. In terms of the epitrochoid parameters, the condition for convexity can be expressed as

, which is easily fulfilled for the Sun and Moon. Remarkably, no other known planet-moon couple in the Solar System obeys the convexity condition.

Contributed by: S. M. Blinder

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The three-body Sun-Earth-Moon problem can be described by the Lagrangian

where the Sun is taken as the origin of the coordinate system and is thus considered stationary. Here

represents the gravitational constant,

the solar mass,

the lunar (or other moon) mass,

the Earth (or other planetary mass), and

the three interbody distances. Because of the great disparity in masses and in distances, an accurate simplification of the problem is possible. For the Sun-Earth-Moon system,

, and

. The Lagrangian is well approximated by

]

where

is the distance from the Sun to the Earth-Moon barycenter (

) and

. The simplest case is when both orbital motions are circular, with angular velocities

("annual") and

("monthly"). To a fair approximation, there are 13 lunar months per solar year:

The thumbnail graphic for this Demonstration shows epichoroidal orbits for a hypothetical twin planet around some other star, in which a planet and its moon are of equal mass.

Snapshot 1: a qualitative representation for a planet with a very massive moon; for example Pluto's moon Charon has approximately 11.6% of the mass of the planet

Snapshot 2: the Sun-Earth-Moon system drawn to scale, with

(average Sun-Earth distance is about 400 times average Earth-Moon distance) and

(lunar months per year); with higher magnification, it can be seen that the Moon's orbit around the Sun is a distorted 13-sided polygon that is a convex figure