The subject of the CR3BP is the motion of a very, very small third body in the presence of a pair of bodies in circular orbits about their center of mass. (The more general problem of the elliptical restricted 3 body problem is a much tougher nut to crack.) Of the two massive bodies, one will be more massive than the other. This larger body is called the primary body, the smaller one, the secondary body. Restricting the third body to having a mass that is many, many orders of magnitude smaller than that of the secondary means that the effect of the third body on the behaviors of the primary and secondary bodies will be negligible and can be ignored.
Those equations of motion are not expressed in SI units. They are instead expressed in units such that
- One mass unit is the sum of the masses of the primary and secondary bodies. In these units, the secondary body has mass μ; the primary body has mass 1-μ. The primary is by definition the more massive of the two bodies, meaning that μ is between 0 and 1/2.
- One distance unit is the distance between the primary and secondary bodies. This distance is constant since the primary and secondary a two bodies are in circular orbits about one another.
- One time unit is the orbital period the primary and secondary bodies divided by (2*pi).
Note that, by definition, this system of units yields numeric values of one for the total mass of the system and for the orbital radius. A couple of other key quantities also have a numeric value of one in this system of units. These are the universal gravitational constant G and the magnitude of the primary and secondary's angular velocity vector ω.