Figure 2

　　The following figure shows the amount of influence the movement of the gravitational field of each celestial body exerts on the origin. The table shows the calculation formulae for this example. On the right, the compositions of υ₁, υ₂ and υ₃ are shown in expanded form.

Figure 3

 
　　The strength of exertion from the gravitational field generated by mass point m₃ (at a distance of 7r₁ from the origin) on the origin would be, from Newton’s law of universal gravitation, 1/(7r₁)² compared with that of m₁. If the mass of m₃ is four times that of m₁, then the influence that speed V₃ exerts on the origin would be V₃ × 4 m₁/(7r₁)². This value is υ_3.
　　Now consider how this compares, as a ratio, to the gravitational movement of m₁. First, the effect that the speed of m₁ has on the origin is similarly calculated as υ₁ = V₁ × m₁ / r₁².
　　If the earlier speed V₃ is five times that of V₁ (V₁ is the speed of m₁), then υ_３ can be expressed as follows:
　　υ₃ = 5V₁ × 4m₁ / (7r₁)².