Editing Orbit (section)

==Scaling in gravity==
The [[gravitational constant]] ''G'' has been calculated as:
* (6.6742 ± 0.001) × 10<sup>−11</sup> (kg/m<sup>3</sup>)<sup>−1</sup>s<sup>−2</sup>.

Thus the constant has dimension density<sup>−1</sup> time<sup>−2</sup>. This corresponds to the following properties.

[[Scale factor|Scaling]] of distances (including sizes of bodies, while keeping the densities the same) gives [[Similarity (geometry)|similar]] orbits without scaling the time: if for example distances are halved, masses are divided by 8, gravitational forces by 16 and gravitational accelerations by 2. Hence velocities are halved and orbital periods and other travel times related to gravity remain the same. For example, when an object is dropped from a tower, the time it takes to fall to the ground remains the same with a scale model of the tower on a scale model of the Earth.

Scaling of distances while keeping the masses the same (in the case of point masses, or by adjusting the densities) gives similar orbits; if distances are multiplied by 4, gravitational forces and accelerations are divided by 16, velocities are halved and orbital periods are multiplied by 8.

When all densities are multiplied by 4, orbits are the same; gravitational forces are multiplied by 16 and accelerations by 4, velocities are doubled and orbital periods are halved.

When all densities are multiplied by 4, and all sizes are halved, orbits are similar; masses are divided by 2, gravitational forces are the same, gravitational accelerations are doubled. Hence velocities are the same and orbital periods are halved.

In all these cases of scaling. if densities are multiplied by 4, times are halved; if velocities are doubled, forces are multiplied by 16.

These properties are illustrated in the formula (derived from the [[Orbital period#Small body orbiting a central body|formula for the orbital period]])

:<math> GT^2 \rho = 3\pi \left( \frac{a}{r} \right)^3, </math>

for an elliptical orbit with [[semi-major axis]] ''a'', of a small body around a spherical body with radius ''r'' and average density ''ρ'', where ''T'' is the orbital period. See also [[Kepler’s third law]].