Explanation

Kepler's Third Law of Planetary Motion states:

T² = (4π²/G * (M₁ + M₂)) * a³

Where:

T = Orbital Period

a = Semi-major Axis

G = Gravitational Constant

M₁ and M₂ = Masses of the two bodies (e.g., planet and star)

This law shows that the square of the orbital period (T) is proportional to the cube of the semi-major axis (a).