#5.4.3a
Kepler’s three laws of planetary motion
#5.4.3b
the centripetal force on a planet is provided by the gravitational force between it and the Sun
#5.4.3c
the equation \(T^2 = \bigg(\dfrac{4π^2}{GM}\bigg)r^3 \)
Learners will also be expected to derive this equation from first principles.
#5.4.3d
the relationship for Kepler’s third law \(T^2 ∝ r^3 \) applied to systems other than our solar system
#5.4.3e
geostationary orbit; uses of geostationary satellites.