Between 1609 and 1619, Johannes Kepler formulated three empirical laws based on Tycho Brahe's meticulous observational data of planetary positions:
- First Law (Law of Orbits): Every planet moves in an elliptical orbit around the Sun, with the Sun situated at one of the two focal points of the ellipse.
An ellipse is characterized by its semi-major axis $a$, semi-minor axis $b$, and eccentricity $e = \sqrt{1 - b^2/a^2}$ ($0 \le e < 1$). The closest approach to the Sun is the perihelion at distance $r_p = a(1 - e)$, and the farthest point is the aphelion at distance $r_a = a(1 + e)$.
- Second Law (Law of Areas): The radius vector drawn from the Sun to a planet sweeps out equal areas in equal intervals of time. That is, the areal velocity of a planet is strictly constant:$$\frac{dA}{dt} = \text{constant}$$Proof via Conservation of Angular Momentum: Consider a planet of mass $m$ moving with velocity $\vec{v}$ at position $\vec{r}$ relative to the Sun. In an infinitesimal time $dt$, its displacement is $d\vec{r} = \vec{v}\,dt$. The area swept out is the triangular area $dA = \frac{1}{2}|\vec{r} \times d\vec{r}| = \frac{1}{2}|\vec{r} \times \vec{v}|\,dt$. Thus:$$\frac{dA}{dt} = \frac{1}{2}|\vec{r} \times \vec{v}| = \frac{|\vec{r} \times m\vec{v}|}{2m} = \frac{L}{2m}$$Because the gravitational force exerted by the Sun is purely central (directed along $-\hat{r}$), the net torque is zero: $\vec{\tau} = \vec{r} \times \vec{F}_g = 0$. Therefore, total angular momentum $\vec{L}$ is conserved, proving that $\frac{dA}{dt} = \frac{L}{2m} = \text{constant}$.
A direct consequence is that the planet moves fastest at perihelion and slowest at aphelion: $v_p r_p = v_a r_a$.
- Third Law (Law of Periods): The square of the orbital period of revolution ($T$) of a planet is directly proportional to the cube of the semi-major axis ($a$) of its elliptical orbit:$$T^2 \propto a^3 \implies \frac{T^2}{a^3} = \text{constant}$$
Assuming a planet of mass $m$ moves in a circular orbit of radius $r$ around the Sun of mass $M_s$ with constant speed $v$ and period $T$:
The required centripetal force is $F = \frac{m v^2}{r} = m \left(\frac{2\pi r}{T}\right)^2 \frac{1}{r} = \frac{4\pi^2 m r}{T^2}$.
From Kepler's Third Law, $T^2 = k r^3$. Substituting into the force equation:
$$F = \frac{4\pi^2 m r}{k r^3} = \left(\frac{4\pi^2}{k}\right) \frac{m}{r^2} \implies F \propto \frac{1}{r^2}$$Newton recognized that by his Third Law, the force must also be directly proportional to the mass of the Sun $M_s$, leading directly to the Universal Law of Gravitation: $F = G\frac{M_s m}{r^2}$.