Updated 2019-09-09
Kepler’s three laws are descriptions based on physical observations and can be used to predict.
Planets travel on elliptical orbits around the sun, where the sun is located at one focus of the ellipse.
A line connecting a planet to the sun sweeps out equal area in equal time interval, regardless of planet’s position. Thus the second law also implies that planet’s orbital speed depends on its location.
The harmonic law is given by: Where $P$ is the orbit period of the planet in years, and $a$ is the average distance / average orbital altitude of the planet from the sun measured in astronomical unit (AU).
In cartesian, the ellipse is given by: An eclipse is also defined by a set of points that satisfies the equation
If $r=r’$, then using Pythagorean theorem, we can derive:
The area of the ellipse is:
The polar equation of ellipse centered around one of the focus given by: When $e$ is in between 0 and 1, we use the above definition as it makes an ellipse. But an ellipse is one of the conic sections. For different ranges of $e$, we may get a parabola or hyperbola.
The elliptical motion of planets follow Newton’s law of motion and gravity.
Recall the ellipse in polar coordinates centered around one focus is
This describes the following ellipse:
When $\theta=0$, the planet is at its perihelion. The orbiting “altitude” $q$ is:
When $\theta=\pi$, the planet is at is aphelion. The orbiting altitude $Q$ is:
The ellipse may be slanted from our point of reference (x-y grid). The slant is described by longitutde of perihelion or $\omega$. The angle $\theta^\star$ is still in reference to the x-axis. The modified polar equation becomes:
The velocity and radius are inversely proportional due to conservation of angular momentum.
Let the area $A$ be the area of the large white triangle. The change in area is
Example: Kepler’s 2nd law using calculus
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Start at $\vec r$ and go a short timestep $\Delta t$ into the future. Then as $\Delta t\rarr 0$ ,the area of the blue triangle approaches 0. The blue triangle area is given by the vertical and horizontal position differences: $v_t\Delta t\times v_r \Delta t \over 2$.
The area of the main triangle is basically: As $\Delta t$ approaches 0, then we have $\frac{dA}{dt}=\frac12 r v_t=\frac{1}{2}rv$ which equals some constant (that’s Kepler’s 2nd law).
Therefore $v$ is proportional to the inverse of the orbit altitude ($\frac{1}{r}$). AKA the planet speeds up at perihelion.
Notice the relationship of $rv=C$ where $C$ is a constant is the conservation of angular momentum. Therefore the angular momentum is constant.
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Example: in polar
The arclength $s$ is just $s=r\theta$ for $\theta$ in radians. Then the velocity $v_t=r\dot{\theta}$, where $\dot\theta=\frac{\mathrm d\theta}{\mathrm d t}$.
$r^2\dot \theta = \frac L M $ is a conserved quantity. This is from $\frac{\mathrm dA}{\mathrm dt}=\frac12 (r)(r\dot\theta)$.
Finding an expression for $\theta$?
Kepler figured it out (Kepler’s method):
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It turns out we can write:
where $e$ is eccentricity. We get this from $r_x=ae-a\cos E$ and $r_y=b \sin E$ (using small dashed circle).
We also find that: