Between 1609 and 1619, Johannes Kepler published his planetary laws of motion. This was based on the data he received from his mentor, Tycho Brahe. As he studied the data he discovered that the planets revolved around the sun, not in circular orbits as many believed, but in elliptical orbits. He also noted that the speed at which the planets moved varied depending on the distance away from the sun.
As a result, in his publication, he developed three laws that describe the behaviour of planets.
Video
Now watch the video on Kepler's Laws. The first 5 mins or so lay the historical background. If you wish to go straight to the three laws, scroll to 5:38
Now watch the video on Kepler's Laws. The first 5 mins or so lay the historical background. If you wish to go straight to the three laws, scroll to 5:38
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Interactive
We will start by looking at some animations that demonstrate what these three laws are about.
We will start by looking at some animations that demonstrate what these three laws are about.
Sample Problem
We are now ready to try a sample problem
Below is a sample problem with a video that explain how to solve it. It is suggested you try the problem beforehand, as this actually aids understanding, even if you are unsure if you are correct.
We are now ready to try a sample problem
Below is a sample problem with a video that explain how to solve it. It is suggested you try the problem beforehand, as this actually aids understanding, even if you are unsure if you are correct.
- Click on the First Law and press PLAY
The first law states that planets move in elliptical orbits
Ellipses are shapes that have two foci (click FOCI) and have an associated eccentricity
Eccentricity is a measure of how elliptical it is, and the greater the eccentricity (closer to 1) the more eccentric it is
(Perfect circles have an eccentricity of 0)
The Sun, in this case is at one of the foci - Click on the Second Law and press PLAY
In essence Kepler's second law states that a satellite sweeps out equal areas in the same time frame. The result is that the satellite moves faster when closer to the central body, and slower when further away.