Western Washington University   College of Sciences and Technology   Physics/Astronomy Dept.   Bellingham, WA USA
 
ASTRO 101

Analemma
Asteroids
Aurora
Big Bang
Black Holes
Bode Titius
Brightest Stars
Comets
Constellations
Coordinates
Cosmology
Cruithne
Dark Matter
Eclipses
Galaxies
Historical
HR Diagram
Hubble's Law
Intelligent Life
Kepler's Laws
Leap Year
Light Waves
Lunar Libration
Messier Objects
Meteors
Milky Way
Moon
Moon Phases
Planets
Precession
Rainbows
Redshift
Seasons
Stellar Evolution
Stardust
Sun & Fusion
Telescopes
Tides
Time of Day
Twilight
Zodiac
 
Kepler's Three Laws of Planetary Motion

Johannes Kepler 1571-1630
Johannes Kepler 1571-1630

Johannes Kepler was born poor and sickly in what is now Germany. His father left home when Johannes was five and never returned. It is believed he was killed in a war. While Johannes was pursuing higher education his mother was tried as a witch. Johannes hired a legal team which was able to obtain her release, mostly on legal technicalities.

Although he had an eventful life, Kepler is most remembered for "cracking the code" that describes the orbits of the planets.

Prior to Kepler's discoveries, the predominate theory of the solar system was an Earth-centered geometry as described by Ptolemy. A Sun-centered theory had been proposed by Copernicus, but its predictions were plagued with inaccuracies.

Working in Prague at the Royal Observatory of Denmark, Kepler succeeded by using the notes of his predecessor, Tycho Brahe, which recorded the precise position of Mars relative to the Sun and Earth.

Kepler developed his laws empirically from observation, as opposed to deriving them from some fundamental theoretical principles. About 30 years after Kepler died, Isaac Newton was able to derive Kepler's Laws from basic laws of gravity.



Law 1. The orbits of the planets are ellipses, with the Sun at one focus.

Any ellipse has two geometrical points called the foci (focus for singular). There is no physical significance of the focus without the Sun but it does have mathematical significance. The total distance from a planet to each of the foci added together is always the same regardless of where the planet is in its orbit.

The importance of this is that by not assuming the orbits are perfect circles, the accuracy of predictions in the Sun-centered theory was (for the first time) greater than those of the Earth-centered theory.



Law 2. The line joining a planet to the Sun sweeps out equal areas in equal times as the planet travels around the ellipse.

In any given amount of time, 30 days for instance, the planet sweeps out the same amount of area regardless of which 30 day period you choose. Therefore the planet moves faster when it is nearer the Sun and slower when it is farther from the Sun. A planet moves with constantly changing speed as it moves about its orbit. The fastest a planet moves is at perihelion (closest) and the slowest is at aphelion (farthest).



Law 3. The square of the total time period (T) of the orbit is proportional to the cube of the average distance of the planet to the Sun (R).

This law is sometimes referred to as the law of harmonies. It compares the orbital time period and radius of an orbit of any planet, to those of the other planets. The discovery Kepler made is that the ratio of the squares of the revolutionary time periods to the cubes of the average distances from the Sun, is the same for every planet.

The Marvelous Lantern
Johannes Kepler found a marvelous way out of his dilemma, how to ascertain the real shape of Earth’s orbit. Imagine a brightly shining lantern somewhere in the plane of the orbit. Assume we know that this lantern remains permanently in its place and thus forms a kind of fixed triangulation point for determining the Earth’s orbit, a point which the inhabitants of Earth can take a sight on at any time of year. Let this lantern be further away from the Sun than the Earth. With the help of such a lantern it is possible to determine the Earth’s orbit in the following way. First of all, in every year there comes a moment when the Earth (E) lies exactly on the line joining the Sun (S) and the Marvelous Lantern (M). If at this moment we look from the Earth (E) at the Lantern (M) our line of sight will coincide with the line Sun-Lantern (SM). Suppose the line to be marked in the heavens. Now imagine the Earth in a different position and at a different time. Since the Sun (S) and the Lantern (M) can both be seen from the Earth, the angle at E in the triangle SEM is known. We might do this at frequent intervals during the year, each time we should get on our piece of paper a position of the Earth with a date attached to it and a certain position in relation to the permanently fixed base SM. The Earth’s orbit could thereby be determined. But, you will say, where did Kepler get his lantern? His genius and nature gave it to him. There was the planet Mars, and the length of the Martian year was known.
Albert Einstein on the occasion of the three hundredth anniversary of Kepler’s death – November 9, 1930.