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Saturn from Cassini Astronomy 161:
An Introduction to Solar System Astronomy
Prof. Richard Pogge, MTWThF 9:30

Lecture 21: The Rotation & Revolution of the Earth

Key Ideas:

Demonstrations of the Earth's Rotation about its axis:

Demonstration of the Earth's Revolution around the Sun:

Eppur si muove (?)

Legend has it that Galileo muttered the words "Eppur si muove" (It still moves) under his breathe after abjuring his "errors and heresies" before the Roman Inquisition in thew matter of teaching the forbidden Copernican system.

This story is almost certainly false, but it touches upon the principal objection to the Heliocentric System since the time of Aristotle:

How do you prove that the Earth really does rotate upon its axis and revolve around the Sun?

The Need for Speed

A major conceptual barrier to accepting the rotation and revolution of the Earth is that the speeds required are enormous.
Speed of the Earth's Rotation at the Equator:

Circumference of the Earth at the Equator = 40,000 kilometers
Time to complete one Rotation = 24 hours

Speed of Rotation = Distance/Time = 40,000 km / 24 hr = 1670 km/hr

The speed of revolution around the Sun is even larger:

Speed of the Earth's Revolution around the Sun:

Radius of the Earth's Orbit = 1 AU = 150,000,000 kilometers
Circumference of the Earth's Orbit = 2*pi*R = 942,000,000 kilometers
Time to complete one Orbit = 365.2422 days = 8766 hr

Speed of Revolution = Distance/Time = 942,000,000 km / 8766 hr = 107,000 km/hr = 30 km/sec

In the typical time it takes to read this sentence (about 15 seconds), the Earth will have moved through space by about 450 km, or about the width of the state of Ohio.

Consider that the fastest things people had experienced prior to the invention of steam power moved at speeds of only a few 10s of km/hr (horses, fast ships). Even the fastest winds are only 150 km/hr.

Riding on a Rotating Sphere

As you move north or south of the equator towards the Poles:
  1. East-West parallel of constant latitude narrows.
  2. The distance covered in 24-hours is less, so the speed is less.

The speed of rotation is greatest at the Equator and gets smaller with increasing latitude. For example, at Columbus (Latitude 40-degrees North):

Circumference of the Earth at 40-deg North = 30,600 kilometers
Time to complete one Rotation = 24 hours

Speed of Rotation at 40 North = Distance/Time = 30,600 km / 24 hr = 1280 km/hr

[Note: For the more mathematically inclined, the rotation speed at a given Latitude = cos(Latitude) x 1670 km/hr.]

The Coriolis Effect

First described by French physicist Gustave Coriolis in 1835.

Deflection of a projectile due to the Earth's Rotation:

An example:

Result is a slight eastward deflection of the cannonball from its original northward trajectory. You get the same effect if you fire the cannon towards the South.

The above is a simple illustration of the Coriolis effect. In general, the Coriolis effect works independently of the direction in which the projectile is travelling.

A Little to the Right (or Left)

The result of the Coriolis Effect is: Long-range artillery sights and missile guidance systems are designed to correct for the Coriolis Effect.

Also affects low-pressure systems & storms:

During the First World War, British and German naval forces engaged in a battle off the Falkland Islands in the South Atlantic. Early in the battle, British shells kept falling consistently about 100 meters to the left of the German ships because the gunners neglected to take into account the opposite sign of the Coriolis effect in the Southern hemisphere (most of their experience was in the North), and so were inadvertently correcting for the Coriolis effect in the wrong direction, resulting in twice the deflection if no correction had been made! Eventually this was figured out.

Flushing an Urban Legend

The Coriolis Effect does not cause water to spiral down drains (or toilets) differently in the Northern & Southern Hemispheres.

Try it. Fill a sink with water, set the water it swirling clockwise and then pull the plug. Then do it again, this time swirling it counterclockwise before pulling the plug.

Sorry Bart (the clockwise flush fallacy was the premise of the Bart vs. Australia episode of The Simpsons).

Foucault Pendulum

Built by Jean Foucault in 1851. He suspended a 67-meter long pendulum with a 25-kg weight from the dome of the Pantheon in Paris. A ball joint let the pendulum swing freely in all directions. The steady clockwise shift of the pendulum's swing is being caused by the rotation of the Earth.

The Pole and the Pendulum

The easiest way to see what is going on is to imagine erecting a Foucault Pendulum at the North Pole.

Start the pendulum swinging towards the direction of a particular star (e.g., the bright star Sirius).

An observer on Sirius looking at the pendulum would see:

An observer at the North Pole would see:

What is rotating (the Earth or the Pendulum) depends on your point of view.

At middle latitudes, a Foucault pendulum takes longer than 24 hours to go around once [more exactly, it takes 24hr x sin(latitude), so in Columbus, it takes 37.3 hours. Foucault pendulums don't swing around at the Equator].

If the earth were not rotating, the pendulum would never change the direction of its swing at any latitude above the Equator.

Stellar Parallax

As the Earth revolves around the Sun, it moves 2 AU from one side of its orbit to another in 6 months.

(Click on the image to view at full scale [Size: 7Kb])

Parallaxes were not observed at the time of Copernicus:

Parallax decreases with Distance

As the distance to a star increases, the amount of parallax decreases. This is easy to see in the following two figures:

In the upper figure, the star is about 2.5 times nearer than the star in the lower figure, and has a parallax angle which is 2.5 times larger.

A movie demonstrating parallaxes is available (beware: it is big, don't try to download it over a slow modem link).

Measuring Stellar Parallaxes

Copernicus and others were right: stellar parallaxes were not easily observed because the stars are much more distant than people originally suspected:

The first stellar parallax was observed in 1837 by the astronomer Friedrich Wilhelm Bessel for the star 61 Cygni.

Modern measurements of parallaxes use photography or digital imaging techniques. A new generation of "interferometric" techniques is being developed for upcoming space missions that will be able to measure parallaxes with a precision of 1 microarcsecond.

As you will learn in Astronomy 162, stellar parallaxes provide us with an important method for making direct measurements of the distances to planets and nearby stars.

The revolution of the earth was first demonstrated not by parallaxes but by the discovery of the "aberration of starlight" by the astronomer James Bradley in 1728. Parallaxes, the "final proof", were to be elusive for more than a century, and were one of the chief goals of astronomers in this period.

Cosmic Anticlimax

Firm observational proof of the rotation and revolution of the Earth did not come until more than two centuries after the death of Copernicus.

By then, the use of the telescope and the revolution in thought started by Isaac Newton's formulation of the laws of motion and gravitation had effectively swept away the last vestiges of the Aristotelian view of the world.

Return to [ Unit 4 Index | Astronomy 161 Main Page ]
Updated: 2006 October 14
Copyright Richard W. Pogge, All Rights Reserved.