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The Extinction of Total Solar Eclipses

Adapted from Chapter 13 of Totality - Eclipses of the Sun (2nd Ed.)

Copyright ©1999 by Mark Littmann, Ken Willcox and Fred Espenak

In 1695, Edmond Halley discovered that eclipses recorded in ancient history did not match calculations for the times or places of those eclipses. Starting with records of eclipses in his day and the observed motion of the Moon and Sun, he used Isaac Newton's new theory of universal gravitation (1687) to calculate when and where ancient should have occurred and compared them with eclipses actually observed more than 2,000 years earlier. They did not match. Halley had great confidence in the theory of gravitation and resisted the temptation to conclude that the force of gravity changed as time passed. Instead, he proposed that the length of a day on Earth must have increased by a small amount.

If the Earth's rotation had slowed down slightly, the Moon must have gained the angular momentum to conserve the total angular momentum of the Earth-Moon system. This boost in angular momentum for the Moon would have caused it to spiral slowly outward from the Earth to a more distant orbit where it travels more slowly. If, 2,000 years earlier, the Earth had been spinning a little faster and the Moon had been a little closer and orbiting a little faster, then eclipse theory and observation would match. Scientists soon realized that Halley was right.

But what would cause the Earth's spin to slow? Tides. The gravitational attraction of the Moon is the principal cause of the ocean tides on Earth. As the shallow continental shelves (primarily in the Bering Sea) collide with high tides, the Earth's rotation is retarded. The slower spin of the Earth causes the Moon to edge farther from our planet.

From 1969 to 1972, the Apollo astronauts left a series of laser reflectors on the Moon's surface. Since then, scientists on Earth have been bouncing powerful lasers off these reflectors. By timing the round trip of each laser pulse, the Moon's distance can be measured to an accuracy of several inches. The Moon is receding from the Earth at the rate of about 1.5 inches (3.8 centimeters) a year.

As the Moon recedes from Earth, its apparent disk becomes smaller. Total eclipses become rarer; annular eclipses more frequent. Total eclipses are moving toward extinction. When the Moon's mean distance from the Earth has increased by 14,550 miles (23,410 kilometers), the Moon's apparent disk will be too small to cover the entire Sun, even when the Moon's elliptical orbit carries it closest to Earth. Total eclipses will no longer be possible.

How long will that take? With the Moon receding at 1.5 inches a year, the last total solar eclipse visible from the surface of the Earth will take place 620 million years from now. There is still time to catch one of these majestic events!

For more information, see:

Totality - Eclipses of the Sun

Second Edition
by Mark Littmann, Ken Willcox and Fred Espenak

Order Totality from

Copyright ©1999 by Mark Littmann, Ken Willcox and Fred Espenak

All rights reserved. This material may not be reproduced, published, copied or transmitted in any form, including electronically on the Internet or World Wide Web, without written permission of the authors.

Contact Espenak (at MrEclipse) for more information.

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Last revised: 2008 Jan 22