What Are Solar Eclipses?
A solar eclipse is a spectacular sight and a rare astronomical event. Each one is only visible from a limited area.
Rare Solstice Annular Solar Eclipse
In 2020, many locations saw a rare solstice annular solar eclipse on the same day as the June solstice. This will happen only once again this century: on June 21, 2039.
The Moon Eclipses the Sun
An eclipse of the Sun happens when the New Moon moves between the Sun and Earth, blocking out the Sun’s rays and casting a shadow on parts of Earth.
The Moon’s shadow is not big enough to engulf the entire planet, so the shadow is always limited to a certain area (see map illustrations below). This area changes during the course of the eclipse because the Moon and Earth are in constant motion: Earth continuously rotates around its axis while it orbits the Sun, and the Moon orbits Earth. This is why solar eclipses seem to travel from one place to another
Types of Solar Eclipses
There are 4 different types of solar eclipses. How much of the Sun’s disk is eclipsed, the eclipse magnitude, depends on which part of the Moon’s shadow falls on Earth.
- Partial solar eclipses occur when the Moon only partially obscures the Sun’s disk and casts only its penumbra on Earth.
- Annular solar eclipses take place when the Moon’s disk is not big enough to cover the entire disk of the Sun, and the Sun’s outer edges remain visible to form a ring of fire in the sky. An annular eclipse of the Sun takes place when the Moon is near apogee, and the Moon’s antumbra falls on Earth.
- Total solar eclipses happen when the Moon completely covers the Sun, and it can only take place when the Moon is near perigee, the point of the Moon’s orbit closest to Earth. You can only see a total solar eclipse if you’re in the path where the Moon casts its darkest shadow, the umbra.
- Hybrid Solar Eclipses, also known as annular-total eclipses, are the rarest type. They occur when the same eclipse changes from an annular to a total solar eclipse, and/or vice versa, along the eclipse’s path.
Solar Eclipses Mainly Look Partial
Solar eclipses are only visible from within the area on Earth where the Moon’s shadow falls, and the closer you are to the center of the shadow’s path, the bigger the eclipse looks.
Solar eclipses are usually named for their darkest, or maximum, point. The exception is the hybrid eclipse.
The darkest point of solar eclipses is only visible from a small area. In most places and for most of the duration, total, annular, and hybrid eclipses look like a partial solar eclipse.
Only around New Moon
For a solar eclipse to take place, the Sun, the Moon, and Earth must be aligned in a perfect or near perfect straight line. This happens around New Moon every lunar month.
A rough alignment of the three planetary bodies happens every lunar month, at the New Moon. So, why isn’t there a solar eclipse every New Moon?
The plane of the Moon’s path around the Earth is inclined at an angle of approximately 5° to Earth’s orbital plane around the Sun—the ecliptic. The points where the plane of the Moon’s orbital path meets the ecliptic are called lunar nodes.
A perfect or near-perfect alignment of the Sun, the Moon, and the Earth can only take place when the New Moon is near a lunar node. This can only happen during periods that come a little less than 6 months apart, and last, on average, around 34.5 days. It is only during this time, also known as the eclipse season, that eclipses can occur.
When there is a Full Moon during the eclipse season, we see a lunar eclipse.
How & Why Solar Eclipses Happen
There’s nothing wrong with the above definition of an eclipse, but it doesn’t begin to convey the thrill and excitement that takes hold of eclipse chasers when the Moon encroaches upon the Sun.
What’s more, a total solar eclipse is a rare event, cosmically speaking. There are close to 200 confirmed moons orbiting six major planets in our solar system (Mercury and Venus lack moons). But in only one instance is there a moon that’s the right size, and at the right distance from its planet, to just barely cover the brilliant solar disk and reveal the Sun’s wispy corona. And that’s our Moon. (Looked at another way, total solar eclipses aren’t rare; they occur roughly once every year or two somewhere on Earth. But any given spot on our planet’s surface gets darkened by the Moon’s shadow on average only once about every 400 years, so in that sense totality is indeed rare.)
The Sun’s diameter is about 400 times that of the Moon. The Sun is also (on average) about 400 times farther away. As a result, the two bodies appear almost exactly the same angular size in the sky — about ½°, roughly half the width of your pinky finger seen at arm’s length. This truly remarkable coincidence is what gives us total solar eclipses. If the Moon were slightly smaller or orbited a little farther away from Earth, it would never completely cover the solar disk. If the Moon were a little larger or orbited a bit closer to Earth, it would block much of the solar corona during totality, and eclipses wouldn’t be nearly as spectacular.
Of course the Moon doesn’t totally eclipse the Sun every month — if it did, seeing totality wouldn’t be as much of a thrill. And even when the lunar disk encroaches on the Sun, it doesn’t always completely cover the solar disk. In fact, at new Moon — the only lunar phase when a solar eclipse can occur — the Moon usually misses the Sun altogether. Given all the variables, it’s almost surprising that we see eclipses at all.
A Celestial Dance
The Moon orbits Earth; both swing around the Sun. In a perfect universe, we’d see totality every month. But we don’t, and here’s why.
First, the apparent size of the Sun varies during the year because Earth’s orbit is an ellipse, not a perfect circle. Our planet is closest to the Sun (perihelion) in early January and farthest (aphelion) in early July. So the Sun appears about 3% larger in January than in July (not that you’d notice), which means at times it’s harder for the Moon to completely cover the Sun and create a total eclipse.
More dramatic is the change in the Moon’s apparent diameter due to its elliptical orbit around Earth. When the Moon is closest to Earth (perigee), its apparent diameter is 14% larger than when it’s farthest (apogee). When near perigee, the Moon can easily cover the entire solar disk and create a total solar eclipse. But at apogee the Moon is too small to cover all of the Sun’s brilliant face. At mideclipse an annulus (ring) of sunlight surrounds the lunar silhouette, resulting in an annular eclipse.
The variability in the apparent size of the Sun and Moon doesn’t preclude a monthly solar eclipse. What does is the tilt of the Moon’s orbit, which is about 5° to the plane of Earth’s orbit around the Sun or, equivalently, the Sun’s apparent path around the sky as seen from Earth. (This path is called the ecliptic, for reasons that will become obvious in a moment.) More often than not, the new Moon passes above or below the Sun, and the lunar shadow misses Earth completely.
But every 173.3 days (roughly every 6 months), the new Moon passes through one of two crossover points (nodes) where the Moon’s tilted orbit intersects the ecliptic. Here, at last, a solar eclipse is possible, though the Moon can pass through a node without the eclipse being total or annular — a partial eclipse can occur instead.
Does this limit eclipses to twice a year? Not quite, because the Moon doesn’t have to move exactly through the middle of a node to cause an eclipse. It can be off by a little, which means it’s possible to have two solar eclipses within a month of each other, though both will be partials.
The complications don’t end there. The nodes slowly shift (precess) westward, which means the months in which eclipses take place slowly change as the years pass. This also affects the type of eclipse that occurs: currently long annulars are more likely in January, long totals in July.
Finally, after 6,585.32 days (18 years, 11 days, 8 hours), the entire eclipse cycle repeats. This is known as the Saros cycle. When two eclipses are separated by a period of one Saros, the Sun, Earth, and Moon return to approximately the same relative geometry, and a nearly identical eclipse will occur (though the eclipse path will be shifted west by eight hours — one third of Earth’s rotation).
Nothing Lasts Forever
The cosmic coincidence that gives us total solar eclipses isn’t permanent. The Moon is ever so slowly moving away from our planet at rate of about 1.5 inches (3.8 centimeters) per year. As it recedes, its average apparent diameter shrinks. Eventually, the Moon will never be large enough to completely cover the Sun, and total eclipses will no longer be visible from Earth’s surface.
And when might this sad prospect come to pass? The calculation is not precise — there are many unknowns such as whether the lunar retreat will continue at a constant rate and whether the solar diameter will remain stable over a long period of time. Still, about a billion years from now, give or take a few hundred million years, the surface of Earth will experience its final total eclipse of the Sun. Annular eclipses will continue to occur, though the percentage of the solar surface hidden by the Moon will gradually decrease.
So, when you stand in the lunar shadow watching the Moon pass between Earth and the Sun, revel in the knowledge that you are witnessing one of the most unusual and spectacular events in the cosmos.