Solar Eclipse in 2017
But, you may ask, the Sun is so much larger than the Moon, so how does this work?
While our daytime star has a diam4eter about 400 times larger than the Moon, it also lies roughly 400 times farther away. This means both disks appear to be the same size, so at certain times from ce3rtain locations, the Moon can completely cover the Sun.
If you want to look, be sure to protect your eyes during the partial phases. The simplest way is to buy a pair of solar viewing glasses: wear them even when 99 percent of the Sun is covered because the remaining part is still intense enough to cause retinal burns. But remember: During the 2 minutes and 40 seconds of totality, remove any solar filters, or you’ll; miss the most spectacular part of the eclipse.
The three main types of solar eclipses are total, where the Moon completely covers the Sun’s surface; annular, during which the Moon lies too far from Earth (or Earth too far from the Sun) for it to cover the Sun completely; and partial, where the lineup isn’t exact and only the Moon’s outer shadow touches our planet.
When do eclipses happen? The geometry has to be right. The Moon’s tilted orbit intersects our orbit around the Sun only twice in each revolution at points called nodes. Only when the Moon lies at one of the nodes can an eclipse (solar or lunar) occur.
As mentioned above, there are two types of shadows that will happen in August, 2017: total and partial. The graphic shows the geometry. If the Sun
The graphics at left explains the two types of shadows.
If the Sun were a point source, like one of the nighttime stars, the Moon would cast only one kind of shadow. Instead, the Sun stretches 0.5° across, so even during total solar eclipses, some of its light passes above or below the Moon, creating a less-dense shadow called the penumbra. Only where the Moon blocks all the light from the Sun—in its dark inner shadow called the umbra—can people on Earth see a total solar eclipse. Anywhere in the penumbra, the eclipse will be partial, but the percentage of the Sun covered will increase as you get near the umbra. Unfortunately, the umbra is small, no more than a hundred miles in diameter. On the other hand, the penumbra measures mare than 4,000 miles across.
This image shows from now until the end of 2037 that 12 total solar eclipses will occur. This map shows the paths of totality in orange and each eclipse’s center line in black. Below the sequence shows an entire total eclipse in 11 images. The center shows totality, while the two diamond rings flank it.
 See Michael E. Bakich, “Solar Eclipse Geometry,” Astronomy (45, 5, May 2017, pp. 34-35)