There are three types of solar eclipses - partial, annular, and total. Not all solar eclipses are created equal. How much of the Sun is covered by the moon determines if you can see a partial, annular, or total eclipse. A solar eclipse occurs when the moon passes between the Sun and Earth, completely or partially blocking our view of the Sun and casting a shadow on Earth. A solar eclipse can only occur during the day, if you have seen an eclipse at night then you have seen a lunar eclipse.
A partial eclipse occurs when the moon only covers part of the Sun.During a partial solar eclipse, the darkest shadow of the moon, the umbra, misses Earth. Only a partial shadow, the penumbra, lands on Earth.
A total solar eclipse is when the moon completely blocks our view of the Sun, revealing the Sun''s outer atmosphere—the corona.A total solar eclipse occurs when the moon is precisely positioned between the Sun and Earth, causing the shadow of the moon to fall on Earth. If you are standing in the middle of this shadow (the umbra), then the view of the Sun will be completely blocked by the moon, allowing you to see the outer atmosphere of the Sun (the corona). If you''re anywhere within the significantly larger partial shadow (the penumbra), you will see a partial eclipse.
Once in a while, an eclipse will be total along parts of its path and annular or partial along other parts.But the plane of the moon''s orbit around Earth is tilted by about five degrees with respect to the Earth''s orbit around the Sun. This causes the moon''s shadow to often pass above or below the Earth. This is the least frequent type of solar eclipse.
From Amsterdam, the Sun will be eclipsed to a maximum of 22%, but elsewhere in Netherlands the Sun will be eclipsed to a maximum of 25% (change location ).
In the northern hemisphere, a maximum of 82% of the Sun''s disk will be eclipsed by the Moon, but nowhere on Earth will see a total solar eclipse. This is because nowhere on Earth will see a perfect alignment between the Sun and Moon in the sky.
This map is also available as a KMZ overlay which can be imported into Google Earth, Google Maps, or other mapping software, to create a more detailed map. Alternatively, it can be downloaded as a non-interactive image in PNG, PDF or SVG format.
The animation above shows the progress of the Moon''s shadow across the Earth as the eclipse proceeds. The red circle shows the edge of the Moon''s shadow: all places inside the red circle will see the Moon covering some part of the Sun''s disk. Within this, the yellow contours show where various fractions of the Sun''s disk is covered.
By default the simulation is drawn with the local vertical in Amsterdam uppermost (Zenith up), so that it is orientated as you would see it looking up at the sky through an appropriate solar filter. The compass shows the direction of celestial north relative to the local vertical. Alternatively, you can orientate the Sun with celestial north orientated uppermost, by selecting the option North up.
In the diagram to the right, the grid represents the plane of the Earth''s orbit around the Sun. As it circles the Earth, the Moon passes through this Earth–Sun plane twice each month, at the points on the left and right labelled as nodes. A solar eclipse happens only when one of these node crossings happens to coincide with New Moon. This happens roughly once every six months.
The Moon is much smaller than the Earth, and the shadow it casts onto the Earth is never more than a few hundred miles across. The diagram to the right is not drawn to scale, but gives an approximate sense of how much of the Earth''s surface can be covered by the Moon''s shadow at any one time. As the Moon travels along its orbit, its shadow sweeps across the Earth, usually travelling from west to east at a speed which varies between 1,000 and 5,000 mph.
The Moon''s shadow can be divided into the umbra, indicated as a dark gray cone, where the Moon appears to completely cover the Sun, and the larger penumbra, where the Moon only partially covers the Sun.
When the Earth and Moon are at their closest, the umbral shadow projects a circle onto the Earth''s surface with a diameter of 170 miles, within which a total solar eclipse can be seen. But when the Earth is at its furthest from the Moon, the planet falls beyond the furthest limit of the Moon''s umbral shadow and the Moon appears too small to entirely cover the Sun''s disk. This gives rise to the possibility of annular eclipses, where a complete ring of sunlight is formed around the Moon.
The region of space where annular eclipses are seen lies beyond the furthest tip of the umbra at a distance of 373,000 km from the Moon, in a third region of shadow called the antumbra.
The Earth is drawn twice, at its closest and furthest possible distances from the Moon – distances of around 363,000 km and 405,000 km respectively. The cross marks the maximum extent of the Moon''s umbra – the furthest distance from Moon at which a total eclipse is possible (373,000 km).
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