There are four types of solar eclipses: The Sun's distance from Earth is about 400 times the Moon's distance, and the Sun's diameter is about 400 times the Moon's diameter. Because these ratios are approximately the same, the Sun and the Moon as seen from Earth appear to be approximately the same size: about 0.5 degree of arc in angular measure. A separate category of solar eclipses is that of the Sun being occluded by a body other than the Earth's Moon, as can be observed at points in space away from the Earth's surface. Two examples are when the crew of Apollo 12 observed the in 1969 and when the "Cassini" probe observed in 2006.
Types
Solar eclipse
Solar eclipse | Types
There are four types of solar eclipses. There are four types of solar eclipses Sorry. I cannot find the answer based on the context. Sorry. I cannot find the answer based on the context.
what factor limits the number of eclipses each year
user
The alignment of the Sun, Moon and Earth.
assistant
what is this phenomena ?
user
A solar eclipse occurs when a portion of the Earth is engulfed in a shadow cast by the Moon which fully or partially blocks sunlight.
assistant
what are the different types of it ?
user
There are four types of solar eclipses: The Sun's distance from Earth is about 400 times the Moon's distance, and the Sun's diameter is about 400 times the Moon's diameter. Because these ratios are approximately the same, the Sun and the Moon as seen from Earth appear to be approximately the same size: about 0.5 degree of arc in angular measure. A separate category of solar eclipses is that of the Sun being occluded by a body other than the Earth's Moon, as can be observed at points in space away from the Earth's surface. Two examples are when the crew of Apollo 12 observed the in 1969 and when the "Cassini" probe observed in 2006.
Solar eclipse | Types
Sun - Moon - Earth: Solar eclipse | annular eclipse | hybrid eclipse | partial eclipse Sun - Earth - Moon: Lunar eclipse | penumbral eclipse | partial lunar eclipse | central lunar eclipse Sun - Phobos - Mars: Transit of Phobos from Mars | Solar eclipses on Mars
Eclipse | Types
As observed from the Earth, a solar eclipse occurs when the Moon passes in front of the Sun. The type of solar eclipse event depends on the distance of the Moon from the Earth during the event. A total solar eclipse occurs when the Earth intersects the umbra portion of the Moon's shadow. When the umbra does not reach the surface of the Earth, the Sun is only partially occulted, resulting in an annular eclipse. Partial solar eclipses occur when the viewer is inside the penumbra. The eclipse magnitude is the fraction of the Sun's diameter that is covered by the Moon.
Eclipse | Solar eclipse
Conversely, an eclipse that occurs when the Moon is near its farthest distance from Earth ("i.e.," near its apogee) can only be an annular eclipse because the Moon will appear to be slightly smaller than the Sun; the magnitude of an annular eclipse is less than 1.
Solar eclipse | Types
The Moon's orbit around the Earth is slightly elliptical, as is the Earth's orbit around the Sun. The apparent sizes of the Sun and Moon therefore vary. The magnitude of an eclipse is the ratio of the apparent size of the Moon to the apparent size of the Sun during an eclipse. An eclipse that occurs when the Moon is near its closest distance to Earth ("i.e.," near its perigee) can be a total eclipse because the Moon will appear to be large enough to completely cover the Sun's bright disk or photosphere; a total eclipse has a magnitude greater than or equal to 1.000.
Solar eclipse | Types
The type of each solar eclipse (whether total or annular, as seen from the sublunar point) depends on the apparent sizes of the Sun and Moon, which are functions of the distances of Earth from the Sun and of the Moon from Earth, respectively, as seen from Earth's surface. These distances vary because both the Earth and the Moon have elliptic orbits.
Eclipse season | Introduction
Earth's shadow can be divided into two distinctive parts: the umbra and penumbra. Earth totally occludes direct solar radiation within the umbra, the central region of the shadow. However, since the Sun's diameter appears about one-quarter of Earth's in the lunar sky, the planet only partially blocks direct sunlight within the penumbra, the outer portion of the shadow. A "penumbral lunar eclipse" occurs when the Moon passes through Earth's penumbra. The penumbra causes a subtle dimming of the lunar surface, which is only visible to the naked eye when about 70% of the Moon's diameter has immersed into Earth's penumbra.
Lunar eclipse | Types of lunar eclipse
A total solar eclipse provides a rare opportunity to observe the corona (the outer layer of the Sun's atmosphere). Normally this is not visible because the photosphere is much brighter than the corona. According to the point reached in the solar cycle, the corona may appear small and symmetric, or large and fuzzy. It is very hard to predict this in advance. As the light filters through leaves of trees during a partial eclipse, the overlapping leaves create natural pinholes, displaying mini eclipses on the ground. Phenomena associated with eclipses include shadow bands (also known as "flying shadows"), which are similar to shadows on the bottom of a swimming pool.
Solar eclipse | Other observations
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 161 appears in the following table.
Solar Saros 161 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or
Solar Saros 132 | Umbral eclipses
A solar eclipse occurs when a portion of the Earth is engulfed in a shadow cast by the Moon which fully or partially blocks sunlight. This occurs when the Sun, Moon and Earth are aligned. Such alignment coincides with a new moon (syzygy) indicating the Moon is closest to the ecliptic plane. In a total eclipse, the disk of the Sun is fully obscured by the Moon. In partial and annular eclipses, only part of the Sun is obscured. If the Moon were in a perfectly circular orbit, a little closer to the Earth, and in the same orbital plane, there would be total solar eclipses every new moon.
Solar eclipse | Introduction
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 155 appears in the following table.
Solar Saros 155 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 151 appears in the following table.
Solar Saros 151 | Umbral eclipses
However, depending on how much of the Sun's disk is obscured, some darkening may be noticeable. If three-quarters or more of the Sun is obscured, then an effect can be observed by which the daylight appears to be dim, as if the sky were overcast, yet objects still cast sharp shadows.
Solar eclipse | Partial and annular eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 131 appears in the following table.
Solar Saros 131 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 157 appears in the following table.
Solar Saros 157 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 159 appears in the following table.
Solar Saros 159 | Umbral eclipses
The type of solar eclipse that happens during each season (whether total, annular, hybrid, or partial) depends on apparent sizes of the Sun and Moon. If the orbit of the Earth around the Sun, and the Moon's orbit around the Earth were both in the same plane with each other, then eclipses would happen each and every month. There would be a lunar eclipse at every full moon, and a solar eclipse at every new moon. And if both orbits were perfectly circular, then each solar eclipse would be the same type every month. It is because of the non-planar and non-circular differences that eclipses are not a common event.
Eclipse | Introduction
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 152 appears in the following table.
Solar Saros 152 | Umbral eclipses
A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. The eclipse is either total or annular. In a total eclipse, the moon's size from earth is large enough to block all of the disk of the sun. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring), that is there is a ring of the sun around the dark moon.
Solar eclipse of May 10, 1994 | The Annular Eclipse of May 10, 1994
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 112 appears in the following table.
Solar Saros 112 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 153 appears in the following table.
Solar Saros 153 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 156 appears in the following table.
Solar Saros 156 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 148 appears in the following table.
Solar Saros 148 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 147 appears in the following table.
Solar Saros 147 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 158 appears in the following table.
Solar Saros 158 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 150 appears in the following table.
Solar Saros 150 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 142 appears in the following table.
Solar Saros 142 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 136 appears in the following table.
Solar Saros 136 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 137 appears in the following table.
Solar Saros 137 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 130 appears in the following table.
Solar Saros 130 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 111 appears in the following table.
Solar Saros 111 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 138 appears in the following table.
Solar Saros 138 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 116 appears in the following table.
Solar Saros 116 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 162 appears in the following table.
Solar Saros 162 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 110 appears in the following table.
Solar Saros 110 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 160 appears in the following table.
Solar Saros 160 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 154 appears in the following table.
Solar Saros 154 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 123 appears in the following table.
Solar Saros 123 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 134 appears in the following table.
Solar Saros 134 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 119 appears in the following table.
Solar Saros 119 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 117 appears in the following table.
Solar Saros 117 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 133 appears in the following table.
Solar Saros 133 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 141 appears in the following table.
Solar Saros 141 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 149 appears in the following table.
Solar Saros 149 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 135 appears in the following table.
Solar Saros 135 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 127 appears in the following table.
Solar Saros 127 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 115 appears in the following table.
Solar Saros 115 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 145 appears in the following table.
Solar Saros 145 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 120 appears in the following table.
Solar Saros 120 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 140 appears in the following table.
Solar Saros 140 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 146 appears in the following table.
Solar Saros 146 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 125 appears in the following table.
Solar Saros 125 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 124 appears in the following table.
Solar Saros 124 | Umbral eclipses
Viewing the Sun during partial and annular eclipses (and during total eclipses outside the brief period of totality) requires special eye protection, or indirect viewing methods if eye damage is to be avoided. The Sun's disk can be viewed using appropriate filtration to block the harmful part of the Sun's radiation. Sunglasses do not make viewing the Sun safe. Only properly designed and certified solar filters should be used for direct viewing of the Sun's disk. Especially, self-made filters using common objects such as a floppy disk removed from its case, a Compact Disc, a black colour slide film, smoked glass, etc.
Solar eclipse | Partial and annular eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 114 appears in the following table.
Solar Saros 114 | Umbral eclipses
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots. These phenomena are apparently generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations. The total sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather.
Solar phenomena | Introduction
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 129 appears in the following table.
Solar Saros 129 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 144 appears in the following table.
Solar Saros 144 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 113 appears in the following table.
Solar Saros 113 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 122 appears in the following table.
Solar Saros 122 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 139 appears in the following table.
Solar Saros 139 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 143 appears in the following table.
Solar Saros 143 | Umbral eclipses
This is because the only sunlight available is refracted through the Earth's atmosphere on the edges of the Earth, forming an atmospheric ring.
Solar eclipses on the Moon | Center of the Earth's shadow
A solar eclipse occurs when the Moon passes between the Earth and the Sun, casting a shadow on Earth that temporarily obscures part or all of the Sun's disc. Eclipses can occur only when all three bodies are properly aligned. Partial eclipses, in which only a portion of the Sun's surface is obscured, are relatively common due to the width of the Moon's outer shadow, or penumbra, which may be several hundred miles wide. Total eclipses occur when the Moon's inner shadow, or umbra, reaches the surface of the Earth, completely obscuring the Sun over a much narrower portion of the ground.
Solar eclipse of July 28, 1851 | Background
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 121 appears in the following table.
Solar Saros 121 | Umbral eclipses
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 128 appears in the following table.
Solar Saros 128 | Umbral eclipses
A special type of penumbral eclipse is a "total penumbral lunar eclipse", during which the Moon lies exclusively within Earth's penumbra. Total penumbral eclipses are rare, and when these occur, the portion of the Moon closest to the umbra may appear slightly darker than the rest of the lunar disk. A "partial lunar eclipse" occurs when only a portion of the Moon enters Earth's umbra, while a "total lunar eclipse" occurs when the entire Moon enters the planet's umbra. The Moon's average orbital speed is about , or a little more than its diameter per hour, so totality may last up to nearly 107 minutes.
Lunar eclipse | Types of lunar eclipse
When the shrinking visible part of the photosphere becomes very small, Baily's beads will occur. These are caused by the sunlight still being able to reach the Earth through lunar valleys. Totality then begins with the diamond ring effect, the last bright flash of sunlight. It is safe to observe the total phase of a solar eclipse directly only when the Sun's photosphere is completely covered by the Moon, and not before or after totality. During this period, the Sun is too dim to be seen through filters. The Sun's faint corona will be visible, and the chromosphere, solar prominences, and possibly even a solar flare may be seen.
Solar eclipse | Totality
A hybrid (annular/total) solar eclipse occurred on October 30, 1845 during winter. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A hybrid solar eclipse shifts between a total and annular eclipse. At certain points on the surface of Earth it appears as a total eclipse, whereas at other points it appears as annular. Hybrid eclipses are comparatively rare. This eclipse is a hybrid event, a narrow total eclipse, and beginning and ending as an annular eclipse. The greatest eclipse was in northeasternmost Antarctica south of where the Indian and Pacific Ocean divides at 69.1 S and 144.5 E at 23:51 UTC (9:51 am on October 31), in that portion of Antarctica and the surrounding waters it shown as a total eclipse, the remainder was as an annular, first in the Indian Ocean then in the Antarctic Peninsula.
Solar eclipse of October 30, 1845 | Introduction
In its eclipses, the penumbral shadow does not appear until it is around 25–30% obscuration. It becomes slightly darker when the Earth blocks the sunlight until it reaches totality in some eclipses. In some eclipses, its penumbral shadow covers the whole surface, whereas the center of the Earth's shadow misses a portion of the Moon while every part of the Nearside sees a partial eclipse. These eclipses are very rare. The last century that not all parts of the near side and the surrounding parts of the far side saw only as partial was the 18th century. On Earth, they are seen as total penumbral eclipses.
Solar eclipses on the Moon | Penumbral shadow
During a total solar eclipse, when the disk of the Sun is covered by that of the Moon, parts of the Sun's surrounding atmosphere can be seen. It is composed of four distinct parts: the chromosphere, the transition region, the corona and the heliosphere. The coolest layer of the Sun is a temperature minimum region extending to about above the photosphere, and has a temperature of about . This part of the Sun is cool enough to allow the existence of simple molecules such as carbon monoxide and water, which can be detected via their absorption spectra. The chromosphere, transition region, and corona are much hotter than the surface of the Sun.
Sun | Atmosphere
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 118 appears in the following table.
Solar Saros 118 | Umbral eclipses Part 1
Umbral eclipses (annular, total and hybrid) can be further classified as either: 1) Central (two limits), 2) Central (one limit) or 3) Non-Central (one limit). The statistical distribution of these classes in Saros series 126 appears in the following table.
Solar Saros 126 | Umbral eclipses
An annular solar eclipse will occur on June 11, 2067. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of June 11, 2067 | Introduction
A hybrid (annular/total) solar eclipse occurred on February 11, 1804. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An hybrid solar eclipse shifts between a total and annular eclipse. At certain points on the surface of Earth it appears as a total eclipse, whereas at other points it appears as annular. Hybrid eclipses are comparatively rare. This eclipse is a hybrid event, a narrow total eclipse, and beginning and ending as an annular eclipse. The greatest eclipse was in the Sahara Desert in modern-day Algeria at 26.7 N, 4.5 W at 11:16:33 UTC, in that portion it shown as a total eclipse, the remainder was as an annular.
Solar eclipse of February 11, 1804 | Introduction
This would be essentially the same as the earthshine which can frequently be seen when the Moon's phase is a narrow crescent. In reality, the corona, though much less brilliant than the Sun's photosphere, is much brighter than the Moon illuminated by earthlight. Therefore, by contrast, the Moon during a total solar eclipse appears to be black, with the corona surrounding it.
Solar eclipse | Earthshine
The absolute value of gamma (denoted as ) allows us to distinguish different kinds of solar eclipses from the earth: If the Earth were a sphere, the limit for a central eclipse would be 1.0, but because of the oblateness of the Earth (which causes the distance between the Earth's north and south poles to be slightly shorter than if the Earth were perfectly spherical), it is 0.9972. The Solar eclipse of April 29, 2014, with a gamma of 0.9999, is an example of the special case of a non-central annular eclipse. The axis of the shadow cone barely missed Earth's south pole.
Gamma (eclipse) | Limiting cases for solar eclipses on the earth
An annular solar eclipse occurred on September 7, 1820. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of September 7, 1820 | Introduction
The diagrams to the right show the alignment of the Sun, Moon, and Earth during a solar eclipse. The dark gray region between the Moon and Earth is the umbra, where the Sun is completely obscured by the Moon. The small area where the umbra touches Earth's surface is where a total eclipse can be seen. The larger light gray area is the penumbra, in which a partial eclipse can be seen. An observer in the antumbra, the area of shadow beyond the umbra, will see an annular eclipse. The Moon's orbit around the Earth is inclined at an angle of just over 5 degrees to the plane of the Earth's orbit around the Sun (the ecliptic).
Solar eclipse | Geometry
A total solar eclipse will occur on December 6, 2067. It is a hybrid event, beginning and ending as an annular eclipse. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of December 6, 2067 | Introduction
The table contains the date and time of the greatest eclipse (in dynamical time, which in this case is the time when the axis of the Moon's shadow cone passes closest to the centre of Earth; this is in (Ephemeris Time). The number of the saros series that the eclipse belongs to is given, followed by the magnitude of the eclipse (the fraction of the Sun's diameter obscured by the Moon) and the type of the eclipse (either total, annular, partial or hybrid). For total and annular eclipses, the duration of the eclipse is given, as well as the location of the greatest eclipse (the point of maximum eclipse) and the path width of the total or annular eclipse.
List of solar eclipses in the 21st century | Introduction
An annular solar eclipse will occur on June 22, 2066. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of June 22, 2066 | Introduction
An annular solar eclipse occurred on April 30, 1957. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. This annular solar eclipse was non-central. Instead, over half of the antumbral shadow fell off into space throughout the eclipse.
Solar eclipse of April 30, 1957 | Introduction
An annular solar eclipse will occur on June 22, 2085. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of June 22, 2085 | Introduction
The region of an object's shadow during an eclipse is divided into three parts: A total eclipse occurs when the observer is within the umbra, an annular eclipse when the observer is within the antumbra, and a partial eclipse when the observer is within the penumbra. During a lunar eclipse only the umbra and penumbra are applicable, because the antumbra of the Sun-Earth system lies far beyond the Moon. Analagously, Earth's apparent diameter from the viewpoint of the Moon is nearly four times that of the Sun and thus cannot produce an annular eclipse. The same terms may be used analogously in describing other eclipses, e.g., the antumbra of Deimos crossing Mars, or Phobos entering Mars's penumbra.
Eclipse | Umbra, penumbra and antumbra
An annual solar eclipse occurred on November 12, 1947. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Annularity was visible from the Pacific Ocean, Peru, Ecuador, Colombia and Brazil.
Solar eclipse of November 12, 1947 | Introduction
An annular solar eclipse occurred on July 14, 1749. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of July 14, 1749 | Introduction
The distance of the Earth from the Sun also varies during the year, but this is a smaller effect. On average, the Moon appears to be slightly smaller than the Sun as seen from the Earth, so the majority (about 60%) of central eclipses are annular. It is only when the Moon is closer to the Earth than average (near its perigee) that a total eclipse occurs.
Solar eclipse | Geometry
An annular solar eclipse will occur on July 24, 2074. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of July 24, 2074 | Introduction
An annular solar eclipse occurred on June 10, 2002. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Annularity was visible in Indonesia, Palau (Kayangel Atoll), Northern Mariana on June 11th (Tuesday), and the western tip of Jalisco, Mexico on June 10th (Monday).
Solar eclipse of June 10, 2002 | Introduction
An annular solar eclipse will occur on October 13, 2061. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of October 13, 2061 | Introduction
An annular solar eclipse occurred on April 29, 2014. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. The center of the Moon's shadow missed the Earth's South Pole, but the partial eclipse was visible from parts of Antarctica and Australia, and an annular eclipse was visible from a small part of Antarctica.
Solar eclipse of April 29, 2014 | Introduction
A partial solar eclipse occurred on June 17, 1928. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth. This is the 1st solar eclipse of Solar Saros 155, and this is the new saros to begin since the partial solar eclipse of July 19, 1917.
Solar eclipse of June 17, 1928 | Introduction
An annular solar eclipse will occur on July 23, 2093. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of July 23, 2093 | Introduction
Total solar eclipses are seen on Earth because of a fortuitous combination of circumstances. Even on Earth, the diversity of eclipses familiar to people today is a temporary (on a geological time scale) phenomenon. Hundreds of millions of years in the past, the Moon was closer to the Earth and therefore apparently larger, so every solar eclipse was total or partial, and there were no annular eclipses. Due to tidal acceleration, the orbit of the Moon around the Earth becomes approximately 3.8 cm more distant each year. Millions of years in the future, the Moon will be too far away to fully occlude the Sun, and no total eclipses will occur.
Solar eclipse | Final totality
An annular solar eclipse occurred on September 5, 1793. A solar eclipse occurs when the Moon passes between the Earth and the Sun, thereby totally or partially obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon’s apparent diameter is smaller than the Sun’s, blocking most of the Sun’s light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometers wide.
Solar eclipse of September 5, 1793 | Introduction
A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth. This was the first of four partial solar eclipses in 2011, with the others occurring on June 1, 2011, July 1, 2011, and November 25, 2011.
Solar eclipse of January 4, 2011 | Introduction
An annular solar eclipse took place at the Moon’s descending node of the orbit on May 9–10 (UTC), 2013, with a magnitude of 0.9544. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun fogghhvfhvsjvhr a viewer on Earth. An annular solar eclipse occurs whenshit the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of May 10, 2013 | Introduction
An annular solar eclipse will occur on October 4, 2070. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide.
Solar eclipse of October 4, 2070 | Introduction