Solar eclipse

An annular solar eclipse (left) occurs when the Moon is too far away to completely cover the Sun's disk (May 20, 2012). During a partial solar eclipse (right), the Moon blocks only part of the Sun's disk (October 25, 2022 ).

A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby obscuring the view of the Sun from a small part of the Earth, totally or partially. Such an alignment occurs approximately every six months, during the eclipse season in its new moon phase, when the Moon's orbital plane is closest to the plane of the Earth's orbit.^[1] 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. Unlike a lunar eclipse, which may be viewed from anywhere on the night side of Earth, a solar eclipse can only be viewed from a relatively small area of the world. As such, although total solar eclipses occur somewhere on Earth every 18 months on average, they recur at any given place only once every 360 to 410 years.

If the Moon were in a perfectly circular orbit and in the same orbital plane as Earth, there would be total solar eclipses once a month, at every new moon. Instead, because the Moon's orbit is

An eclipse is a natural phenomenon. In some ancient and modern cultures, solar eclipses were attributed to supernatural causes or regarded as bad omens. Astronomers' predictions of eclipses began in China as early as the 4th century BC; eclipses hundreds of years into the future may now be predicted with high accuracy.

Looking directly at the Sun can lead to permanent eye damage, so special eye protection or indirect viewing techniques are used when viewing a solar eclipse. Only the total phase of a total solar eclipse is safe to view without protection. Enthusiasts known as eclipse chasers or umbraphiles travel to remote locations to see solar eclipses.^[4][5]

The symbol for an occultation, and especially a solar eclipse, is

Types

Partial and annular phases of the solar eclipse of May 20, 2012

• A total eclipse occurs when the dark silhouette of the Moon completely obscures the intensely bright light of the Sun, allowing the much fainter
  solar corona to be visible. During any one eclipse, totality occurs at best only in a narrow track on the surface of Earth.^[6] This narrow track is called the path of totality.^[7]
• An annular eclipse occurs when the Sun and Moon are exactly in line with the Earth, but the apparent size of the Moon is smaller than that of the Sun. Hence the Sun appears as a very bright ring, or annulus, surrounding the dark disk of the Moon.^[8]
• A hybrid eclipse (also called annular/total 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.^[8]
• A partial eclipse occurs when the Sun and Moon are not exactly in line with the Earth and the Moon only partially obscures the Sun. This phenomenon can usually be seen from a large part of the Earth outside of the track of an annular or total eclipse. However, some eclipses can be seen only as a partial eclipse, because the
  civil twilight.^[9]

Comparison of minimum and maximum apparent sizes of the Sun and Moon (and planets). An annular eclipse can occur when the Sun has a larger apparent size than the Moon, whereas a total eclipse can occur when the Moon has a larger apparent size.

A hybrid eclipse occurs when the magnitude of an eclipse changes during the event from less to greater than one, so the eclipse appears to be total at locations nearer the midpoint, and annular at other locations nearer the beginning and end, since the sides of the Earth are slightly further away from the Moon. These eclipses are extremely narrow in their path width and relatively short in their duration at any point compared with fully total eclipses; the 2023 April 20 hybrid eclipse's totality is over a minute in duration at various points along the path of totality. Like a focal point, the width and duration of totality and annularity are near zero at the points where the changes between the two occur.^[12]

Because the Earth's orbit around the Sun is also elliptical, the Earth's distance from the Sun similarly varies throughout the year. This affects the apparent size of the Sun in the same way, but not as much as does the Moon's varying distance from Earth.

Terminology for central eclipse

Diamond ring effect at third contact—the end of totality—with visible prominences

Central eclipse is often used as a generic term for a total, annular, or hybrid eclipse.[14] This is, however, not completely correct: the definition of a central eclipse is an eclipse during which the central line of the umbra touches the Earth's surface. It is possible, though extremely rare, that part of the umbra intersects with the Earth (thus creating an annular or total eclipse), but not its central line. This is then called a non-central total or annular eclipse.^[14] Gamma is a measure of how centrally the shadow strikes. The last (umbral yet) non-central solar eclipse was on April 29, 2014. This was an annular eclipse. The next non-central total solar eclipse will be on April 9, 2043.^[15]

The visual phases observed during a total eclipse are called:^[16]

• First contact—when the Moon's limb (edge) is exactly tangential to the Sun's limb.
• Second contact—starting with
  diamond ring effect
  . Almost the entire disk is covered.
• Totality—the Moon obscures the entire disk of the Sun and only the solar corona is visible.
• Third contact—when the first bright light becomes visible and the Moon's shadow is moving away from the observer. Again a diamond ring may be observed.
• Fourth contact—when the trailing edge of the Moon ceases to overlap with the solar disk and the eclipse ends.

Predictions

Geometry

antumbra, the area of shadow beyond the umbra, will see an annular eclipse.^[17]

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). Because of this, at the time of a new moon, the Moon will usually pass to the north or south of the Sun. A solar eclipse can occur only when a new moon occurs close to one of the points (known as nodes) where the Moon's orbit crosses the ecliptic.^[18]

As noted above, the Moon's orbit is also

perigee) that a total eclipse occurs.^[19][20]

	Moon		Sun
	At perigee (nearest)	At apogee (farthest)	At perihelion (nearest)	At aphelion (farthest)
Mean radius	1,737.10 km (1,079.38 mi)		696,000 km (432,000 mi)
Distance	363,104 km (225,622 mi)	405,696 km (252,088 mi)	147,098,070 km (91,402,500 mi)	152,097,700 km (94,509,100 mi)
Angular diameter[21]	33' 30" (0.5583°)	29' 26" (0.4905°)	32' 42" (0.5450°)	31' 36" (0.5267°)
Apparent size to scale
Order by decreasing apparent size	1st	4th	2nd	3rd

The Moon orbits the Earth in approximately 27.3 days, relative to a

synodic month and corresponds to what is commonly called the lunar month.^[18]

The Moon crosses from south to north of the ecliptic at its

draconic month.^[22]

Finally, the Moon's perigee is moving forwards or precessing in its orbit and makes a complete circuit in 8.85 years. The time between one perigee and the next is slightly longer than the sidereal month and known as the

anomalistic month.^[23]

The Moon's orbit intersects with the ecliptic at the two nodes that are 180 degrees apart. Therefore, the new moon occurs close to the nodes at two periods of the year approximately six months (173.3 days) apart, known as eclipse seasons, and there will always be at least one solar eclipse during these periods. Sometimes the new moon occurs close enough to a node during two consecutive months to eclipse the Sun on both occasions in two partial eclipses. This means that, in any given year, there will always be at least two solar eclipses, and there can be as many as five.^[24]

Eclipses can occur only when the Sun is within about 15 to 18 degrees of a node, (10 to 12 degrees for central eclipses). This is referred to as an eclipse limit, and is given in ranges because the apparent sizes and speeds of the Sun and Moon vary throughout the year. In the time it takes for the Moon to return to a node (draconic month), the apparent position of the Sun has moved about 29 degrees, relative to the nodes.^[2] Since the eclipse limit creates a window of opportunity of up to 36 degrees (24 degrees for central eclipses), it is possible for partial eclipses (or rarely a partial and a central eclipse) to occur in consecutive months.^[25][26]

Fraction of the Sun's disc covered, f, when the same-sized discs are offset a fraction t of their diameter.^[27]

Path

During a central eclipse, the Moon's umbra (or antumbra, in the case of an annular eclipse) moves rapidly from west to east across the Earth. The Earth is also rotating from west to east, at about 28 km/min at the Equator, but as the Moon is moving in the same direction as the Earth's rotation at about 61 km/min, the umbra almost always appears to move in a roughly west–east direction across a map of the Earth at the speed of the Moon's orbital velocity minus the Earth's rotational velocity.^[28]

The width of the track of a central eclipse varies according to the relative apparent diameters of the Sun and Moon. In the most favourable circumstances, when a total eclipse occurs very close to perigee, the track can be up to 267 km (166 mi) wide and the duration of totality may be over 7 minutes.^[29] Outside of the central track, a partial eclipse is seen over a much larger area of the Earth. Typically, the umbra is 100–160 km wide, while the penumbral diameter is in excess of 6400 km.^[30]

Besselian elements are used to predict whether an eclipse will be partial, annular, or total (or annular/total), and what the eclipse circumstances will be at any given location.^{[31]: Chapter 11}

Calculations with Besselian elements can determine the exact shape of the umbra's shadow on the Earth's surface. But at what longitudes on the Earth's surface the shadow will fall, is a function of the Earth's rotation, and on how much that rotation has slowed down over time. A number called ΔT is used in eclipse prediction to take this slowing into account. As the Earth slows, ΔT increases. ΔT for dates in the future can only be roughly estimated because the Earth's rotation is slowing irregularly. This means that, although it is possible to predict that there will be a total eclipse on a certain date in the far future, it is not possible to predict in the far future exactly at what longitudes that eclipse will be total. Historical records of eclipses allow estimates of past values of ΔT and so of the Earth's rotation. ^{[31]: Equation 11.132}

Duration

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The following factors determine the duration of a total solar eclipse (in order of decreasing importance):^[32][33]

1. The Moon being almost exactly at perigee (making its angular diameter as large as possible).
2. The Earth being very near aphelion (furthest away from the Sun in its elliptical orbit, making its angular diameter nearly as small as possible).
3. The midpoint of the eclipse being very close to the Earth's equator, where the rotational velocity is greatest and is closest to the speed of the lunar shadow moving over Earth's surface.
4. The vector of the eclipse path at the midpoint of the eclipse aligning with the vector of the Earth's rotation (i.e. not diagonal but due east).
5. The midpoint of the eclipse being near the subsolar point (the part of the Earth closest to the Sun).

The longest eclipse that has been calculated thus far is the eclipse of July 16, 2186 (with a maximum duration of 7 minutes 29 seconds over northern Guyana).^[32]

Occurrence and cycles

Main article: Eclipse cycle

lunar nodes relative to the Earth. This causes an eclipse season approximately every six months, in which a solar eclipse can occur at the new moon phase and a lunar eclipse can occur at the full moon

phase.

Total solar eclipse paths: 1001–2000, showing that total solar eclipses occur almost everywhere on Earth. This image was merged from 50 separate images from NASA.^[34]

Total solar eclipses are rare events. Although they occur somewhere on Earth every 18 months on average,[35] it is estimated that they recur at any given place only once every 360 to 410 years, on average.^[36] The total eclipse lasts for only a maximum of a few minutes at any location, because the Moon's umbra moves eastward at over 1700 km/h.^[37] Totality currently can never last more than 7 min 32 s. This value changes over the millennia and is currently decreasing. By the 8th millennium, the longest theoretically possible total eclipse will be less than 7 min 2 s.^[32] The last time an eclipse longer than 7 minutes occurred was June 30, 1973 (7 min 3 sec). Observers aboard a Concorde supersonic aircraft were able to stretch totality for this eclipse to about 74 minutes by flying along the path of the Moon's umbra.^[38] The next total eclipse exceeding seven minutes in duration will not occur until June 25, 2150. The longest total solar eclipse during the 11,000 year period from 3000 BC to at least 8000 AD will occur on July 16, 2186, when totality will last 7 min 29 s.^[32][39] For comparison, the longest total eclipse of the 20th century at 7 min 8 s occurred on June 20, 1955, and there will be no total solar eclipses over 7 min in duration in the 21st century.^[40]

It is possible to predict other eclipses using

saros is probably the best known and one of the most accurate. A saros lasts 6,585.3 days (a little over 18 years), which means that, after this period, a practically identical eclipse will occur. The most notable difference will be a westward shift of about 120° in longitude (due to the 0.3 days) and a little in latitude (north-south for odd-numbered cycles, the reverse for even-numbered ones). A saros series always starts with a partial eclipse near one of Earth's polar regions, then shifts over the globe through a series of annular or total eclipses, and ends with a partial eclipse at the opposite polar region. A saros series lasts 1226 to 1550 years and 69 to 87 eclipses, with about 40 to 60 of them being central.^[41]

Frequency per year

Between two and five solar eclipses occur every year, with at least one per eclipse season. Since the Gregorian calendar was instituted in 1582, years that have had five solar eclipses were 1693, 1758, 1805, 1823, 1870, and 1935. The next occurrence will be 2206.^[42] On average, there are about 240 solar eclipses each century.^[43]

The 5 solar eclipses of 1935

January 5	February 3	June 30	July 30	December 25
Partial (south)	Partial (north)	Partial (north)	Partial (south)	Annular (south)
Saros 111	Saros 149	Saros 116	Saros 154	Saros 121

Final totality

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. In the same timeframe, the Sun may become brighter, making it appear larger in size.^[44] Estimates of the time when the Moon will be unable to occlude the entire Sun when viewed from the Earth range between 650 million^[45] and 1.4 billion years in the future.^[44]

Historical eclipses

Astronomers Studying an Eclipse painted by Antoine Caron

in 1571

Historical eclipses are a very valuable resource for historians, in that they allow a few historical events to be dated precisely, from which other dates and ancient calendars may be deduced.[46] A solar eclipse of June 15, 763 BC mentioned in an Assyrian text is important for the chronology of the ancient Near East.^[47] There have been other claims to date earlier eclipses. The legendary Chinese king Zhong Kang supposedly beheaded two astronomers, Hsi and Ho, who failed to predict an eclipse 4,000 years ago.^[48] Perhaps the earliest still-unproven claim is that of archaeologist Bruce Masse, who putatively links an eclipse that occurred on May 10, 2807, BC with a possible meteor impact in the Indian Ocean on the basis of several ancient flood myths that mention a total solar eclipse.^[49] The earliest preserved depiction of a partial solar eclipse from 1143 BCE might be the one in tomb KV9 of Ramses V and Ramses VI.^[50]

Records of the solar eclipses of 993 and 1004 as well as the lunar eclipses of 1001 and 1002 by Ibn Yunus

of Cairo (c. 1005).

Eclipses have been interpreted as

Asia Minor.^[53] An eclipse recorded by Herodotus before Xerxes departed for his expedition against Greece,^[54] which is traditionally dated to 480 BC, was matched by John Russell Hind to an annular eclipse of the Sun at Sardis on February 17, 478 BC.^[55] Alternatively, a partial eclipse was visible from Persia on October 2, 480 BC.^[56] Herodotus also reports a solar eclipse at Sparta during the Second Persian invasion of Greece.^[57] The date of the eclipse (August 1, 477 BC) does not match exactly the conventional dates for the invasion accepted by historians.^[58]

Chinese records of eclipses begin at around 720 BC.[59] The 4th century BC astronomer Shi Shen described the prediction of eclipses by using the relative positions of the Moon and Sun.^[60]

Attempts have been made to establish the exact date of

Spectroscope observations were made of the solar eclipse of August 18, 1868, which helped to determine the chemical composition of the Sun.^[56]

John Fiske summed up myths about the solar eclipse like this in his 1872 book Myth and Myth-Makers,

the myth of Hercules and Cacus, the fundamental idea is the victory of the solar god over the robber who steals the light. Now whether the robber carries off the light in the evening when Indra has gone to sleep, or boldly rears his black form against the sky during the daytime, causing darkness to spread over the earth, would make little difference to the framers of the myth. To a chicken a solar eclipse is the same thing as nightfall, and he goes to roost accordingly. Why, then, should the primitive thinker have made a distinction between the darkening of the sky caused by black clouds and that caused by the rotation of the earth? He had no more conception of the scientific explanation of these phenomena than the chicken has of the scientific explanation of an eclipse. For him it was enough to know that the solar radiance was stolen, in the one case as in the other, and to suspect that the same demon was to blame for both robberies.^[65]

Viewing

2017 total solar eclipse viewed in real time with audience reactions

Looking directly at the

blindness. The retina has no sensitivity to pain, and the effects of retinal damage may not appear for hours, so there is no warning that injury is occurring.^[66][67]

Under normal conditions, the Sun is so bright that it is difficult to stare at it directly. However, during an eclipse, with so much of the Sun covered, it is easier and more tempting to stare at it. Looking at the Sun during an eclipse is as dangerous as looking at it outside an eclipse, except during the brief period of totality, when the Sun's disk is completely covered (totality occurs only during a total eclipse and only very briefly; it does not occur during a partial or annular eclipse). Viewing the Sun's disk through any kind of optical aid (binoculars, a telescope, or even an optical camera viewfinder) is extremely hazardous and can cause irreversible eye damage within a fraction of a second.[68]^[69]

Partial and annular eclipses

Pinhole projection method of observing partial solar eclipse. Insert (upper left): partially eclipsed Sun photographed with a white solar filter. Main image: projections of the partially eclipsed Sun (bottom right)

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.

Compact Disc, a black colour slide film, smoked glass, etc. must be avoided.^[71][72]

The safest way to view the Sun's disk is by indirect projection.[73] This can be done by projecting an image of the disk onto a white piece of paper or card using a pair of binoculars (with one of the lenses covered), a telescope, or another piece of cardboard with a small hole in it (about 1 mm diameter), often called a pinhole camera. The projected image of the Sun can then be safely viewed; this technique can be used to observe sunspots, as well as eclipses. Care must be taken, however, to ensure that no one looks through the projector (telescope, pinhole, etc.) directly.^[74] Viewing the Sun's disk on a video display screen (provided by a video camera or digital camera) is safe, although the camera itself may be damaged by direct exposure to the Sun. The optical viewfinders provided with some video and digital cameras are not safe. Securely mounting #14 welder's glass in front of the lens and viewfinder protects the equipment and makes viewing possible.^[72] Professional workmanship is essential because of the dire consequences any gaps or detaching mountings will have. In the partial eclipse path, one will not be able to see the corona or nearly complete darkening of the sky. 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.^[75]

Totality

corona, prominences

, and diamond ring effect

A dedicated group of eclipse chasers have pursued the observation of solar eclipses when they occur around the Earth.^[77] A person who chases eclipses is known as an umbraphile, meaning shadow lover.^[78] Umbraphiles travel for eclipses and use various tools to help view the sun including solar viewing glasses, also known as eclipse glasses, as well as telescopes.^[79][80]

Photography

The progression of a solar eclipse on August 1, 2008 in Novosibirsk, Russia

. All times UTC (local time was UTC+7). The time span between shots is three minutes.

Pinholes in shadows during no eclipse (1 & 4), a partial eclipse (2 & 5) and an annular eclipse (3 & 6)

As the light filters through leaves of trees during a partial eclipse, the overlapping leaves create natural pinholes, displaying mini eclipses on the ground.[84]

Phenomena associated with eclipses include shadow bands (also known as flying shadows), which are similar to shadows on the bottom of a swimming pool. They occur only just prior to and after totality, when a narrow solar crescent acts as an anisotropic light source.^[85]

1919 observations

Eddington's original photograph of the 1919 eclipse, which provided evidence for Einstein's theory of general relativity

.

The observation of a total solar eclipse of May 29, 1919, helped to confirm Einstein's theory of general relativity. By comparing the apparent distance between stars in the constellation Taurus, with and without the Sun between them, Arthur Eddington stated that the theoretical predictions about gravitational lenses were confirmed.^[86] The observation with the Sun between the stars was possible only during totality since the stars are then visible. Though Eddington's observations were near the experimental limits of accuracy at the time, work in the later half of the 20th century confirmed his results.^[87][88]

Gravity anomalies

There is a long history of observations of gravity-related phenomena during solar eclipses, especially during the period of totality. In 1954, and again in 1959, Maurice Allais reported observations of strange and unexplained movement during solar eclipses.^[89] The reality of this phenomenon, named the Allais effect, has remained controversial. Similarly, in 1970, Saxl and Allen observed the sudden change in motion of a torsion pendulum; this phenomenon is called the Saxl effect.^[90]

Observation during the 1997 solar eclipse by Wang et al. suggested a possible gravitational shielding effect,^[91] which generated debate. In 2002, Wang and a collaborator published detailed data analysis, which suggested that the phenomenon still remains unexplained.^[92]

Eclipses and transits

In principle, the simultaneous occurrence of a solar eclipse and a transit of a planet is possible. But these events are extremely rare because of their short durations. The next anticipated simultaneous occurrence of a solar eclipse and a transit of Mercury will be on July 5, 6757, and a solar eclipse and a transit of Venus is expected on April 5, 15232.^[93]

More common, but still infrequent, is a

The Moon's shadow over Turkey and Cyprus, seen from the ISS during a 2006 total solar eclipse

.

A composite image showing the ISS transit of the Sun while the 2017 solar eclipse was in progress.

Artificial satellites can also pass in front of the Sun as seen from the Earth, but none is large enough to cause an eclipse. At the altitude of the International Space Station, for example, an object would need to be about 3.35 km (2.08 mi) across to blot the Sun out entirely. These transits are difficult to watch because the zone of visibility is very small. The satellite passes over the face of the Sun in about a second, typically. As with a transit of a planet, it will not get dark.^[95]

Observations of eclipses from spacecraft or artificial satellites orbiting above the Earth's atmosphere are not subject to weather conditions. The crew of Gemini 12 observed a total solar eclipse from space in 1966.^[96] The partial phase of the 1999 total eclipse was visible from Mir.^[97]

Impact

The

Eclipses may cause the temperature to decrease by 3 °C, with wind power potentially decreasing as winds are reduced by 0.7 m/s.^[100]

In addition to the drop in light level and air temperature, animals change their behavior during totality. For example, birds and squirrels return to their nests and crickets chirp.^[101]

Recent and forthcoming solar eclipses

Eclipse path for total and hybrid eclipses from 2021 to 2040.

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[102]

Solar eclipse series sets from 1997–2000

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
120 Chita, Russia	Total	0.91830		125	Partial (south)	-1.03521
130 Total eclipse near Guadeloupe	Total	0.23909		135	Annular	-0.26441
140	Annular	-0.47260		145 Totality from France	Total	0.50623
150	Partial (south)	-1.22325		155	Partial (north)	1.21664

Partial solar eclipses on July 1, 2000 and December 25, 2000 occur in the next lunar year eclipse set.

2000–2003

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[103]

Partial solar eclipses on February 5, 2000 and July 31, 2000 occur in the previous lunar year set.

Solar eclipse series sets from 2000–2003

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
117	Partial (south)	-1.28214		122	Partial (north)	1.13669
127 Lusaka, Zambia	Total	-0.57013		132 Minneapolis, MN	Annular	0.40885
137 Los Angeles, CA	Annular	0.19933		142 Totality from Woomera	Total	-0.30204
147 Culloden, Scotland	Annular	0.99598		152	Total	-0.96381

2004–2007

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[104]

Solar eclipse series sets from 2004–2007

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
119	Partial (south)	-1.13345		124	Partial (north)	1.03481
129 Partial from Naiguatá	Hybrid	-0.34733		134 Madrid, Spain	Annular	0.33058
139 Total from Side, Turkey	Total	0.38433		144 São Paulo, Brazil	Annular	-0.40624
149 Jaipur, India	Partial (north)	1.07277		154 From Córdoba, Argentina	Partial (south)	-1.12552

2008–2011

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[105]

Solar eclipse series sets from 2008–2011

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
121 Partial from Christchurch , NZ	Annular	-0.95701		126 Novosibirsk, Russia	Total	0.83070
131 Palangka Raya , Indonesia	Annular	-0.28197		136 Kurigram , Bangladesh	Total	0.06977
141 Bangui, Central African Republic	Annular	0.40016		146 Hao, French Polynesia	Total	-0.67877
151 Vienna, Austria	Partial (north)	1.06265		156	Partial (south)	-1.49171

Partial solar eclipses on June 1, 2011, and November 25, 2011, occur on the next lunar year eclipse set.

2011–2014

This eclipse is a member of the 2011–2014 solar eclipse semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^{[106][Note 1]}

Solar eclipse series sets from 2011–2014

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
118 Partial from Tromsø, Norway	Partial (north)	1.21300		123	Partial (south)	-1.05359
128 Middlegate, Nevada	Annular	0.48279		133 Cairns , Australia	Total	-0.37189
138 Churchills Head , Australia	Annular	-0.26937		143 Libreville, Gabon	Hybrid	0.32715
148 Partial from Adelaide , Australia	Annular (non-central)	-0.99996		153 Partial from Minneapolis	Partial (north)	1.09078

2015–2018

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[107]

Solar eclipse series sets from 2015–2018

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
120 Longyearbyen , Svalbard	Total	0.94536		125 Solar Dynamics Observatory	Partial (south)	-1.10039
130 Balikpapan , Indonesia	Total	0.26092		135 L'Étang-Salé , Réunion	Annular	-0.33301
140 Partial from Buenos Aires	Annular	-0.45780		145 Casper, Wyoming	Total	0.43671
150 Partial from Olivos, Buenos Aires	Partial (south)	-1.21163		155 Partial from Huittinen , Finland	Partial (north)	1.14758

Partial solar eclipses on July 13, 2018, and January 6, 2019, occur during the next semester series.

2018–2021

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[108]

Note: Partial solar eclipses on February 15, 2018, and August 11, 2018, occurred during the previous semester series.

Solar eclipse series sets from 2018–2021

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
117 Partial from Melbourne , Australia	Partial	-1.35423		122 Partial from Nakhodka , Russia	Partial	1.14174
127 La Serena, Chile	Total	-0.64656		132 Jaffna, Sri Lanka	Annular	0.41351
137 Beigang, Yunlin , Taiwan	Annular	0.12090		142 Gorbea, Chile	Total	-0.29394
147 Halifax, Canada	Annular	0.91516		152	Total	-0.95261

2022–2025

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[109]

Solar eclipse series sets from 2022–2025

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
119 Santiago, Chile	Partial	-1.19008		124 Saratov, Russia	Partial	1.07014
129 Partial from Magetan, Indonesia	Hybrid	-0.39515		134	Annular	0.37534
139	Total	0.34314		144	Annular	-0.35087
149	Partial	1.04053		154	Partial	-1.06509

2026–2029

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.^[110]

Solar eclipse series sets from 2026–2029

Ascending node				Descending node
Saros	Map	Gamma		Saros	Map	Gamma
121	Annular	-0.97427		126	Total	0.89774
131	Annular	-0.29515		136	Total	0.14209
141	Annular	0.39014		146	Total	-0.60557
151	Partial	1.05532		156	Partial	-1.41908

Partial solar eclipses on June 12, 2029, and December 5, 2029, occur in the next lunar year eclipse set.

See also

• Lists of solar eclipses
• List of films featuring eclipses
• Apollo–Soyuz:First joint U.S.–Soviet space flight. Mission included an arranged eclipse of the Sun by the Apollo module to allow instruments on the Soyuz to take photographs of the solar corona
• Eclipse chasing: Travel to eclipse locations for study and enjoyment
• Occultation: generic term for occlusion of an object by another object that passes between it and the observer, thus revealing (for example) the presence of an exoplanet orbiting a distant star by eclipsing it as seen from the earth
• Solar eclipses in fiction
• Solar eclipses on the Moon: eclipse of the sun by planet Earth, as seen from the moon.
  • Lunar eclipse: A solar eclipse of the moon, as seen from Earth; the shadow cast on the moon by that eclipse
• Transit of Venus: passage of the planet Venus between the Sun and the Earth, as seen from Earth. Technically, a partial eclipse.
• Transit of Deimos from Mars: passage of the Martian moon Deimos between the Sun and Mars, as seen from Mars.
• Transit of Phobos from Mars: passage of the Martian moon Phobos between the Sun and Mars, as seen from Mars.

Footnotes

Notes

References

• Mucke, Hermann; Meeus, Jean (1992). Canon of Solar Eclipses −2003 to +2526 (2 ed.). Vienna: Astronomisches Büro.
• Harrington, Philip S. (1997). Eclipse! The What, Where, When, Why and How Guide to Watching Solar and Lunar Eclipses. New York: John Wiley and Sons.
  ISBN 0-471-12795-7
  .
• ISBN 0-7472-7385-5
  .
• Mobberley, Martin (2007). Total Solar Eclipses and How to Observe Them. Astronomers' Observing Guides. New York: Springer.
  ISBN 978-0-387-69827-4
  .
• ISBN 978-1-941983-02-7
  .
• Espenak, Fred (2016). 21st Century Canon of Solar Eclipses. Portal AZ: Astropixels Publishing.
  ISBN 978-1-941983-12-6
  .
• Fotheringham, John Knight (1921). Historical eclipses: being the Halley lecture delivered 17 May 1921. Oxford: Clarendon Press.

External links

Wikimedia Commons has media related to Solar eclipses.

Wikivoyage has a travel guide for Solar eclipses.

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• NASA Eclipse Web Site
• Eclipsewise, Fred Espenak's new eclipse site
• Andrew Lowe's Eclipse Page, with maps and circumstances for 5000 years of solar eclipses
• A Guide to Eclipse Activities for Educators, Explaining eclipses in educational settings
• Detailed eclipse explanations and predictions, Hermit Eclipse
• Eclipse Photography, Prof. Miroslav Druckmüller
• Animated maps of August 21, 2017 solar eclipses, Larry Koehn
• Five Millennium (−1999 to +3000) Canon of Solar Eclipses Database, Xavier M. Jubier
• Animated explanation of the mechanics of a solar eclipse Archived 2013-05-25 at the Wayback Machine, University of South Wales
• Eclipse Image Gallery Archived 2016-10-15 at the Wayback Machine, The World at Night
• Ring of Fire Eclipse: 2012, Photos
• "Sun, Eclipses of the" . Collier's New Encyclopedia. 1921.
• Centered and aligned video recording of Total Solar Eclipse 20th March 2015 on
  YouTube
• Solar eclipse photographs taken from the Lick Observatory from the Lick Observatory Records Digital Archive, UC Santa Cruz Library’s Digital Collections Archived 2020-06-05 at the Wayback Machine
• Video with Total Solar Eclipse March 09 2016 (From the Beginning to the Total Phase) on
  YouTube
• Total Solar Eclipse Shadow on Earth March 09 2016 CIMSSSatelite
• List of all solar eclipses
• National Geographic Solar Eclipse 101 video Archived 2018-08-04 at the Wayback Machine
• Wikiversity has a solar eclipse lab that students can do on any sunny day.