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May 1920 lunar eclipse
Total lunar eclipse May 3, 1920 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s ascending node of orbit on Monday, May 3, 1920,[1] with an umbral magnitude of 1.2194. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. Unlike a solar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on the night side of Earth. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon's shadow is smaller. Occurring only about 3.8 days before apogee (on May 6, 1920, at 21:00 UTC), the Moon's apparent diameter was smaller.[2]
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This lunar eclipse was the first of an almost tetrad, with the others being on October 27, 1920 (total); April 22, 1921 (total); and October 16, 1921 (partial).
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Visibility
The eclipse was completely visible over South America, west and southern Africa, western Europe, and Antarctica, seen rising over much of North America and the eastern Pacific Ocean and setting over eastern Europe, east Africa, and the western half of Asia.[3]
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Eclipse details
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[4]
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Eclipse season
This eclipse is part of an eclipse season, a period, roughly every six months, when eclipses occur. Only two (or occasionally three) eclipse seasons occur each year, and each season lasts about 35 days and repeats just short of six months (173 days) later; thus two full eclipse seasons always occur each year. Either two or three eclipses happen each eclipse season. In the sequence below, each eclipse is separated by a fortnight.
Related eclipses
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Eclipses in 1920
- A total lunar eclipse on May 3.
- A partial solar eclipse on May 18.
- A total lunar eclipse on October 27.
- A partial solar eclipse on November 10.
Metonic
- Preceded by: Lunar eclipse of July 15, 1916
- Followed by: Lunar eclipse of February 20, 1924
Tzolkinex
- Preceded by: Lunar eclipse of March 22, 1913
- Followed by: Lunar eclipse of June 15, 1927
Half-Saros
- Preceded by: Solar eclipse of April 28, 1911
- Followed by: Solar eclipse of May 9, 1929
Tritos
- Preceded by: Lunar eclipse of June 4, 1909
- Followed by: Lunar eclipse of April 2, 1931
Lunar Saros 120
- Preceded by: Lunar eclipse of April 22, 1902
- Followed by: Lunar eclipse of May 14, 1938
Inex
- Preceded by: Lunar eclipse of May 23, 1891
- Followed by: Lunar eclipse of April 13, 1949
Triad
- Preceded by: Lunar eclipse of July 2, 1833
- Followed by: Lunar eclipse of March 3, 2007
Lunar eclipses of 1919–1922
This eclipse is a member of a semester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[5]
The penumbral lunar eclipse on March 13, 1922 occurs in the next lunar year eclipse set.
Saros 120
This eclipse is a part of Saros series 120, repeating every 18 years, 11 days, and containing 83 events. The series started with a penumbral lunar eclipse on October 16, 1000. It contains partial eclipses from May 31, 1379 through August 4, 1487; total eclipses from August 14, 1505 through May 14, 1938; and a second set of partial eclipses from May 24, 1956 through July 28, 2064. The series ends at member 83 as a penumbral eclipse on April 7, 2479.
The longest duration of totality was produced by member 43 at 104 minutes, 55 seconds on January 24, 1758. All eclipses in this series occur at the Moon’s ascending node of orbit.[6]
Eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
Tritos series
This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.
Inex series
This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee). However, groupings of 3 inex cycles (≈ 87 years minus 2 months) comes close (≈ 1,151.02 anomalistic months), so eclipses are similar in these groupings.
Half-Saros cycle
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros).[8] This lunar eclipse is related to two total solar eclipses of Solar Saros 127.
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See also
Notes
External links
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