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November 1956 lunar eclipse
Total lunar eclipse November 18, 1956 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Sunday, November 18, 1956,[1] with an umbral magnitude of 1.3172. 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 about 3.4 days before perigee (on November 21, 1956, at 16:45 UTC), the Moon's apparent diameter was larger.[2]
This lunar eclipse was the second of an almost tetrad, with the others being on May 24, 1956 (partial); May 13, 1957 (total); and November 7, 1957 (total).
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Visibility
The eclipse was completely visible over North America and western South America, seen rising over northeast Asia and eastern Australia and setting over eastern South America, west and central Africa, and Europe.[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 1956
- A partial lunar eclipse on May 24.
- A total solar eclipse on June 8.
- A total lunar eclipse on November 18.
- A partial solar eclipse on December 2.
Metonic
- Preceded by: Lunar eclipse of January 29, 1953
- Followed by: Lunar eclipse of September 5, 1960
Tzolkinex
- Preceded by: Lunar eclipse of October 7, 1949
- Followed by: Lunar eclipse of December 30, 1963
Half-Saros
- Preceded by: Solar eclipse of November 12, 1947
- Followed by: Solar eclipse of November 23, 1965
Tritos
- Preceded by: Lunar eclipse of December 19, 1945
- Followed by: Lunar eclipse of October 18, 1967
Lunar Saros 125
- Preceded by: Lunar eclipse of November 7, 1938
- Followed by: Lunar eclipse of November 29, 1974
Inex
- Preceded by: Lunar eclipse of December 8, 1927
- Followed by: Lunar eclipse of October 28, 1985
Triad
- Preceded by: Lunar eclipse of January 17, 1870
- Followed by: Lunar eclipse of September 19, 2043
Lunar eclipses of 1955–1958
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 January 8, 1955 occurs in the previous lunar year eclipse set, and the penumbral lunar eclipse on April 4, 1958 occurs in the next lunar year eclipse set.
Saros 125
This eclipse is a part of Saros series 125, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on July 17, 1163. It contains partial eclipses from January 17, 1470 through June 6, 1686; total eclipses from June 17, 1704 through March 19, 2155; and a second set of partial eclipses from March 29, 2173 through June 25, 2317. The series ends at member 72 as a penumbral eclipse on September 9, 2443.
The longest duration of totality was produced by member 37 at 100 minutes, 23 seconds on August 22, 1812. All eclipses in this series occur at the Moon’s descending 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 annular solar eclipses of Solar Saros 132.
| November 12, 1947 | November 23, 1965 |
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See also
Notes
External links
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