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January 1953 lunar eclipse
Total lunar eclipse January 29, 1953 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Thursday, January 29, 1953,[1] with an umbral magnitude of 1.3314. It was a central lunar eclipse, in which part of the Moon passed through the center of the Earth's shadow. 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 2.5 days before apogee (on February 1, 1953, at 11:46 UTC), the Moon's apparent diameter was smaller.[2]
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Visibility
The eclipse was completely visible over Africa, Europe, and west and central Asia, seen rising over North and South America and setting over western Australia and much 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 1953
- A total lunar eclipse on January 29.
- A partial solar eclipse on February 14.
- A partial solar eclipse on July 11.
- A total lunar eclipse on July 26.
- A partial solar eclipse on August 9.
Metonic
- Preceded by: Lunar eclipse of April 13, 1949
- Followed by: Lunar eclipse of November 18, 1956
Tzolkinex
- Preceded by: Lunar eclipse of December 19, 1945
- Followed by: Lunar eclipse of March 13, 1960
Half-Saros
- Preceded by: Solar eclipse of January 25, 1944
- Followed by: Solar eclipse of February 5, 1962
Tritos
- Preceded by: Lunar eclipse of March 3, 1942
- Followed by: Lunar eclipse of December 30, 1963
Lunar Saros 123
- Preceded by: Lunar eclipse of January 19, 1935
- Followed by: Lunar eclipse of February 10, 1971
Inex
- Preceded by: Lunar eclipse of February 20, 1924
- Followed by: Lunar eclipse of January 9, 1982
Triad
- Preceded by: Lunar eclipse of March 31, 1866
- Followed by: Lunar eclipse of November 30, 2039
Lunar eclipses of 1951–1955
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 eclipses on March 23, 1951 and September 15, 1951 occur in the previous lunar year eclipse set, and the lunar eclipses on June 5, 1955 (penumbral) and November 29, 1955 (partial) occur in the next lunar year eclipse set.
Saros 123
This eclipse is a part of Saros series 123, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on August 16, 1087. It contains partial eclipses from May 2, 1520 through July 6, 1610; total eclipses from July 16, 1628 through April 4, 2061; and a second set of partial eclipses from April 16, 2079 through July 2, 2205. The series ends at member 72 as a penumbral eclipse on October 8, 2367.
The longest duration of totality was produced by member 37 at 105 minutes, 58 seconds on September 20, 1736. 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 total solar eclipses of Solar Saros 130.
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Notes
External links
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