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January 1954 lunar eclipse
Total lunar eclipse January 19, 1954 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Tuesday, January 19, 1954,[1] with an umbral magnitude of 1.0322. 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 6.4 days before apogee (on January 25, 1954, at 12:20 UTC), the Moon's apparent diameter was smaller.[2]
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Visibility
The eclipse was completely visible over much of North and South America, west Africa, and Europe, seen rising over western North America and the eastern Pacific Ocean and setting over southern and east Africa 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 1954
- An annular solar eclipse on January 5.
- A total lunar eclipse on January 19.
- A total solar eclipse on June 30.
- A partial lunar eclipse on July 16.
- An annular solar eclipse on December 25.
Metonic
- Preceded by: Lunar eclipse of April 2, 1950
- Followed by: Lunar eclipse of November 7, 1957
Tzolkinex
- Preceded by: Lunar eclipse of December 8, 1946
- Followed by: Lunar eclipse of March 2, 1961
Half-Saros
- Preceded by: Solar eclipse of January 14, 1945
- Followed by: Solar eclipse of January 25, 1963
Tritos
- Preceded by: Lunar eclipse of February 20, 1943
- Followed by: Lunar eclipse of December 19, 1964
Lunar Saros 133
- Preceded by: Lunar eclipse of January 8, 1936
- Followed by: Lunar eclipse of January 30, 1972
Inex
- Preceded by: Lunar eclipse of February 8, 1925
- Followed by: Lunar eclipse of December 30, 1982
Triad
- Preceded by: Lunar eclipse of March 20, 1867
- Followed by: Lunar eclipse of November 18, 2040
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 133
This eclipse is a part of Saros series 133, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on May 13, 1557. It contains partial eclipses from August 7, 1683 through December 17, 1899; total eclipses from December 28, 1917 through August 3, 2278; and a second set of partial eclipses from August 14, 2296 through March 11, 2639. The series ends at member 71 as a penumbral eclipse on June 29, 2819.
The longest duration of totality will be produced by member 35 at 101 minutes, 41 seconds on May 30, 2170. 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 140.
| January 14, 1945 | January 25, 1963 |
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See also
Notes
External links
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