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September 1960 lunar eclipse
Total lunar eclipse September 5, 1960 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Monday, September 5, 1960,[1] with an umbral magnitude of 1.4239. 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 after perigee (on September 2, 1960, at 22:20 UTC), the Moon's apparent diameter was larger.[2]
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Visibility
The eclipse was completely visible over eastern Australia, northeast Asia, and northwestern North America, seen rising over western Australia and the eastern half of Asia and setting over North and South America.[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 1960
- A total lunar eclipse on March 13.
- A partial solar eclipse on March 27.
- A total lunar eclipse on September 5.
- A partial solar eclipse on September 20.
Metonic
- Preceded by: Lunar eclipse of November 18, 1956
- Followed by: Lunar eclipse of June 25, 1964
Tzolkinex
- Preceded by: Lunar eclipse of July 26, 1953
- Followed by: Lunar eclipse of October 18, 1967
Half-Saros
- Preceded by: Solar eclipse of September 1, 1951
- Followed by: Solar eclipse of September 11, 1969
Tritos
- Preceded by: Lunar eclipse of October 7, 1949
- Followed by: Lunar eclipse of August 6, 1971
Lunar Saros 127
- Preceded by: Lunar eclipse of August 26, 1942
- Followed by: Lunar eclipse of September 16, 1978
Inex
- Preceded by: Lunar eclipse of September 26, 1931
- Followed by: Lunar eclipse of August 17, 1989
Triad
- Preceded by: Lunar eclipse of November 4, 1873
- Followed by: Lunar eclipse of July 7, 2047
Lunar eclipses of 1958–1962
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 lunar eclipses on May 3, 1958 (partial) and October 28, 1958 (penumbral) occur in the previous lunar year eclipse set, and the penumbral lunar eclipse on July 17, 1962 occurs in the next lunar year eclipse set.
Saros 127
This eclipse is a part of Saros series 127, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on July 9, 1275. It contains partial eclipses from November 4, 1473 through May 18, 1780; total eclipses from May 29, 1798 through November 9, 2068; and a second set of partial eclipses from November 20, 2086 through June 17, 2429. The series ends at member 72 as a penumbral eclipse on September 2, 2555.
The longest duration of totality was produced by member 35 at 101 minutes, 46 seconds on July 23, 1888. 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 134.
| September 1, 1951 | September 11, 1969 |
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Notes
External links
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