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December 1964 lunar eclipse
Total lunar eclipse December 19, 1964 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s ascending node of orbit on Saturday, December 19, 1964,[1] with an umbral magnitude of 1.1748. 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 8.5 hours before perigee (on December 19, 1964, at 11:05 UTC), the Moon's apparent diameter was larger.[2]
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The eclipse afforded astrophysicist J. M. Saari the opportunity to make infrared pyrometric scans of the lunar surface with improved equipment, following up on Richard W. Shorthill's discovery of "hot spots" in the Tycho crater during the March 13, 1960 eclipse.[3]
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Visibility
The eclipse was completely visible over North and South America, west Africa, Europe, and north Asia, seen rising over the eastern Pacific Ocean and setting over southern and east Africa and the western half of Asia.[4]
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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.[5]
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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 1964
- A partial solar eclipse on January 14.
- A partial solar eclipse on June 10.
- A total lunar eclipse on June 25.
- A partial solar eclipse on July 9.
- A partial solar eclipse on December 4.
- A total lunar eclipse on December 19.
Metonic
- Preceded by: Lunar eclipse of March 2, 1961
- Followed by: Lunar eclipse of October 6, 1968
Tzolkinex
- Preceded by: Lunar eclipse of November 7, 1957
- Followed by: Lunar eclipse of January 30, 1972
Half-Saros
- Preceded by: Solar eclipse of December 14, 1955
- Followed by: Solar eclipse of December 24, 1973
Tritos
- Preceded by: Lunar eclipse of January 19, 1954
- Followed by: Lunar eclipse of November 18, 1975
Lunar Saros 134
- Preceded by: Lunar eclipse of December 8, 1946
- Followed by: Lunar eclipse of December 30, 1982
Inex
- Preceded by: Lunar eclipse of January 8, 1936
- Followed by: Lunar eclipse of November 29, 1993
Triad
- Preceded by: Lunar eclipse of February 17, 1878
- Followed by: Lunar eclipse of October 19, 2051
Lunar eclipses of 1962–1965
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.[6]
The penumbral lunar eclipses on February 19, 1962 and August 15, 1962 occur in the previous lunar year eclipse set.
Saros 134
This eclipse is a part of Saros series 134, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on April 1, 1550. It contains partial eclipses from July 7, 1694 through October 13, 1856; total eclipses from October 25, 1874 through July 26, 2325; and a second set of partial eclipses from August 7, 2343 through November 12, 2505. The series ends at member 72 as a penumbral eclipse on May 28, 2830.
The longest duration of totality will be produced by member 38 at 100 minutes, 23 seconds on May 22, 2217. All eclipses in this series occur at the Moon’s ascending node of orbit.[7]
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).[9] This lunar eclipse is related to two total solar eclipses of Solar Saros 141.
| December 14, 1955 | December 24, 1973 |
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See also
Notes
External links
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