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Solar eclipse of November 23, 1965
20th-century annular solar eclipse From Wikipedia, the free encyclopedia
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An annular solar eclipse occurred at the Moon's descending node of orbit on Tuesday, November 23, 1965,[1] with a magnitude of 0.9656. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring about 6.3 days before apogee (on November 29, 1965, at 12:00 UTC), the Moon's apparent diameter was smaller.[2]
Annularity was visible from the Soviet Union (today's eastern Turkmenistan, southern Uzbekistan and southwestern Tajikistan), Afghanistan, West Pakistan, India, China, Nepal (including the capital city Kathmandu), southwestern Sikkim (now merged with India), East Pakistan (today's Bangladesh), Union of Burma (today's Myanmar), southwestern tip of Sainyabuli Province in Laos, Cambodia, South Vietnam (now belonging to Vietnam), Spratly Islands, Brunei, Malaysia, Indonesia, the Territory of Papua New Guinea (today's Papua New Guinea), and Gilbert and Ellice Islands (the part now belonging to Kiribati). 8 of the 14 eight-thousanders—Dhaulagiri, Annapurna, Manaslu, Shishapangma, Cho Oyu, Everest, Lhotse and Makalu, as well as the highest peak of Oceania, Puncak Jaya, lie in the path of annularity. A partial eclipse was visible for most of Asia, Australia, and Oceania.
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Observation
An observation team of the Lockheed Corporation and the United States Air Force observed the annular eclipse near Chiang Mai, Thailand's second largest city. They calculated the relationship between the angular diameters of the moon and the sun during annularity, and the flattening of the moon based on the results.[3]
Eclipse details
Summarize
Perspective
Shown below are two tables displaying details about this particular solar eclipse. The first table outlines times at which the moon's penumbra or umbra attains the specific parameter, and the second table describes various other 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
Eclipses in 1965
- A total solar eclipse on May 30.
- A partial lunar eclipse on June 14.
- An annular solar eclipse on November 23.
- A penumbral lunar eclipse on December 8.
Metonic
- Preceded by: Solar eclipse of February 5, 1962
- Followed by: Solar eclipse of September 11, 1969
Tzolkinex
- Preceded by: Solar eclipse of October 12, 1958
- Followed by: Solar eclipse of January 4, 1973
Half-Saros
- Preceded by: Lunar eclipse of November 18, 1956
- Followed by: Lunar eclipse of November 29, 1974
Tritos
- Preceded by: Solar eclipse of December 25, 1954
- Followed by: Solar eclipse of October 23, 1976
Solar Saros 132
- Preceded by: Solar eclipse of November 12, 1947
- Followed by: Solar eclipse of December 4, 1983
Inex
- Preceded by: Solar eclipse of December 13, 1936
- Followed by: Solar eclipse of November 3, 1994
Triad
- Preceded by: Solar eclipse of January 22, 1879
- Followed by: Solar eclipse of September 22, 2052
Solar eclipses of 1964–1967
This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[5]
The partial solar eclipses on January 14, 1964 and July 9, 1964 occur in the previous lunar year eclipse set.
Saros 132
This eclipse is a part of Saros series 132, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on August 13, 1208. It contains annular eclipses from March 17, 1569 through March 12, 2146; hybrid eclipses on March 23, 2164 and April 3, 2182; and total eclipses from April 14, 2200 through June 19, 2308. The series ends at member 71 as a partial eclipse on September 25, 2470. Its 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.
The longest duration of annularity was produced by member 25 at 6 minutes, 56 seconds on May 9, 1641, and the longest duration of totality will be produced by member 61 at 2 minutes, 14 seconds on June 8, 2290. All eclipses in this series occur at the Moon’s descending node of orbit.[6]
Metonic series
The metonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition, the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days). All eclipses in this table occur at the Moon's descending node.
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.
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Notes
References
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