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February 1990 lunar eclipse
Total lunar eclipse February 9, 1990 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Friday, February 9, 1990,[1] with an umbral magnitude of 1.0750. 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. The Moon's apparent diameter will be near the average diameter because it will occur 7.7 days after perigee (on February 2, 1990, at 2:40 UTC) and 6.75 days before apogee (on February 16, 1990, at 13:05 UTC).[2]
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Visibility
The eclipse was completely visible over east Africa, eastern Europe, and Asia, seen rising over northeastern North America, eastern South America, western Europe and west and central Africa and setting over Australia, northwestern North America, and the western and central Pacific Ocean.[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 1990
- An annular solar eclipse on January 26.
- A total lunar eclipse on February 9.
- A total solar eclipse on July 22.
- A partial lunar eclipse on August 6.
Metonic
- Preceded by: Lunar eclipse of April 24, 1986
- Followed by: Lunar eclipse of November 29, 1993
Tzolkinex
- Preceded by: Lunar eclipse of December 30, 1982
- Followed by: Lunar eclipse of March 24, 1997
Half-Saros
- Preceded by: Solar eclipse of February 4, 1981
- Followed by: Solar eclipse of February 16, 1999
Tritos
- Preceded by: Lunar eclipse of March 13, 1979
- Followed by: Lunar eclipse of January 9, 2001
Lunar Saros 133
- Preceded by: Lunar eclipse of January 30, 1972
- Followed by: Lunar eclipse of February 21, 2008
Inex
- Preceded by: Lunar eclipse of March 2, 1961
- Followed by: Lunar eclipse of January 21, 2019
Triad
- Preceded by: Lunar eclipse of April 12, 1903
- Followed by: Lunar eclipse of December 10, 2076
Lunar eclipses of 1988–1991
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 June 27, 1991 (penumbral) and December 21, 1991 (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.
| February 4, 1981 | February 16, 1999 |
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Notes
External links
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