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June 1991 lunar eclipse
Penumbral lunar eclipse June 27, 1991 From Wikipedia, the free encyclopedia
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A penumbral lunar eclipse occurred at the Moon’s ascending node of orbit on Thursday, June 27, 1991,[1] with an umbral magnitude of −0.7571. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A penumbral lunar eclipse occurs when part or all of the Moon's near side passes into the Earth's penumbra. 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. Occurring only about 5 hours before apogee (on June 27, 1991, at 8:20 UTC), the Moon's apparent diameter was smaller.[2]
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This eclipse was the second of four lunar eclipses in 1991, with the others occurring on January 30 (penumbral), July 26 (penumbral), and December 21 (partial).
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Visibility
The eclipse was completely visible over eastern North America, South America, west and southern Africa, and Antarctica, seen rising over western and northern North America and the eastern Pacific Ocean and setting over Europe, east and north Africa, and the Middle East.[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. The first and last eclipse in this sequence is separated by one synodic month.
Related eclipses
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Eclipses in 1991
- An annular solar eclipse on January 15.
- A penumbral lunar eclipse on January 30.
- A penumbral lunar eclipse on June 27.
- A total solar eclipse on July 11.
- A penumbral lunar eclipse on July 26.
- A partial lunar eclipse on December 21.
Metonic
- Followed by: Lunar eclipse of April 15, 1995
Tzolkinex
- Preceded by: Lunar eclipse of May 15, 1984
- Followed by: Lunar eclipse of August 8, 1998
Half-Saros
- Preceded by: Solar eclipse of June 21, 1982
- Followed by: Solar eclipse of July 1, 2000
Tritos
- Preceded by: Lunar eclipse of July 27, 1980
- Followed by: Lunar eclipse of May 26, 2002
Lunar Saros 110
- Preceded by: Lunar eclipse of June 15, 1973
- Followed by: Lunar eclipse of July 7, 2009
Inex
- Preceded by: Lunar eclipse of July 17, 1962
- Followed by: Lunar eclipse of June 5, 2020
Triad
- Followed by: Lunar eclipse of April 27, 2078
Lunar eclipses of 1991–1994
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 January 30, 1991 and July 26, 1991 occur in the previous lunar year eclipse set.
Metonic series
The Metonic cycle repeats nearly exactly every 19 years and represents a Saros cycle plus one lunar year. Because it occurs on the same calendar date, the Earth's shadow will be in nearly the same location relative to the background stars.
Saros 110
This eclipse is a part of Saros series 110, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on May 28, 747 AD. It contains partial eclipses from August 23, 891 AD through April 18, 1288; total eclipses from April 29, 1306 through September 5, 1522; and a second set of partial eclipses from September 16, 1540 through April 22, 1883. The series ends at member 72 as a penumbral eclipse on July 18, 2027.
The longest duration of totality was produced by member 38 at 103 minutes, 8 seconds on July 3, 1414. All eclipses in this series occur at the Moon’s ascending 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 partial solar eclipses of Solar Saros 117.
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See also
References
External links
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