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May 1984 lunar eclipse
Penumbral lunar eclipse May 15, 1984 From Wikipedia, the free encyclopedia
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A penumbral lunar eclipse occurred at the Moon’s descending node of orbit on Tuesday, May 15, 1984,[1] with an umbral magnitude of −0.1759. 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 about 3 days after perigee (on May 12, 1984, at 4:05 UTC), the Moon's apparent diameter was larger.[2]
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Visibility
The eclipse was completely visible over much of North America, South America, and Antarctica, seen rising over northwestern North America and the central Pacific Ocean and setting over Africa and much of Europe.[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 1984
- A penumbral lunar eclipse on May 15.
- An annular solar eclipse on May 30.
- A penumbral lunar eclipse on June 13.
- A penumbral lunar eclipse on November 8.
- A total solar eclipse on November 22.
Metonic
- Preceded by: Lunar eclipse of July 27, 1980
- Followed by: Lunar eclipse of March 3, 1988
Tzolkinex
- Preceded by: Lunar eclipse of April 4, 1977
- Followed by: Lunar eclipse of June 27, 1991
Half-Saros
- Preceded by: Solar eclipse of May 11, 1975
- Followed by: Solar eclipse of May 21, 1993
Tritos
- Preceded by: Lunar eclipse of June 15, 1973
- Followed by: Lunar eclipse of April 15, 1995
Lunar Saros 111
- Preceded by: Lunar eclipse of May 4, 1966
- Followed by: Lunar eclipse of May 26, 2002
Inex
- Preceded by: Lunar eclipse of June 5, 1955
- Followed by: Lunar eclipse of April 25, 2013
Triad
- Preceded by: Lunar eclipse of July 14, 1897
- Followed by: Lunar eclipse of March 16, 2071
Lunar eclipses of 1984–1987
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 eclipse on June 13, 1984 occurs 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.
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Saros 111
This eclipse is a part of Saros series 111, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on June 10, 830 AD. It contains partial eclipses from September 14, 992 AD through April 8, 1335; total eclipses from April 19, 1353 through August 4, 1533; and a second set of partial eclipses from August 16, 1551 through April 23, 1948. The series ends at member 71 as a penumbral eclipse on July 19, 2092.
The longest duration of totality was produced by member 35 at 106 minutes, 14 seconds on June 12, 1443. 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 partial solar eclipses of Solar Saros 118.
| May 11, 1975 | May 21, 1993 |
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Notes
External links
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