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August 1951 lunar eclipse
Penumbral lunar eclipse August 17, 1951 From Wikipedia, the free encyclopedia
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A penumbral lunar eclipse occurred at the Moon’s ascending node of orbit on Friday, August 17, 1951,[1] with an umbral magnitude of −0.8455. 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 1.9 days after perigee (on August 15, 1951, at 5:05 UTC), the Moon's apparent diameter was larger.[2]
This eclipse was the third of four penumbral lunar eclipses in 1951, with the others occurring on February 21, March 23, and September 15.
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Visibility
The eclipse was completely visible over eastern and central North America, South America, western Europe, and much of Africa, seen rising over northwestern North America and setting over Eastern Europe, east Africa, and the Middle East.[3]
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 1951
- A penumbral lunar eclipse on February 21.
- An annular solar eclipse on March 7.
- A penumbral lunar eclipse on March 23.
- A penumbral lunar eclipse on August 17.
- An annular solar eclipse on September 1.
- A penumbral lunar eclipse on September 15.
Metonic
- Followed by: Lunar eclipse of June 5, 1955
Tzolkinex
- Preceded by: Lunar eclipse of July 6, 1944
Half-Saros
- Preceded by: Solar eclipse of August 12, 1942
Tritos
- Followed by: Lunar eclipse of July 17, 1962
Lunar Saros 108
- Preceded by: Lunar eclipse of August 5, 1933
- Followed by: Lunar eclipse of August 27, 1969
Inex
- Followed by: Lunar eclipse of July 27, 1980
Triad
- Preceded by: Lunar eclipse of October 15, 1864
- Followed by: Lunar eclipse of June 17, 2038
Lunar eclipses of 1951–1955
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 March 23, 1951 and September 15, 1951 occur in the previous lunar year eclipse set, and the lunar eclipses on June 5, 1955 (penumbral) and November 29, 1955 (partial) occur in the next 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 in nearly the same location relative to the background stars.
Saros 108
This eclipse is a part of Saros series 108, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on July 8, 689 AD. It contains partial eclipses from February 9, 1050 through May 17, 1212; total eclipses from May 28, 1230 through September 23, 1428; and a second set of partial eclipses from October 5, 1446 through June 1, 1825. The series ends at member 72 as a penumbral eclipse on August 27, 1969.
The longest duration of totality was produced by member 35 at 105 minutes, 57 seconds on July 10, 1302. 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 one partial solar eclipse of Solar Saros 115.
| August 12, 1942 |
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Notes
External links
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