Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.<ref>{{cite web|title=Total Lunar Eclipse of 1953 Jan 29|url=https://eclipsewise.com/lunar/LEprime/1901-2000/LE1953Jan29Tprime.html|publisher=EclipseWise.com|access-date=22 December 2024}}</ref>
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.<ref>{{cite web|title=Total Lunar Eclipse of 1953 Jan 29|url=https://eclipsewise.com/lunar/LEprime/1901-2000/LE1953Jan29Tprime.html|publisher=EclipseWise.com|access-date=22 December 2024}}</ref>
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|+January 29, 1953 Lunar Eclipse Parameters
|+January 29, 1953 Lunar Eclipse Parameters
! Parameter
! Parameter
Total lunar eclipse January 29, 1953
The Moon’s hourly motion shown right to left |
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| Date | January 29, 1953 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | 0.2606 | ||||||||||||||||
| Magnitude | 1.3314 | ||||||||||||||||
| Saros cycle | 123 (49 of 73) | ||||||||||||||||
| Totality | 84 minutes, 31 seconds | ||||||||||||||||
| Partiality | 225 minutes, 47 seconds | ||||||||||||||||
| Penumbral | 370 minutes, 57 seconds | ||||||||||||||||
|
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A total lunar eclipse occurred at the Moon’s descending node of orbit on Thursday, January 29, 1953,[1] with an umbral magnitude of 1.3314. It was a central lunar eclipse, in which part of the Moon passed through the center of the Earth’s shadow. 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. Occurring about 2.5 days before apogee (on February 1, 1953, at 11:46 UTC), the Moon’s apparent diameter was smaller.[2]
The eclipse was completely visible over Africa, Europe, and west and central Asia, seen rising over North and South America and setting over western Australia and much of Asia.[3]
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Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Parameter | Value |
|---|---|
| Penumbral Magnitude | 2.42906 |
| Umbral Magnitude | 1.33137 |
| Gamma | 0.26061 |
| Sun Right Ascension | 20h48m59.2s |
| Sun Declination | -17°47’59.2″ |
| Sun Semi-Diameter | 16’14.1″ |
| Sun Equatorial Horizontal Parallax | 08.9″ |
| Moon Right Ascension | 08h49m20.8s |
| Moon Declination | +18°01’09.9″ |
| Moon Semi-Diameter | 14’47.4″ |
| Moon Equatorial Horizontal Parallax | 0°54’16.9″ |
| ΔT | 30.3 s |
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.
Lunar eclipses of 1951–1955
[edit]
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.
This eclipse is a part of Saros series 123, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on August 16, 1087. It contains partial eclipses from May 2, 1520 through July 6, 1610; total eclipses from July 16, 1628 through April 4, 2061; and a second set of partial eclipses from April 16, 2079 through July 2, 2205. The series ends at member 72 as a penumbral eclipse on October 8, 2367.
The longest duration of totality was produced by member 37 at 105 minutes, 58 seconds on September 20, 1736. All eclipses in this series occur at the Moon’s descending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on 1736 Sep 20, lasting 105 minutes, 58 seconds.[7] | Penumbral | Partial | Total | Central |
| 1087 Aug 16 | 1520 May 02 | 1628 Jul 16 | 1682 Aug 18 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1953 Jan 29
|
2061 Apr 04 | 2205 Jul 02 | 2367 Oct 08 | |
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.
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.
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.
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 total solar eclipses of Solar Saros 130.
