Penumbral lunar eclipse May 25, 1937. From Wikipedia, the free encyclopedia
A penumbral lunar eclipse occurred at the Moon’s ascending node of orbit on Tuesday, May 25, 1937,[1] with an umbral magnitude of −0.3033. 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 18 hours after apogee (on May 24, 1937, at 13:30 UTC), the Moon's apparent diameter was smaller.[2]
| Penumbral eclipse | |||||||||
The Moon's hourly motion shown right to left | |||||||||
| Date | May 25, 1937 | ||||||||
|---|---|---|---|---|---|---|---|---|---|
| Gamma | −1.1582 | ||||||||
| Magnitude | −0.3033 | ||||||||
| Saros cycle | 110 (67 of 72) | ||||||||
| Penumbral | 254 minutes, 43 seconds | ||||||||
| |||||||||
The eclipse was completely visible over much of North America, western and central South America, and Antarctica, seen rising over Australia and setting over northeastern North America, eastern South America, and west Africa.[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 | 0.76969 |
| Umbral Magnitude | −0.30327 |
| Gamma | −1.15820 |
| Sun Right Ascension | 04h06m39.7s |
| Sun Declination | +20°53'38.5" |
| Sun Semi-Diameter | 15'47.3" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 16h06m15.0s |
| Moon Declination | -21°55'55.1" |
| Moon Semi-Diameter | 14'42.9" |
| Moon Equatorial Horizontal Parallax | 0°54'00.1" |
| ΔT | 23.9 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.
| May 25 Ascending node (full moon) | June 8 Descending node (new moon) |
|---|---|
|  |
| Penumbral lunar eclipse Lunar Saros 110 | Total solar eclipse Solar Saros 136 |
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 March 23, 1940 occurs in the next lunar year eclipse set.
| Lunar eclipse series sets from 1937 to 1940 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing |
Type Chart |
Gamma | Saros | Date Viewing |
Type Chart |
Gamma | |
| 110 | 1937 May 25 |
Penumbral |
−1.1582 | 115 | 1937 Nov 18 |
Partial |
0.9421 | |
| 120 | 1938 May 14 |
Total |
−0.3994 | 125 | 1938 Nov 07 |
Total |
0.2739 | |
| 130 | 1939 May 03 |
Total |
0.3693 | 135 | 1939 Oct 28 |
Partial |
−0.4581 | |
| 140 | 1940 Apr 22 |
Penumbral |
1.0741 | 145 | 1940 Oct 16 |
Penumbral |
−1.1925 | |
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]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on 1414 Jul 03, lasting 103 minutes, 8 seconds.[7] | Penumbral | Partial | Total | Central |
| 747 May 28 |
891 Aug 23 |
1306 Apr 29 |
1360 May 31 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1468 Aug 04 |
1522 Sep 05 |
1883 Apr 22 |
2027 Jul 18 | |
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.
| Series members 60–72 occur between 1801 and 2027: | |||||
|---|---|---|---|---|---|
| 60 | 61 | 62 | |||
| 1811 Mar 10 | 1829 Mar 20 | 1847 Mar 31 | |||
| 63 | 64 | 65 | |||
| 1865 Apr 11 | 1883 Apr 22 | 1901 May 03 | |||
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| 66 | 67 | 68 | |||
| 1919 May 15 | 1937 May 25 | 1955 Jun 05 | |||
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| 69 | 70 | 71 | |||
| 1973 Jun 15 | 1991 Jun 27 | 2009 Jul 07 | |||
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| 72 | |||||
| 2027 Jul 18 | |||||
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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.
| Series members between 1817 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1817 May 01 (Saros 99) |
1828 Mar 31 (Saros 100) |
1839 Feb 28 (Saros 101) |
1850 Jan 28 (Saros 102) |
1860 Dec 28 (Saros 103) | |||||
| 1893 Sep 25 (Saros 106) |
1915 Jul 26 (Saros 108) | ||||||||
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| 1926 Jun 25 (Saros 109) |
1937 May 25 (Saros 110) |
1948 Apr 23 (Saros 111) |
1959 Mar 24 (Saros 112) |
1970 Feb 21 (Saros 113) | |||||
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| 1981 Jan 20 (Saros 114) |
1991 Dec 21 (Saros 115) |
2002 Nov 20 (Saros 116) |
2013 Oct 18 (Saros 117) |
2024 Sep 18 (Saros 118) | |||||
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| 2035 Aug 19 (Saros 119) |
2046 Jul 18 (Saros 120) |
2057 Jun 17 (Saros 121) |
2068 May 17 (Saros 122) |
2079 Apr 16 (Saros 123) | |||||
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| 2090 Mar 15 (Saros 124) |
2101 Feb 14 (Saros 125) |
2112 Jan 14 (Saros 126) |
2122 Dec 13 (Saros 127) |
2133 Nov 12 (Saros 128) | |||||
| 2144 Oct 11 (Saros 129) |
2155 Sep 11 (Saros 130) |
2166 Aug 11 (Saros 131) |
2177 Jul 11 (Saros 132) |
2188 Jun 09 (Saros 133) | |||||
| 2199 May 10 (Saros 134) | |||||||||
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 total and one partial = two solar eclipses of Solar Saros 117.
| May 19, 1928 | May 30, 1946 |
|---|---|
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