| Partial eclipse | |||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||
| Date | March 13, 1941 | ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.8437 | ||||||||||||
| Magnitude | 0.3226 | ||||||||||||
| Saros cycle | 112 (61 of 72) | ||||||||||||
| Partiality | 119 minutes, 46 seconds | ||||||||||||
| Penumbral | 272 minutes, 11 seconds | ||||||||||||
| |||||||||||||
A partiallunar eclipse occurred at the Moon’sascending node of orbit on Thursday, March 13, 1941,[1] with an umbralmagnitude of 0.3226. A lunar eclipse occurs when theMoon moves into theEarth's shadow, causing the Moon to be darkened. A partial lunar eclipse occurs when one part of the Moon is in the Earth's umbra, while the other part is in the Earth's penumbra. Unlike asolar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on thenight side of Earth. Occurring about 1.5 days beforeperigee (on March 14, 1941, at 23:05 UTC), the Moon's apparent diameter was larger.[2]
The eclipse was completely visible overnortheast Asia, easternAustralia, and westernNorth America, seen rising over much ofAsia and western Australia and setting over much of North andSouth America.[3]
 |
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 | 1.29706 |
| Umbral Magnitude | 0.32264 |
| Gamma | −0.84368 |
| Sun Right Ascension | 23h32m32.0s |
| Sun Declination | -02°58'04.6" |
| Sun Semi-Diameter | 16'05.3" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 11h31m29.9s |
| Moon Declination | +02°09'22.2" |
| Moon Semi-Diameter | 16'30.6" |
| Moon Equatorial Horizontal Parallax | 1°00'35.5" |
| ΔT | 24.9 s |
This eclipse is part of aneclipse 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 afortnight.
| March 13 Ascending node (full moon) | March 27 Descending node (new moon) |
|---|---|
|  |
| Partial lunar eclipse Lunar Saros 112 | Annular solar eclipse Solar Saros 138 |
This eclipse is a member of asemester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternatingnodes of the Moon's orbit.[5]
The penumbral lunar eclipses onApril 22, 1940 andOctober 16, 1940 occur in the previous lunar year eclipse set, and the penumbral lunar eclipses onJuly 6, 1944 andDecember 29, 1944 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 1940 to 1944 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 102 | 1940 Mar 23 | Penumbral | −1.5034 | 107 | ||||
| 112 | 1941 Mar 13 | Partial | −0.8437 | 117 | 1941 Sep 05 | Partial | 0.9747 | |
| 122 | 1942 Mar 03 | Total | −0.1545 | 127 | 1942 Aug 26 | Total | 0.1818 | |
| 132 | 1943 Feb 20 | Partial | 0.5752 | 137 | 1943 Aug 15 | Partial | −0.5534 | |
| 142 | 1944 Feb 09 | Penumbral | 1.2698 | 147 | 1944 Aug 04 | Penumbral | −1.2843 | |
This eclipse is a part ofSaros series 112, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on May 20, 859 AD. It contains partial eclipses from August 3, 985 AD through March 8, 1346; total eclipses from March 18, 1364 through August 27, 1616; and a second set of partial eclipses from September 7, 1634 throughApril 25, 2013. The series ends at member 72 as a penumbral eclipse onJuly 12, 2139.
The longest duration of totality was produced by member 36 at 99 minutes, 51 seconds on June 2, 1490. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1490 Jun 02, lasting 99 minutes, 51 seconds.[7] | Penumbral | Partial | Total | Central |
| 859 May 20 | 985 Aug 03 | 1364 Mar 18 | 1436 Apr 30 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1562 Jul 16 | 1616 Aug 27 | 2013 Apr 25 | 2139 Jul 12 | |
Eclipses are tabulated in three columns; every third eclipse in the same column is oneexeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
| Series members 54–72 occur between 1801 and 2139: | |||||
|---|---|---|---|---|---|
| 54 | 55 | 56 | |||
| 1814 Dec 26 | 1833 Jan 06 | 1851 Jan 17 | |||
| 57 | 58 | 59 | |||
| 1869 Jan 28 | 1887 Feb 08 | 1905 Feb 19 | |||
 |  | ||||
| 60 | 61 | 62 | |||
| 1923 Mar 03 | 1941 Mar 13 | 1959 Mar 24 | |||
 |  | | |  |  |
| 63 | 64 | 65 | |||
| 1977 Apr 04 | 1995 Apr 15 | 2013 Apr 25 | |||
 |  |  |  | |  |
| 66 | 67 | 68 | |||
| 2031 May 07 | 2049 May 17 | 2067 May 28 | |||
 |  |  |  |  |  |
| 69 | 70 | 71 | |||
| 2085 Jun 08 | 2103 Jun 20 | 2121 Jun 30 | |||
| 72 | |||||
| 2139 Jul 12 | |||||
This eclipse is a part of atritos cycle, repeating at alternating nodes every 135synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic 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 1801 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1810 Mar 21 (Saros 100) | 1821 Feb 17 (Saros 101) | 1832 Jan 17 (Saros 102) | 1842 Dec 17 (Saros 103) | ||||||
| 1864 Oct 15 (Saros 105) | 1875 Sep 15 (Saros 106) | 1886 Aug 14 (Saros 107) | 1897 Jul 14 (Saros 108) | 1908 Jun 14 (Saros 109) | |||||
 |  | ||||||||
| 1919 May 15 (Saros 110) | 1930 Apr 13 (Saros 111) | 1941 Mar 13 (Saros 112) | 1952 Feb 11 (Saros 113) | 1963 Jan 09 (Saros 114) | |||||
 |  |  |  | | |  |  |  |  |
| 1973 Dec 10 (Saros 115) | 1984 Nov 08 (Saros 116) | 1995 Oct 08 (Saros 117) | 2006 Sep 07 (Saros 118) | 2017 Aug 07 (Saros 119) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2028 Jul 06 (Saros 120) | 2039 Jun 06 (Saros 121) | 2050 May 06 (Saros 122) | 2061 Apr 04 (Saros 123) | 2072 Mar 04 (Saros 124) | |||||
 |  |  |  |  |  | ||||
| 2083 Feb 02 (Saros 125) | 2094 Jan 01 (Saros 126) | 2104 Dec 02 (Saros 127) | 2115 Nov 02 (Saros 128) | 2126 Oct 01 (Saros 129) | |||||
| 2137 Aug 30 (Saros 130) | 2148 Jul 31 (Saros 131) | 2159 Jun 30 (Saros 132) | 2170 May 30 (Saros 133) | 2181 Apr 29 (Saros 134) | |||||
| 2192 Mar 28 (Saros 135) | |||||||||
This eclipse is a part of the long periodinex cycle, repeating at alternating nodes, every 358synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic 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.
| Series members between 1801 and 2200 | |||||
|---|---|---|---|---|---|
| 1825 Jun 01 (Saros 108) | 1854 May 12 (Saros 109) | 1883 Apr 22 (Saros 110) | |||
| 1912 Apr 01 (Saros 111) | 1941 Mar 13 (Saros 112) | 1970 Feb 21 (Saros 113) | |||
 |  | | |  |  |
| 1999 Jan 31 (Saros 114) | 2028 Jan 12 (Saros 115) | 2056 Dec 22 (Saros 116) | |||
 |  |  |  |  |  |
| 2085 Dec 01 (Saros 117) | 2114 Nov 12 (Saros 118) | 2143 Oct 23 (Saros 119) | |||
| 2172 Oct 02 (Saros 120) | |||||
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (ahalf saros).[8] This lunar eclipse is related to two annular solar eclipses ofSolar Saros 119.
| March 7, 1932 | March 18, 1950 |
|---|---|
 |  |
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