| Partial eclipse | |||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||
| Date | September 5, 1941 | ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | 0.9747 | ||||||||||||
| Magnitude | 0.0511 | ||||||||||||
| Saros cycle | 117 (48 of 72) | ||||||||||||
| Partiality | 53 minutes, 21 seconds | ||||||||||||
| Penumbral | 279 minutes, 17 seconds | ||||||||||||
| |||||||||||||
A partiallunar eclipse occurred at the Moon’sdescending node of orbit on Friday, September 5, 1941,[1] with an umbralmagnitude of 0.0511. 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 5.9 days beforeapogee (on September 11, 1941, at 14:15 UTC), the Moon's apparent diameter was smaller.[2]
The eclipse was completely visible over much ofAsia,Australia, andAntarctica, seen rising overAfrica andEurope and setting overnortheast Asia and the centralPacific Ocean.[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 | 1.08839 |
| Umbral Magnitude | 0.05110 |
| Gamma | 0.97469 |
| Sun Right Ascension | 10h56m24.2s |
| Sun Declination | +06°46'29.9" |
| Sun Semi-Diameter | 15'52.1" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 22h55m20.3s |
| Moon Declination | -05°54'07.9" |
| Moon Semi-Diameter | 15'17.9" |
| Moon Equatorial Horizontal Parallax | 0°56'08.6" |
| ΔT | 25.2 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.
| September 5 Descending node (full moon) | September 21 Ascending node (new moon) |
|---|---|
|  |
| Partial lunar eclipse Lunar Saros 117 | Total solar eclipse Solar Saros 143 |
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 117, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on April 3, 1094. It contains partial eclipses from June 29, 1238 through September 23, 1382; total eclipses from October 3, 1400 through June 21, 1815; and a second set of partial eclipses from July 2, 1833 throughSeptember 5, 1941. The series ends at member 71 as a penumbral eclipse on May 15, 2356.
The longest duration of totality was produced by member 35 at 105 minutes, 43 seconds on April 17, 1707. All eclipses in this series occur at the Moon’sdescending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1707 Apr 17, lasting 105 minutes, 43 seconds.[7] | Penumbral | Partial | Total | Central |
| 1094 Apr 03 | 1238 Jun 29 | 1400 Oct 03 | 1563 Jan 09 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1761 May 18 | 1815 Jun 21 | 1941 Sep 05 | 2356 May 15 | |
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 41–62 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 41 | 42 | 43 | |||
| 1815 Jun 21 | 1833 Jul 02 | 1851 Jul 13 | |||
| 44 | 45 | 46 | |||
| 1869 Jul 23 | 1887 Aug 03 | 1905 Aug 15 | |||
 |  | ||||
| 47 | 48 | 49 | |||
| 1923 Aug 26 | 1941 Sep 05 | 1959 Sep 17 | |||
 |  | | |  |  |
| 50 | 51 | 52 | |||
| 1977 Sep 27 | 1995 Oct 08 | 2013 Oct 18 | |||
 |  |  |  |  |  |
| 53 | 54 | 55 | |||
| 2031 Oct 30 | 2049 Nov 09 | 2067 Nov 21 | |||
 |  |  |  |  |  |
| 56 | 57 | 58 | |||
| 2085 Dec 01 | 2103 Dec 13 | 2121 Dec 24 | |||
| 59 | 60 | 61 | |||
| 2140 Jan 04 | 2158 Jan 14 | 2176 Jan 26 | |||
| 62 | |||||
| 2194 Feb 05 | |||||
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 Sep 13 (Saros 105) | 1821 Aug 13 (Saros 106) | 1832 Jul 12 (Saros 107) | 1843 Jun 12 (Saros 108) | 1854 May 12 (Saros 109) | |||||
| 1865 Apr 11 (Saros 110) | 1876 Mar 10 (Saros 111) | 1887 Feb 08 (Saros 112) | 1898 Jan 08 (Saros 113) | 1908 Dec 07 (Saros 114) | |||||
 |  | ||||||||
| 1919 Nov 07 (Saros 115) | 1930 Oct 07 (Saros 116) | 1941 Sep 05 (Saros 117) | 1952 Aug 05 (Saros 118) | 1963 Jul 06 (Saros 119) | |||||
 |  |  |  | | |  |  |  |  |
| 1974 Jun 04 (Saros 120) | 1985 May 04 (Saros 121) | 1996 Apr 04 (Saros 122) | 2007 Mar 03 (Saros 123) | 2018 Jan 31 (Saros 124) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2028 Dec 31 (Saros 125) | 2039 Nov 30 (Saros 126) | 2050 Oct 30 (Saros 127) | 2061 Sep 29 (Saros 128) | 2072 Aug 28 (Saros 129) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2083 Jul 29 (Saros 130) | 2094 Jun 28 (Saros 131) | 2105 May 28 (Saros 132) | 2116 Apr 27 (Saros 133) | 2127 Mar 28 (Saros 134) | |||||
 |  |  |  | ||||||
| 2138 Feb 24 (Saros 135) | 2149 Jan 23 (Saros 136) | 2159 Dec 24 (Saros 137) | 2170 Nov 23 (Saros 138) | 2181 Oct 22 (Saros 139) | |||||
| 2192 Sep 21 (Saros 140) | |||||||||
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 Nov 25 (Saros 113) | 1854 Nov 04 (Saros 114) | 1883 Oct 16 (Saros 115) | |||
| 1912 Sep 26 (Saros 116) | 1941 Sep 05 (Saros 117) | 1970 Aug 17 (Saros 118) | |||
 |  | | |  |  |
| 1999 Jul 28 (Saros 119) | 2028 Jul 06 (Saros 120) | 2057 Jun 17 (Saros 121) | |||
 |  |  |  |  |  |
| 2086 May 28 (Saros 122) | 2115 May 08 (Saros 123) | 2144 Apr 18 (Saros 124) | |||
| 2173 Mar 29 (Saros 125) | |||||
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 total solar eclipses ofSolar Saros 124.
| August 31, 1932 | September 12, 1950 |
|---|---|
 |  |
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