| Total eclipse | |||||||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||||||
| Date | January 8, 1936 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.4429 | ||||||||||||||||
| Magnitude | 1.0173 | ||||||||||||||||
| Saros cycle | 133 (22 of 71) | ||||||||||||||||
| Totality | 20 minutes, 48 seconds | ||||||||||||||||
| Partiality | 202 minutes, 31 seconds | ||||||||||||||||
| Penumbral | 342 minutes, 5 seconds | ||||||||||||||||
| |||||||||||||||||
A totallunar eclipse occurred at the Moon’sdescending node of orbit on Wednesday, January 8, 1936,[1] with an umbralmagnitude of 1.0173. A lunar eclipse occurs when theMoon moves into theEarth'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 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. 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'sshadow is smaller. Occurring about 6.2 days beforeapogee (on January 14, 1936, at 23:50 UTC), the Moon's apparent diameter was smaller.[2]
The eclipse was completely visible overeastern Europe,Asia, and westernAustralia, seen rising overAfrica andwestern Europe and setting over eastern Australia, northwesternNorth America, 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 | 2.07396 |
| Umbral Magnitude | 1.01725 |
| Gamma | −0.44288 |
| Sun Right Ascension | 19h15m02.9s |
| Sun Declination | -22°19'38.2" |
| Sun Semi-Diameter | 16'15.9" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 07h14m38.5s |
| Moon Declination | +21°55'15.9" |
| Moon Semi-Diameter | 15'23.6" |
| Moon Equatorial Horizontal Parallax | 0°56'29.6" |
| ΔT | 23.8 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.
| December 25 Ascending node (new moon) | January 8 Descending node (full moon) |
|---|---|
 | |
| Annular solar eclipse Solar Saros 121 | Total lunar eclipse Lunar Saros 133 |
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 onMarch 12, 1933 andSeptember 4, 1933 occur in the previous lunar year eclipse set.
| Lunar eclipse series sets from 1933 to 1936 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 103 | 1933 Feb 10 | Penumbral | 1.5600 | 108 | 1933 Aug 05 | Penumbral | −1.4216 | |
| 113 | 1934 Jan 30 | Partial | 0.9258 | 118 | 1934 Jul 26 | Partial | −0.6681 | |
| 123 | 1935 Jan 19 | Total | 0.2498 | 128 | 1935 Jul 16 | Total | 0.0672 | |
| 133 | 1936 Jan 08 | Total | −0.4429 | 138 | 1936 Jul 04 | Partial | 0.8642 | |
| 143 | 1936 Dec 28 | Penumbral | −1.0971 | |||||
This eclipse is a part ofSaros series 133, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on May 13, 1557. It contains partial eclipses from August 7, 1683 through December 17, 1899; total eclipses fromDecember 28, 1917 through August 3, 2278; and a second set of partial eclipses from August 14, 2296 through March 11, 2639. The series ends at member 71 as a penumbral eclipse on June 29, 2819.
The longest duration of totality will be produced by member 35 at 101 minutes, 41 seconds onMay 30, 2170. All eclipses in this series occur at the Moon’sdescending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series will occur on2170 May 30, lasting 101 minutes, 41 seconds.[7] | Penumbral | Partial | Total | Central |
| 1557 May 13 | 1683 Aug 07 | 1917 Dec 28 | 2098 Apr 15 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 2224 Jul 01 | 2278 Aug 03 | 2639 Mar 11 | 2819 Jun 29 | |
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 15–36 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 15 | 16 | 17 | |||
| 1809 Oct 23 | 1827 Nov 03 | 1845 Nov 14 | |||
| 18 | 19 | 20 | |||
| 1863 Nov 25 | 1881 Dec 05 | 1899 Dec 17 | |||
| 21 | 22 | 23 | |||
| 1917 Dec 28 | 1936 Jan 08 | 1954 Jan 19 | |||
|  | | |  |  |
| 24 | 25 | 26 | |||
| 1972 Jan 30 | 1990 Feb 09 | 2008 Feb 21 | |||
 |  |  |  |  |  |
| 27 | 28 | 29 | |||
| 2026 Mar 03 | 2044 Mar 13 | 2062 Mar 25 | |||
 |  |  |  | ||
| 30 | 31 | 32 | |||
| 2080 Apr 04 | 2098 Apr 15 | 2116 Apr 27 | |||
 |  | |  | ||
| 33 | 34 | 35 | |||
| 2134 May 08 | 2152 May 18 | 2170 May 30 | |||
| 36 | |||||
| 2188 Jun 09 | |||||
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 2187 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1805 Jan 15 (Saros 121) | 1815 Dec 16 (Saros 122) | 1826 Nov 14 (Saros 123) | 1837 Oct 13 (Saros 124) | 1848 Sep 13 (Saros 125) | |||||
| 1859 Aug 13 (Saros 126) | 1870 Jul 12 (Saros 127) | 1881 Jun 12 (Saros 128) | 1892 May 11 (Saros 129) | 1903 Apr 12 (Saros 130) | |||||
 |  | ||||||||
| 1914 Mar 12 (Saros 131) | 1925 Feb 08 (Saros 132) | 1936 Jan 08 (Saros 133) | 1946 Dec 08 (Saros 134) | 1957 Nov 07 (Saros 135) | |||||
 |  |  |  | | |  |  |  |  |
| 1968 Oct 06 (Saros 136) | 1979 Sep 06 (Saros 137) | 1990 Aug 06 (Saros 138) | 2001 Jul 05 (Saros 139) | 2012 Jun 04 (Saros 140) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2023 May 05 (Saros 141) | 2034 Apr 03 (Saros 142) | 2045 Mar 03 (Saros 143) | 2056 Feb 01 (Saros 144) | 2066 Dec 31 (Saros 145) | |||||
 |  |  |  |  |  |  |  | ||
| 2077 Nov 29 (Saros 146) | 2088 Oct 30 (Saros 147) | 2099 Sep 29 (Saros 148) | 2110 Aug 29 (Saros 149) | 2121 Jul 30 (Saros 150) | |||||
 |  | ||||||||
| 2132 Jun 28 (Saros 151) | 2143 May 28 (Saros 152) | 2154 Apr 28 (Saros 153) | |||||||
| 2187 Jan 24 (Saros 156) | |||||||||
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 | |||||
|---|---|---|---|---|---|
| 1820 Mar 29 (Saros 129) | 1849 Mar 09 (Saros 130) | 1878 Feb 17 (Saros 131) | |||
| 1907 Jan 29 (Saros 132) | 1936 Jan 08 (Saros 133) | 1964 Dec 19 (Saros 134) | |||
 |  | | |  |  |
| 1993 Nov 29 (Saros 135) | 2022 Nov 08 (Saros 136) | 2051 Oct 19 (Saros 137) | |||
 |  |  |  |  |  |
| 2080 Sep 29 (Saros 138) | 2109 Sep 09 (Saros 139) | 2138 Aug 20 (Saros 140) | |||
| 2167 Aug 01 (Saros 141) | 2196 Jul 10 (Saros 142) | ||||
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 140.
| January 3, 1927 | January 14, 1945 |
|---|---|
 |  |
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