| Partial eclipse | |||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||
| Date | July 26, 1934 | ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.6681 | ||||||||||||
| Magnitude | 0.6612 | ||||||||||||
| Saros cycle | 118 (47 of 74) | ||||||||||||
| Partiality | 160 minutes, 49 seconds | ||||||||||||
| Penumbral | 285 minutes, 41 seconds | ||||||||||||
| |||||||||||||
A partiallunar eclipse occurred at the Moon’sascending node of orbit on Thursday, July 26, 1934,[1] with an umbralmagnitude of 0.6612. 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 only about an hour afterperigee (on July 26, 1934, at 11:20 UTC), the Moon's apparent diameter was larger.[2]
The eclipse was completely visible overAustralia andAntarctica, seen rising oversouth andeast Asia and setting over much ofNorth 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 | 1.60248 |
| Umbral Magnitude | 0.66121 |
| Gamma | −0.66811 |
| Sun Right Ascension | 08h20m22.6s |
| Sun Declination | +19°32'24.6" |
| Sun Semi-Diameter | 15'44.9" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 20h21m19.0s |
| Moon Declination | -20°11'13.8" |
| Moon Semi-Diameter | 16'43.9" |
| Moon Equatorial Horizontal Parallax | 1°01'24.3" |
| 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.
| July 26 Ascending node (full moon) | August 10 Descending node (new moon) |
|---|---|
|  |
| Partial lunar eclipse Lunar Saros 118 | Annular solar eclipse Solar Saros 144 |
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 118, repeating every 18 years, 11 days, and containing 73 events. The series started with a penumbral lunar eclipse on March 2, 1105. It contains partial eclipses from June 8, 1267 through August 12, 1375; total eclipses from August 22, 1393 through June 22, 1880; and a second set of partial eclipses from July 3, 1898 throughSeptember 18, 2024. The series ends at member 73 as a penumbral eclipse on May 7, 2403.
The longest duration of totality was produced by member 37 at 99 minutes, 22 seconds on April 7, 1754. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1754 Apr 07, lasting 99 minutes, 22 seconds.[7] | Penumbral | Partial | Total | Central |
| 1105 Mar 02 | 1267 Jun 08 | 1393 Aug 22 | 1465 Oct 04 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
| 1826 May 21 | 1880 Jun 22 | 2024 Sep 18 | 2403 May 07 | |
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 40–61 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 40 | 41 | 42 | |||
| 1808 May 10 | 1826 May 21 | 1844 May 31 | |||
| 43 | 44 | 45 | |||
| 1862 Jun 12 | 1880 Jun 22 | 1898 Jul 03 | |||
| 46 | 47 | 48 | |||
| 1916 Jul 15 | 1934 Jul 26 | 1952 Aug 05 | |||
 |  | | |  |  |
| 49 | 50 | 51 | |||
| 1970 Aug 17 | 1988 Aug 27 | 2006 Sep 07 | |||
 |  |  |  |  |  |
| 52 | 53 | 54 | |||
| 2024 Sep 18 | 2042 Sep 29 | 2060 Oct 09 | |||
|  |  |  | ||
| 55 | 56 | 57 | |||
| 2078 Oct 21 | 2096 Oct 31 | 2114 Nov 12 | |||
| 58 | 59 | 60 | |||
| 2132 Nov 23 | 2150 Dec 04 | 2168 Dec 14 | |||
| 61 | |||||
| 2186 Dec 26 | |||||
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 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1803 Aug 03 (Saros 106) | 1814 Jul 02 (Saros 107) | 1825 Jun 01 (Saros 108) | 1836 May 01 (Saros 109) | 1847 Mar 31 (Saros 110) | |||||
| 1858 Feb 27 (Saros 111) | 1869 Jan 28 (Saros 112) | 1879 Dec 28 (Saros 113) | 1890 Nov 26 (Saros 114) | 1901 Oct 27 (Saros 115) | |||||
 |  | ||||||||
| 1912 Sep 26 (Saros 116) | 1923 Aug 26 (Saros 117) | 1934 Jul 26 (Saros 118) | 1945 Jun 25 (Saros 119) | 1956 May 24 (Saros 120) | |||||
 |  |  |  | | |  |  |  |  |
| 1967 Apr 24 (Saros 121) | 1978 Mar 24 (Saros 122) | 1989 Feb 20 (Saros 123) | 2000 Jan 21 (Saros 124) | 2010 Dec 21 (Saros 125) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2021 Nov 19 (Saros 126) | 2032 Oct 18 (Saros 127) | 2043 Sep 19 (Saros 128) | 2054 Aug 18 (Saros 129) | 2065 Jul 17 (Saros 130) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2076 Jun 17 (Saros 131) | 2087 May 17 (Saros 132) | 2098 Apr 15 (Saros 133) | 2109 Mar 17 (Saros 134) | 2120 Feb 14 (Saros 135) | |||||
 |  |  |  |  |  | ||||
| 2131 Jan 13 (Saros 136) | 2141 Dec 13 (Saros 137) | 2152 Nov 12 (Saros 138) | 2163 Oct 12 (Saros 139) | 2174 Sep 11 (Saros 140) | |||||
| 2185 Aug 11 (Saros 141) | 2196 Jul 10 (Saros 142) | ||||||||
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 | |||||
|---|---|---|---|---|---|
| 1818 Oct 14 (Saros 114) | 1847 Sep 24 (Saros 115) | 1876 Sep 03 (Saros 116) | |||
| 1905 Aug 15 (Saros 117) | 1934 Jul 26 (Saros 118) | 1963 Jul 06 (Saros 119) | |||
 |  | | |  |  |
| 1992 Jun 15 (Saros 120) | 2021 May 26 (Saros 121) | 2050 May 06 (Saros 122) | |||
 |  |  |  |  |  |
| 2079 Apr 16 (Saros 123) | 2108 Mar 27 (Saros 124) | 2137 Mar 07 (Saros 125) | |||
| 2166 Feb 15 (Saros 126) | 2195 Jan 26 (Saros 127) | ||||
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 125.
| July 20, 1925 | August 1, 1943 |
|---|---|
 |  |
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