| Total eclipse | |||||||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||||||
| Date | September 15, 1913 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.2109 | ||||||||||||||||
| Magnitude | 1.4304 | ||||||||||||||||
| Saros cycle | 126 (39 of 70) | ||||||||||||||||
| Totality | 93 minutes, 29 seconds | ||||||||||||||||
| Partiality | 230 minutes, 33 seconds | ||||||||||||||||
| Penumbral | 373 minutes, 1 second | ||||||||||||||||
| |||||||||||||||||
← March 1913 | |||||||||||||||||
A totallunar eclipse occurred at the Moon’sascending node of orbit on Monday, September 15, 1913,[1] with an umbralmagnitude of 1.4304. It was acentral lunar eclipse, in which part of theMoon passed through thecenter of theEarth's shadow. 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 only about 30 minutes afterapogee (on September 15, 1913, at 12:20 UTC), the Moon's apparent diameter was smaller.[2]
The eclipse was completely visible overnortheast Asia andAustralia, seen rising over much ofAsia andeast Africa and setting overNorth America and westernSouth 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 | 2.51225 |
| Umbral Magnitude | 1.43037 |
| Gamma | −0.21093 |
| Sun Right Ascension | 11h30m49.6s |
| Sun Declination | +03°09'08.3" |
| Sun Semi-Diameter | 15'54.6" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 23h31m11.8s |
| Moon Declination | -03°19'05.5" |
| Moon Semi-Diameter | 14'42.3" |
| Moon Equatorial Horizontal Parallax | 0°53'58.2" |
| ΔT | 15.4 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. The first and last eclipse in this sequence is separated by onesynodic month.
| August 31 Descending node (new moon) | September 15 Ascending node (full moon) | September 30 Descending node (new moon) |
|---|---|---|
 | |  |
| Partial solar eclipse Solar Saros 114 | Total lunar eclipse Lunar Saros 126 | Partial solar eclipse Solar Saros 152 |
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 onJanuary 31, 1915 andJuly 26, 1915 occur in the next lunar year eclipse set.
| Lunar eclipse series sets from 1912 to 1915 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 111 | 1912 Apr 01 | Partial | 0.9116 | 116 | 1912 Sep 26 | Partial | −0.9320 | |
| 121 | 1913 Mar 22 | Total | 0.1671 | 126 | 1913 Sep 15 | Total | −0.2109 | |
| 131 | 1914 Mar 12 | Partial | −0.5254 | 136 | 1914 Sep 04 | Partial | 0.5301 | |
| 141 | 1915 Mar 01 | Penumbral | −1.2573 | 146 | 1915 Aug 24 | Penumbral | 1.2435 | |
This eclipse is a part ofSaros series 126, repeating every 18 years, 11 days, and containing 70 events. The series started with a penumbral lunar eclipse on July 18, 1228. It contains partial eclipses from March 24, 1625 through June 9, 1751; total eclipses from June 19, 1769 throughNovember 9, 2003; and a second set of partial eclipses fromNovember 19, 2021 through June 5, 2346. The series ends at member 70 as a penumbral eclipse on August 19, 2472.
The longest duration of totality was produced by member 36 at 106 minutes, 27 seconds onAugust 13, 1859. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1859 Aug 13, lasting 106 minutes, 27 seconds.[7] | Penumbral | Partial | Total | Central |
| 1228 Jul 18 | 1625 Mar 24 | 1769 Jun 19 | 1805 Jul 11 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
1931 Sep 26 | 2003 Nov 09 | 2346 Jun 05 | 2472 Aug 19 | |
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 33–54 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 33 | 34 | 35 | |||
| 1805 Jul 11 | 1823 Jul 23 | 1841 Aug 02 | |||
| 36 | 37 | 38 | |||
| 1859 Aug 13 | 1877 Aug 23 | 1895 Sep 04 | |||
| 39 | 40 | 41 | |||
| 1913 Sep 15 | 1931 Sep 26 | 1949 Oct 07 | |||
| | |  |  |  |
| 42 | 43 | 44 | |||
| 1967 Oct 18 | 1985 Oct 28 | 2003 Nov 09 | |||
 |  |  |  | |  |
| 45 | 46 | 47 | |||
| 2021 Nov 19 | 2039 Nov 30 | 2057 Dec 11 | |||
 |  |  |  |  |  |
| 48 | 49 | 50 | |||
| 2075 Dec 22 | 2094 Jan 01 | 2112 Jan 14 | |||
| 51 | 52 | 53 | |||
| 2130 Jan 24 | 2148 Feb 04 | 2166 Feb 15 | |||
| 54 | |||||
| 2184 Feb 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 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1804 Jul 22 (Saros 116) | 1815 Jun 21 (Saros 117) | 1826 May 21 (Saros 118) | 1837 Apr 20 (Saros 119) | 1848 Mar 19 (Saros 120) | |||||
| 1859 Feb 17 (Saros 121) | 1870 Jan 17 (Saros 122) | 1880 Dec 16 (Saros 123) | 1891 Nov 16 (Saros 124) | 1902 Oct 17 (Saros 125) | |||||
 |  | ||||||||
| 1913 Sep 15 (Saros 126) | 1924 Aug 14 (Saros 127) | 1935 Jul 16 (Saros 128) | 1946 Jun 14 (Saros 129) | 1957 May 13 (Saros 130) | |||||
| |  |  |  |  |  |  |  |  |
| 1968 Apr 13 (Saros 131) | 1979 Mar 13 (Saros 132) | 1990 Feb 09 (Saros 133) | 2001 Jan 09 (Saros 134) | 2011 Dec 10 (Saros 135) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2022 Nov 08 (Saros 136) | 2033 Oct 08 (Saros 137) | 2044 Sep 07 (Saros 138) | 2055 Aug 07 (Saros 139) | 2066 Jul 07 (Saros 140) | |||||
 |  |  |  |  |  |  |  | ||
| 2077 Jun 06 (Saros 141) | 2088 May 05 (Saros 142) | 2099 Apr 05 (Saros 143) | 2110 Mar 06 (Saros 144) | 2121 Feb 02 (Saros 145) | |||||
 |  | ||||||||
| 2132 Jan 02 (Saros 146) | 2142 Dec 03 (Saros 147) | 2153 Nov 01 (Saros 148) | 2164 Sep 30 (Saros 149) | 2175 Aug 31 (Saros 150) | |||||
| 2186 Jul 31 (Saros 151) | 2197 Jun 29 (Saros 152) | ||||||||
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 | |||||
|---|---|---|---|---|---|
| 1826 Nov 14 (Saros 123) | 1855 Oct 25 (Saros 124) | 1884 Oct 04 (Saros 125) | |||
| 1913 Sep 15 (Saros 126) | 1942 Aug 26 (Saros 127) | 1971 Aug 06 (Saros 128) | |||
| |  |  |  |  |
| 2000 Jul 16 (Saros 129) | 2029 Jun 26 (Saros 130) | 2058 Jun 06 (Saros 131) | |||
 |  |  |  |  |  |
| 2087 May 17 (Saros 132) | 2116 Apr 27 (Saros 133) | 2145 Apr 07 (Saros 134) | |||
 |  | ||||
| 2174 Mar 18 (Saros 135) | |||||
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 133.
| September 9, 1904 | September 21, 1922 |
|---|---|
 |  |
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