| Partial eclipse | |
 Map | |
| Gamma | −1.1005 |
|---|---|
| Magnitude | 0.8252 |
| Maximum eclipse | |
| Coordinates | 61°00′S11°36′E / 61°S 11.6°E /-61; 11.6 |
| Times (UTC) | |
| Greatest eclipse | 4:45:49 |
| References | |
| Saros | 152 (7 of 70) |
| Catalog # (SE5000) | 9311 |
A partialsolar eclipse occurred at the Moon'sdescending node of orbit on Tuesday, September 30, 1913,[1][2][3][4][5] with amagnitude of 0.8252. Asolar eclipse occurs when theMoon passes betweenEarth and theSun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth.
A partial eclipse was visible for parts ofSouthern Africa andAntarctica.
Shown below are two tables displaying details about this particular solar eclipse. The first table outlines times at which the Moon's penumbra or umbra attains the specific parameter, and the second table describes various other parameters pertaining to this eclipse.[6]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1913 September 30 at 02:55:44.7 UTC |
| Greatest Eclipse | 1913 September 30 at 04:45:48.6 UTC |
| Ecliptic Conjunction | 1913 September 30 at 04:56:47.2 UTC |
| Equatorial Conjunction | 1913 September 30 at 05:48:14.4 UTC |
| Last Penumbral External Contact | 1913 September 30 at 06:35:28.6 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.82521 |
| Eclipse Obscuration | 0.78907 |
| Gamma | −1.10053 |
| Sun Right Ascension | 12h23m33.6s |
| Sun Declination | -02°32'57.4" |
| Sun Semi-Diameter | 15'58.5" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 12h21m23.5s |
| Moon Declination | -03°31'54.0" |
| Moon Semi-Diameter | 16'42.2" |
| Moon Equatorial Horizontal Parallax | 1°01'18.1" |
| ΔT | 15.6 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 solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternatingnodes of the Moon's orbit.[7]
The partial solar eclipse onAugust 31, 1913 occurs in the next lunar year eclipse set.
| Solar eclipse series sets from 1910 to 1913 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 117 | May 9, 1910 Total | −0.9437 | 122 | November 2, 1910 Partial | 1.0603 | |
| 127 | April 28, 1911 Total | −0.2294 | 132 | October 22, 1911 Annular | 0.3224 | |
| 137 | April 17, 1912 Hybrid | 0.528 | 142 | October 10, 1912 Total | −0.4149 | |
| 147 | April 6, 1913 Partial | 1.3147 | 152 | September 30, 1913 Partial | −1.1005 | |
This eclipse is a part ofSaros series 152, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on July 26, 1805. It contains total eclipses fromNovember 2, 1967 through September 14, 2490; hybrid eclipses from September 26, 2508 through October 17, 2544; and annular eclipses from October 29, 2562 through June 16, 2941. The series ends at member 70 as a partial eclipse on August 20, 3049. Its 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.
The longest duration of totality will be produced by member 30 at 5 minutes, 16 seconds on June 9, 2328, and the longest duration of annularity will be produced by member 53 at 5 minutes, 20 seconds on February 16, 2743. All eclipses in this series occur at the Moon’sdescending node of orbit.[8]
| Series members 1–22 occur between 1805 and 2200: | ||
|---|---|---|
| 1 | 2 | 3 |
 July 26, 1805 |  August 6, 1823 |  August 16, 1841 |
| 4 | 5 | 6 |
 August 28, 1859 |  September 7, 1877 |  September 18, 1895 |
| 7 | 8 | 9 |
September 30, 1913 |  October 11, 1931 |  October 21, 1949 |
| 10 | 11 | 12 |
 November 2, 1967 |  November 12, 1985 |  November 23, 2003 |
| 13 | 14 | 15 |
 December 4, 2021 |  December 15, 2039 |  December 26, 2057 |
| 16 | 17 | 18 |
 January 6, 2076 |  January 16, 2094 |  January 29, 2112 |
| 19 | 20 | 21 |
 February 8, 2130 |  February 19, 2148 |  March 2, 2166 |
| 22 | ||
 March 12, 2184 | ||
Themetonic series repeats eclipses every 19 years (6939.69 days), lasting about 5 cycles. Eclipses occur in nearly the same calendar date. In addition, the octon subseries repeats 1/5 of that or every 3.8 years (1387.94 days). All eclipses in this table occur at the Moon's descending node.
| 22 eclipse events between February 23, 1830 and July 19, 1917 | ||||
|---|---|---|---|---|
| February 22–23 | December 11–12 | September 29–30 | July 18–19 | May 6–7 |
| 108 | 110 | 112 | 114 | 116 |
 February 23, 1830 |  July 18, 1841 |  May 6, 1845 | ||
| 118 | 120 | 122 | 124 | 126 |
 February 23, 1849 |  December 11, 1852 |  September 29, 1856 |  July 18, 1860 |  May 6, 1864 |
| 128 | 130 | 132 | 134 | 136 |
 February 23, 1868 |  December 12, 1871 |  September 29, 1875 |  July 19, 1879 |  May 6, 1883 |
| 138 | 140 | 142 | 144 | 146 |
 February 22, 1887 |  December 12, 1890 |  September 29, 1894 |  July 18, 1898 |  May 7, 1902 |
| 148 | 150 | 152 | 154 | |
 February 23, 1906 |  December 12, 1909 | September 30, 1913 |  July 19, 1917 | |
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 1946 | ||||
|---|---|---|---|---|
 August 5, 1804 (Saros 142) |  July 6, 1815 (Saros 143) |  June 5, 1826 (Saros 144) |  May 4, 1837 (Saros 145) |  April 3, 1848 (Saros 146) |
 March 4, 1859 (Saros 147) |  January 31, 1870 (Saros 148) |  December 31, 1880 (Saros 149) |  December 1, 1891 (Saros 150) |  October 31, 1902 (Saros 151) |
September 30, 1913 (Saros 152) |  August 30, 1924 (Saros 153) |  July 30, 1935 (Saros 154) |  June 29, 1946 (Saros 155) | |
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 | ||
|---|---|---|
 November 29, 1826 (Saros 149) |  November 9, 1855 (Saros 150) |  October 19, 1884 (Saros 151) |
September 30, 1913 (Saros 152) |  September 10, 1942 (Saros 153) |  August 20, 1971 (Saros 154) |
 July 31, 2000 (Saros 155) |  July 11, 2029 (Saros 156) |  June 21, 2058 (Saros 157) |
 June 1, 2087 (Saros 158) | ||
 April 1, 2174 (Saros 161) | ||
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