| Partial eclipse | |
 Map | |
| Gamma | 1.4512 |
|---|---|
| Magnitude | 0.1513 |
| Maximum eclipse | |
| Coordinates | 61°30′N26°48′W / 61.5°N 26.8°W /61.5; -26.8 |
| Times (UTC) | |
| Greatest eclipse | 20:52:12 |
| References | |
| Saros | 114 (71 of 72) |
| Catalog # (SE5000) | 9312 |
A partialsolar eclipse occurred at the Moon'sdescending node of orbit on Sunday, August 31, 1913,[1][2][3] with amagnitude of 0.1513. 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 of easternCanada andGreenland.
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.[4]
| Event | Time (UTC) |
|---|---|
| Equatorial Conjunction | 1913 August 31 at 19:35:08.9 UTC |
| First Penumbral External Contact | 1913 August 31 at 20:02:37.1 UTC |
| Ecliptic Conjunction | 1913 August 31 at 20:38:01.7 UTC |
| Greatest Eclipse | 1913 August 31 at 20:52:11.8 UTC |
| Last Penumbral External Contact | 1913 August 31 at 21:42:17.1 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.15134 |
| Eclipse Obscuration | 0.06998 |
| Gamma | 1.45121 |
| Sun Right Ascension | 10h37m57.1s |
| Sun Declination | +08°38'38.2" |
| Sun Semi-Diameter | 15'51.0" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 10h40m42.4s |
| Moon Declination | +09°57'27.7" |
| Moon Semi-Diameter | 16'42.1" |
| Moon Equatorial Horizontal Parallax | 1°01'17.9" |
| ΔT | 15.5 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.[5]
The partial solar eclipses onApril 6, 1913 andSeptember 30, 1913 occur in the previous lunar year eclipse set, and the solar eclipses onDecember 24, 1916 (partial),June 19, 1917 (partial), andDecember 14, 1917 (annular) occur in the next lunar year eclipse set.
| Solar eclipse series sets from 1913 to 1917 | ||||||
|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 114 | August 31, 1913 Partial | 1.4512 | 119 | February 25, 1914 Annular | −0.9416 | |
| 124 | August 21, 1914 Total | 0.7655 | 129 | February 14, 1915 Annular | −0.2024 | |
| 134 | August 10, 1915 Annular | 0.0124 | 139.png) | February 3, 1916 Total | 0.4987 | |
| 144 | July 30, 1916 Annular | −0.7709 | 149 | January 23, 1917 Partial | 1.1508 | |
| 154 | July 19, 1917 Partial | −1.5101 | ||||
This eclipse is a part ofSaros series 114, repeating every 18 years, 11 days, and containing 72 events. The series started with a partial solar eclipse on July 23, 651 AD. It contains annular eclipses from February 3, 976 AD through June 11, 1192; hybrid eclipses from June 22, 1210 through December 1, 1480; and total eclipses from December 13, 1498 through June 15, 1787. The series ends at member 72 as a partial eclipse onSeptember 12, 1931. 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 annularity was produced by member 20 at 4 minutes, 33 seconds on February 13, 994 AD, and the longest duration of totality was produced by member 59 at 4 minutes, 18 seconds on April 21, 1697. All eclipses in this series occur at the Moon’sdescending node of orbit.[6]
| Series members 65–72 occur between 1801 and 1931: | ||
|---|---|---|
| 65 | 66 | 67 |
 June 26, 1805 |  July 8, 1823 |  July 18, 1841 |
| 68 | 69 | 70 |
 July 29, 1859 |  August 9, 1877 |  August 20, 1895 |
| 71 | 72 | |
August 31, 1913 |  September 12, 1931 | |
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 April 8, 1902 and August 31, 1989 | ||||
|---|---|---|---|---|
| April 7–8 | January 24–25 | November 12 | August 31–September 1 | June 19–20 |
| 108 | 110 | 112 | 114 | 116 |
 April 8, 1902 | August 31, 1913 |  June 19, 1917 | ||
| 118 | 120 | 122 | 124 | 126 |
 April 8, 1921 |  January 24, 1925 |  November 12, 1928 |  August 31, 1932 |  June 19, 1936 |
| 128 | 130 | 132 | 134 | 136 |
 April 7, 1940 |  January 25, 1944 |  November 12, 1947 |  September 1, 1951 |  June 20, 1955 |
| 138 | 140 | 142 | 144 | 146 |
 April 8, 1959 |  January 25, 1963 |  November 12, 1966 |  August 31, 1970 |  June 20, 1974 |
| 148 | 150 | 152 | 154 | |
 April 7, 1978 |  January 25, 1982 |  November 12, 1985 |  August 31, 1989 | |
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 1837 and 2200 | ||||
|---|---|---|---|---|
 April 5, 1837 (Saros 107) |  March 5, 1848 (Saros 108) |  February 3, 1859 (Saros 109) |  December 2, 1880 (Saros 111) | |
August 31, 1913 (Saros 114) |  July 31, 1924 (Saros 115) |  June 30, 1935 (Saros 116) | ||
 May 30, 1946 (Saros 117) |  April 30, 1957 (Saros 118) |  March 28, 1968 (Saros 119) |  February 26, 1979 (Saros 120) |  January 26, 1990 (Saros 121) |
 December 25, 2000 (Saros 122) |  November 25, 2011 (Saros 123) |  October 25, 2022 (Saros 124) |  September 23, 2033 (Saros 125) |  August 23, 2044 (Saros 126) |
 July 24, 2055 (Saros 127) |  June 22, 2066 (Saros 128) |  May 22, 2077 (Saros 129) |  April 21, 2088 (Saros 130) |  March 21, 2099 (Saros 131) |
 February 18, 2110 (Saros 132) |  January 19, 2121 (Saros 133) |  December 19, 2131 (Saros 134) |  November 17, 2142 (Saros 135) |  October 17, 2153 (Saros 136) |
 September 16, 2164 (Saros 137) |  August 16, 2175 (Saros 138) |  July 16, 2186 (Saros 139) |  June 15, 2197 (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 | ||
|---|---|---|
 October 31, 1826 (Saros 111) | ||
August 31, 1913 (Saros 114) |  August 12, 1942 (Saros 115) |  July 22, 1971 (Saros 116) |
 July 1, 2000 (Saros 117) |  June 12, 2029 (Saros 118) |  May 22, 2058 (Saros 119) |
 May 2, 2087 (Saros 120) |  April 13, 2116 (Saros 121) |  March 23, 2145 (Saros 122) |
 March 3, 2174 (Saros 123) | ||
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