| Annular eclipse | |
 Map | |
| Gamma | 0.3224 |
|---|---|
| Magnitude | 0.965 |
| Maximum eclipse | |
| Duration | 227 s (3 min 47 s) |
| Coordinates | 6°18′N121°24′E / 6.3°N 121.4°E /6.3; 121.4 |
| Max. width of band | 133 km (83 mi) |
| Times (UTC) | |
| Greatest eclipse | 4:13:02 |
| References | |
| Saros | 132 (40 of 71) |
| Catalog # (SE5000) | 9307 |
An annularsolar eclipse occurred at the Moon'sdescending node of orbit on Sunday, October 22, 1911,[1][2][3] with amagnitude of 0.965. Asolar eclipse occurs when theMoon passes betweenEarth and theSun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon'sapparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like anannulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring about 5.75 days beforeapogee (on October 27, 1911, at 22:30 UTC), the Moon's apparent diameter was larger.[4]
Annularity was visible from theRussian Empire (the parts now belonging toKazakhstan,Uzbekistan andKyrgyzstan),China,French Indochina (the part now belonging toVietnam),Philippines,Dutch East Indies (today'sIndonesia),Territory of Papua (now belonging toPapua New Guinea) including the capital cityPort Moresby, andBritish Western Pacific Territories (the parts now belonging toSolomon Islands andTuvalu, including the city ofHoniara andTulagi). A partial eclipse was visible for parts ofSouth Asia,Southeast Asia,East Asia,Australia, andOceania.
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.[5]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1911 October 22 at 01:19:29.5 UTC |
| First Umbral External Contact | 1911 October 22 at 02:23:49.9 UTC |
| First Central Line | 1911 October 22 at 02:25:31.6 UTC |
| First Umbral Internal Contact | 1911 October 22 at 02:27:13.6 UTC |
| First Penumbral Internal Contact | 1911 October 22 at 03:39:33.3 UTC |
| Equatorial Conjunction | 1911 October 22 at 03:54:33.7 UTC |
| Ecliptic Conjunction | 1911 October 22 at 04:09:22.2 UTC |
| Greatest Eclipse | 1911 October 22 at 04:13:02.1 UTC |
| Last Penumbral Internal Contact | 1911 October 22 at 04:46:55.9 UTC |
| Greatest Duration | 1911 October 22 at 04:53:44.9 UTC |
| Last Umbral Internal Contact | 1911 October 22 at 05:59:00.0 UTC |
| Last Central Line | 1911 October 22 at 06:00:44.7 UTC |
| Last Umbral External Contact | 1911 October 22 at 06:02:29.3 UTC |
| Last Penumbral External Contact | 1911 October 22 at 07:06:48.6 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.96497 |
| Eclipse Obscuration | 0.93116 |
| Gamma | 0.32241 |
| Sun Right Ascension | 13h42m39.4s |
| Sun Declination | -10°38'28.3" |
| Sun Semi-Diameter | 16'04.4" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 13h43m12.3s |
| Moon Declination | -10°22'21.8" |
| Moon Semi-Diameter | 15'16.9" |
| Moon Equatorial Horizontal Parallax | 0°56'05.1" |
| ΔT | 13.0 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.
| October 22 Descending node (new moon) | November 6 Ascending node (full moon) |
|---|---|
|  |
| Total solar eclipse Solar Saros 132 | Penumbral lunar eclipse Lunar Saros 144 |
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.[6]
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 132, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on August 13, 1208. It contains annular eclipses from March 17, 1569 through March 12, 2146; hybrid eclipses on March 23, 2164 and April 3, 2182; and total eclipses from April 14, 2200 through June 19, 2308. The series ends at member 71 as a partial eclipse on September 25, 2470. 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 25 at 6 minutes, 56 seconds on May 9, 1641, and the longest duration of totality will be produced by member 61 at 2 minutes, 14 seconds on June 8, 2290. All eclipses in this series occur at the Moon’sdescending node of orbit.[7]
| Series members 34–56 occur between 1801 and 2200: | |||
|---|---|---|---|
| 34 | 35 | 36 | |
 August 17, 1803 |  August 27, 1821 |  September 7, 1839 | |
| 37 | 38 | 39 | |
 September 18, 1857 |  September 29, 1875 |  October 9, 1893 | |
| 40 | 41 | 42 | |
October 22, 1911 |  November 1, 1929 |  November 12, 1947 | |
| 43 | 44 | 45 | |
 November 23, 1965 |  December 4, 1983 |  December 14, 2001 | |
| 46 | 47 | 48 | |
 December 26, 2019 |  January 5, 2038 |  January 16, 2056 | |
| 49 | 50 | 51 | |
 January 27, 2074 |  February 7, 2092 |  February 18, 2110 | |
| 52 | 53 | 54 | |
 March 1, 2128 |  March 12, 2146 |  March 23, 2164 | |
| 55 | 56 | ||
 April 3, 2182 |  April 14, 2200 | ||
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 March 16, 1866 and August 9, 1953 | ||||
|---|---|---|---|---|
| March 16–17 | January 1–3 | October 20–22 | August 9–10 | May 27–29 |
| 108 | 110 | 112 | 114 | 116 |
 March 16, 1866 |  August 9, 1877 |  May 27, 1881 | ||
| 118 | 120 | 122 | 124 | 126 |
 March 16, 1885 |  January 1, 1889 |  October 20, 1892 |  August 9, 1896 |  May 28, 1900 |
| 128 | 130 | 132 | 134 | 136 |
 March 17, 1904 |  January 3, 1908 | October 22, 1911 |  August 10, 1915 |  May 29, 1919 |
| 138 | 140 | 142 | 144 | 146 |
 March 17, 1923 |  January 3, 1927 |  October 21, 1930 |  August 10, 1934 |  May 29, 1938 |
| 148 | 150 | 152 | 154 | |
 March 16, 1942 |  January 3, 1946 |  October 21, 1949 |  August 9, 1953 | |
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 | ||||
|---|---|---|---|---|
 August 28, 1802 (Saros 122) |  July 27, 1813 (Saros 123) |  June 26, 1824 (Saros 124) |  May 27, 1835 (Saros 125) |  April 25, 1846 (Saros 126) |
 March 25, 1857 (Saros 127) |  February 23, 1868 (Saros 128) |  January 22, 1879 (Saros 129) |  December 22, 1889 (Saros 130) |  November 22, 1900 (Saros 131) |
October 22, 1911 (Saros 132) |  September 21, 1922 (Saros 133) |  August 21, 1933 (Saros 134) |  July 20, 1944 (Saros 135) |  June 20, 1955 (Saros 136) |
 May 20, 1966 (Saros 137) |  April 18, 1977 (Saros 138) |  March 18, 1988 (Saros 139) |  February 16, 1999 (Saros 140) |  January 15, 2010 (Saros 141) |
 December 14, 2020 (Saros 142) |  November 14, 2031 (Saros 143) |  October 14, 2042 (Saros 144) |  September 12, 2053 (Saros 145) |  August 12, 2064 (Saros 146) |
 July 13, 2075 (Saros 147) |  June 11, 2086 (Saros 148) |  May 11, 2097 (Saros 149) |  April 11, 2108 (Saros 150) |  March 11, 2119 (Saros 151) |
 February 8, 2130 (Saros 152) |  January 8, 2141 (Saros 153) |  December 8, 2151 (Saros 154) |  November 7, 2162 (Saros 155) |  October 7, 2173 (Saros 156) |
 September 4, 2184 (Saros 157) |  August 5, 2195 (Saros 158) | |||
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 | ||
|---|---|---|
 December 20, 1824 (Saros 129) |  November 30, 1853 (Saros 130) |  November 10, 1882 (Saros 131) |
October 22, 1911 (Saros 132) |  October 1, 1940 (Saros 133) |  September 11, 1969 (Saros 134) |
 August 22, 1998 (Saros 135) |  August 2, 2027 (Saros 136) |  July 12, 2056 (Saros 137) |
 June 22, 2085 (Saros 138) |  June 3, 2114 (Saros 139) |  May 14, 2143 (Saros 140) |
 April 23, 2172 (Saros 141) | ||
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