| Annular eclipse | |
 Map | |
| Gamma | 0.8251 |
|---|---|
| Magnitude | 0.9329 |
| Maximum eclipse | |
| Duration | 349 s (5 min 49 s) |
| Coordinates | 51°36′N8°42′E / 51.6°N 8.7°E /51.6; 8.7 |
| Max. width of band | 432 km (268 mi) |
| Times (UTC) | |
| Greatest eclipse | 13:59:58 |
| References | |
| Saros | 122 (47 of 70) |
| Catalog # (SE5000) | 9091 |
← March 14, 1820 March 4, 1821 → | |
An annularsolar eclipse occurred at the Moon'sdescending node of orbit on Thursday, September 7, 1820, with amagnitude of 0.9329. 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 only about 5 hours beforeapogee (on September 7, 1820, at 18:50 UTC), the Moon's apparent diameter was smaller.[1]
The path of annularity was visible from parts of modern-day northernCanada,Greenland, westernNorway,Denmark, theNetherlands,Germany,Switzerland, theCzech Republic,Austria,Italy,Slovenia,Croatia,Bosnia and Herzegovina,Montenegro,Albania,Greece, northeasternLibya,Egypt,Israel,Jordan, andSaudi Arabia. A partial solar eclipse was also visible for parts of northernNorth America,Europe,North Africa, theMiddle East, andCentral Asia.
This map was drawn in the bookElementa eclipsium, published in Prague in 1816, byFranz Ignaz Cassian Hallaschka (František Ignác Kassián Halaška) (1780-1847), contained maps of the paths of solar eclipses from 1816 and 1860. The geometric constructions used by Hallaschka anticipated the standard theory of eclipses later developed byFriedrich Wilhelm Bessel.[2]
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.[3]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1820 September 7 at 11:21:45.1 UTC |
| First Umbral External Contact | 1820 September 7 at 12:48:53.2 UTC |
| First Central Line | 1820 September 7 at 12:53:29.4 UTC |
| First Umbral Internal Contact | 1820 September 7 at 12:58:19.3 UTC |
| Equatorial Conjunction | 1820 September 7 at 13:06:52.6 UTC |
| Ecliptic Conjunction | 1820 September 7 at 13:50:09.9 UTC |
| Greatest Duration | 1820 September 7 at 13:57:39.4 UTC |
| Greatest Eclipse | 1820 September 7 at 13:59:57.6 UTC |
| Last Umbral Internal Contact | 1820 September 7 at 15:02:09.4 UTC |
| Last Central Line | 1820 September 7 at 15:06:58.7 UTC |
| Last Umbral External Contact | 1820 September 7 at 15:11:34.3 UTC |
| Last Penumbral External Contact | 1820 September 7 at 16:38:31.5 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.93295 |
| Eclipse Obscuration | 0.87040 |
| Gamma | 0.82506 |
| Sun Right Ascension | 11h04m02.1s |
| Sun Declination | +05°59'29.3" |
| Sun Semi-Diameter | 15'53.0" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 11h05m27.2s |
| Moon Declination | +06°38'30.8" |
| Moon Semi-Diameter | 14'41.9" |
| Moon Equatorial Horizontal Parallax | 0°53'56.6" |
| ΔT | 11.4 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.
| September 7 Descending node (new moon) | September 22 Ascending node (full moon) |
|---|---|
| |
| Annular solar eclipse Solar Saros 122 | Partial lunar eclipse Lunar Saros 134 |
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.[4]
The partial solar eclipses on April 24, 1819 and October 19, 1819 occur in the previous lunar year eclipse set, and the partial solar eclipses on January 12, 1823 and July 8, 1823 occur in the next lunar year eclipse set.
| Solar eclipse series sets from 1819 to 1823 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 107 | March 25, 1819 Partial | −1.4722 | 112 | September 19, 1819 Partial | 1.5258 | |
| 117 | March 14, 1820 Total | −0.7199 | 122 | September 7, 1820 Annular | 0.8251 | |
| 127 | March 4, 1821 Total | −0.0284 | 132 | August 27, 1821 Annular | 0.0671 | |
| 137 | February 21, 1822 Annular | 0.6914 | 142 | August 16, 1822 Total | −0.6904 | |
| 147 | February 11, 1823 Partial | −1.5413 | 152 | August 6, 1823 Partial | 1.4546 | |
This eclipse is a part ofSaros series 122, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on April 17, 991 AD. It contains total eclipses from July 12, 1135 through August 3, 1171; hybrid eclipses on August 13, 1189 and August 25, 1207; and annular eclipses from September 4, 1225 through October 10, 1874. The series ends at member 70 as a partial eclipse on May 17, 2235. 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 was produced by member 9 at 1 minutes, 25 seconds on July 12, 1135, and the longest duration of annularity was produced by member 50 at 6 minutes, 28 seconds on October 10, 1874. All eclipses in this series occur at the Moon’sdescending node of orbit.[5]
| Series members 46–68 occur between 1801 and 2200: | ||
|---|---|---|
| 46 | 47 | 48 |
 August 28, 1802 |  September 7, 1820 |  September 18, 1838 |
| 49 | 50 | 51 |
 September 29, 1856 |  October 10, 1874 |  October 20, 1892 |
| 52 | 53 | 54 |
 November 2, 1910 |  November 12, 1928 |  November 23, 1946 |
| 55 | 56 | 57 |
 December 4, 1964 |  December 15, 1982 |  December 25, 2000 |
| 58 | 59 | 60 |
 January 6, 2019 |  January 16, 2037 |  January 27, 2055 |
| 61 | 62 | 63 |
 February 7, 2073 |  February 18, 2091 |  March 1, 2109 |
| 64 | 65 | 66 |
 March 13, 2127 |  March 23, 2145 |  April 3, 2163 |
| 67 | 68 | |
 April 14, 2181 |  April 25, 2199 | |
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 September 8, 1801 and September 7, 1877 | ||||
|---|---|---|---|---|
| September 7–8 | June 26–27 | April 14–15 | January 31–February 1 | November 19–20 |
| 112 | 114 | 116 | 118 | 120 |
 September 8, 1801 |  June 26, 1805 |  April 14, 1809 |  February 1, 1813 |  November 19, 1816 |
| 122 | 124 | 126 | 128 | 130 |
September 7, 1820 |  June 26, 1824 |  April 14, 1828 |  February 1, 1832 |  November 20, 1835 |
| 132 | 134 | 136 | 138 | 140 |
 September 7, 1839 |  June 27, 1843 |  April 15, 1847 |  February 1, 1851 |  November 20, 1854 |
| 142 | 144 | 146 | 148 | 150 |
 September 7, 1858 |  June 27, 1862 |  April 15, 1866 |  January 31, 1870 |  November 20, 1873 |
| 152 | ||||
 September 7, 1877 | ||||
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 | ||||
|---|---|---|---|---|
 October 9, 1809 (Saros 121) | September 7, 1820 (Saros 122) |  August 7, 1831 (Saros 123) |  July 8, 1842 (Saros 124) |  June 6, 1853 (Saros 125) |
 May 6, 1864 (Saros 126) |  April 6, 1875 (Saros 127) |  March 5, 1886 (Saros 128) |  February 1, 1897 (Saros 129) |  January 3, 1908 (Saros 130) |
 December 3, 1918 (Saros 131) |  November 1, 1929 (Saros 132) |  October 1, 1940 (Saros 133) |  September 1, 1951 (Saros 134) |  July 31, 1962 (Saros 135) |
 June 30, 1973 (Saros 136) |  May 30, 1984 (Saros 137) |  April 29, 1995 (Saros 138) |  March 29, 2006 (Saros 139) |  February 26, 2017 (Saros 140) |
 January 26, 2028 (Saros 141) |  December 26, 2038 (Saros 142) |  November 25, 2049 (Saros 143) |  October 24, 2060 (Saros 144) |  September 23, 2071 (Saros 145) |
 August 24, 2082 (Saros 146) |  July 23, 2093 (Saros 147) |  June 22, 2104 (Saros 148) |  May 24, 2115 (Saros 149) |  April 22, 2126 (Saros 150) |
 March 21, 2137 (Saros 151) |  February 19, 2148 (Saros 152) |  January 19, 2159 (Saros 153) |  December 18, 2169 (Saros 154) |  November 17, 2180 (Saros 155) |
 October 18, 2191 (Saros 156) | ||||
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 | ||
|---|---|---|
September 7, 1820 (Saros 122) |  August 18, 1849 (Saros 123) |  July 29, 1878 (Saros 124) |
 July 10, 1907 (Saros 125) |  June 19, 1936 (Saros 126) |  May 30, 1965 (Saros 127) |
 May 10, 1994 (Saros 128) |  April 20, 2023 (Saros 129) |  March 30, 2052 (Saros 130) |
 March 10, 2081 (Saros 131) |  February 18, 2110 (Saros 132) |  January 30, 2139 (Saros 133) |
 January 10, 2168 (Saros 134) |  December 19, 2196 (Saros 135) | |
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