| Annular eclipse | |
 Map | |
| Gamma | −0.0048 |
|---|---|
| Magnitude | 0.9657 |
| Maximum eclipse | |
| Duration | 227 s (3 min 47 s) |
| Coordinates | 13°36′N54°42′E / 13.6°N 54.7°E /13.6; 54.7 |
| Max. width of band | 124 km (77 mi) |
| Times (UTC) | |
| Greatest eclipse | 8:25:03 |
| References | |
| Saros | 132 (34 of 71) |
| Catalog # (SE5000) | 9048 |
An annularsolar eclipse occurred at the Moon'sdescending node of orbit on Wednesday, August 17, 1803, with amagnitude of 0.9657. 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 4.5 days beforeapogee (on August 21, 1803, at 19:20 UTC), the Moon's apparent diameter was smaller.[1]
The path of annularity was visible from parts of modern-dayWestern Sahara,Mauritania, far northernMali,Algeria,Libya,Egypt,Saudi Arabia, andYemen. A partial solar eclipse was also visible for parts ofEurope,North Africa,Central Africa, theMiddle East,South Asia, andSoutheast Asia.[2] It was the first solar eclipse to be subject to detailed spectroscopic study.[3]
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) |
|---|---|
| First Penumbral External Contact | 1803 August 17 at 05:24:35.4 UTC |
| First Umbral External Contact | 1803 August 17 at 06:27:46.8 UTC |
| First Central Line | 1803 August 17 at 06:29:24.5 UTC |
| First Umbral Internal Contact | 1803 August 17 at 06:31:02.3 UTC |
| First Penumbral Internal Contact | 1803 August 17 at 07:34:15.4 UTC |
| Greatest Duration | 1803 August 17 at 07:56:21.3 UTC |
| Greatest Eclipse | 1803 August 17 at 08:25:03.0 UTC |
| Ecliptic Conjunction | 1803 August 17 at 08:25:06.3 UTC |
| Equatorial Conjunction | 1803 August 17 at 08:25:18.6 UTC |
| Last Penumbral Internal Contact | 1803 August 17 at 09:15:49.4 UTC |
| Last Umbral Internal Contact | 1803 August 17 at 10:19:01.8 UTC |
| Last Central Line | 1803 August 17 at 10:20:42.0 UTC |
| Last Umbral External Contact | 1803 August 17 at 10:22:22.3 UTC |
| Last Penumbral External Contact | 1803 August 17 at 11:25:36.2 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.96571 |
| Eclipse Obscuration | 0.93259 |
| Gamma | −0.00483 |
| Sun Right Ascension | 09h43m00.2s |
| Sun Declination | +13°43'47.1" |
| Sun Semi-Diameter | 15'48.3" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 09h42m59.7s |
| Moon Declination | +13°43'32.7" |
| Moon Semi-Diameter | 15'01.8" |
| Moon Equatorial Horizontal Parallax | 0°55'09.5" |
| ΔT | 12.4 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 3 Ascending node (full moon) | August 17 Descending node (new moon) | September 1 Ascending node (full moon) |
|---|---|---|
| ||
| Penumbral lunar eclipse Lunar Saros 106 | Annular 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.[5]
The partial solar eclipses onApril 13, 1801 andOctober 7, 1801 occur in the previous lunar year eclipse set, and the solar eclipses on January 1, 1805 (partial); June 26, 1805 (partial); and December 21, 1805 (annular) occur in the next lunar year eclipse set.
| Solar eclipse series sets from 1801 to 1805 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 107 | March 14, 1801 Partial | −1.4434 | 112 | September 8, 1801 Partial | 1.4657 | |
| 117 | March 4, 1802 Total | −0.6943 | 122 | August 28, 1802 Annular | 0.7569 | |
| 127 | February 21, 1803 Total | −0.0075 | 132 | August 17, 1803 Annular | −0.0048 | |
| 137 | February 11, 1804 Hybrid | 0.7053 | 142 | August 5, 1804 Total | −0.7622 | |
| 147 | January 30, 1805 Partial | 1.4651 | 152 | July 26, 1805 Partial | −1.4571 | |
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.[6]
| 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.
| 24 eclipse events between August 17, 1803 and August 16, 1841 | ||||
|---|---|---|---|---|
| August 16–17 | June 5–6 | March 24 | January 9–10 | October 29 |
| 132 | 134 | 136 | 138 | 140 |
August 17, 1803 |  June 6, 1807 |  March 24, 1811 |  January 10, 1815 |  October 29, 1818 |
| 142 | 144 | 146 | 148 | 150 |
 August 16, 1822 |  June 5, 1826 |  March 24, 1830 |  January 9, 1834 |  October 29, 1837 |
| 152 | ||||
 August 16, 1841 | ||||
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 2087 | ||||
|---|---|---|---|---|
August 17, 1803 (Saros 132) |  July 17, 1814 (Saros 133) |  June 16, 1825 (Saros 134) |  May 15, 1836 (Saros 135) |  April 15, 1847 (Saros 136) |
 March 15, 1858 (Saros 137) |  February 11, 1869 (Saros 138) |  January 11, 1880 (Saros 139) |  December 12, 1890 (Saros 140) |  November 11, 1901 (Saros 141) |
 October 10, 1912 (Saros 142) |  September 10, 1923 (Saros 143) |  August 10, 1934 (Saros 144) |  July 9, 1945 (Saros 145) |  June 8, 1956 (Saros 146) |
 May 9, 1967 (Saros 147) |  April 7, 1978 (Saros 148) |  March 7, 1989 (Saros 149) |  February 5, 2000 (Saros 150) |  January 4, 2011 (Saros 151) |
 December 4, 2021 (Saros 152) |  November 3, 2032 (Saros 153) |  October 3, 2043 (Saros 154) |  September 2, 2054 (Saros 155) |  August 2, 2065 (Saros 156) |
 July 1, 2076 (Saros 157) |  June 1, 2087 (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 | ||
|---|---|---|
August 17, 1803 (Saros 132) |  July 27, 1832 (Saros 133) |  July 8, 1861 (Saros 134) |
 June 17, 1890 (Saros 135) |  May 29, 1919 (Saros 136) |  May 9, 1948 (Saros 137) |
 April 18, 1977 (Saros 138) |  March 29, 2006 (Saros 139) |  March 9, 2035 (Saros 140) |
 February 17, 2064 (Saros 141) |  January 27, 2093 (Saros 142) |  January 8, 2122 (Saros 143) |
 December 19, 2150 (Saros 144) |  November 28, 2179 (Saros 145) | |
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