| Partial eclipse | |
 Map | |
| Gamma | 1.3152 |
|---|---|
| Magnitude | 0.4208 |
| Maximum eclipse | |
| Coordinates | 61°18′N11°42′E / 61.3°N 11.7°E /61.3; 11.7 |
| Times (UTC) | |
| Greatest eclipse | 4:08:06 |
| References | |
| Saros | 145 (10 of 77) |
| Catalog # (SE5000) | 9041 |
A partialsolar eclipse occurred at the Moon'sascending node of orbit on Monday, April 13, 1801, with amagnitude of 0.4208. 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.
The partial solar eclipse was visible for parts of modern-day easternEurope, theMiddle East,Central Asia, and westernRussia.[1]
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.[2]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1801 April 13 at 02:34:55.9 UTC |
| Greatest Eclipse | 1801 April 13 at 04:08:06.0 UTC |
| Ecliptic Conjunction | 1801 April 13 at 04:22:34.4 UTC |
| Equatorial Conjunction | 1801 April 13 at 05:24:45.4 UTC |
| Last Penumbral External Contact | 1801 April 13 at 05:40:50.4 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.42080 |
| Eclipse Obscuration | 0.30319 |
| Gamma | 1.31524 |
| Sun Right Ascension | 01h24m07.8s |
| Sun Declination | +08°51'22.7" |
| Sun Semi-Diameter | 15'56.2" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 01h21m49.0s |
| Moon Declination | +09°57'16.7" |
| Moon Semi-Diameter | 15'25.5" |
| Moon Equatorial Horizontal Parallax | 0°56'36.5" |
| ΔT | 12.9 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.
| March 14 Ascending node (new moon) | March 30 Descending node (full moon) | April 13 Ascending node (new moon) |
|---|---|---|
 | | |
| Partial solar eclipse Solar Saros 107 | Total lunar eclipse Lunar Saros 119 | Partial solar eclipse Solar Saros 145 |
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.[3]
The partial solar eclipses on [h] occur in the previous lunar year eclipse set, and the partial solar eclipses on March 14, 1801 and September 8, 1801 occur in the next lunar year eclipse set.
| Solar eclipse series sets from 1798 to 1801 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 115 | May 15, 1798 Annular | −0.8744 | 120 | November 8, 1798 Total | 0.8270 | |
| 125 | May 5, 1799 Annular | −0.1310 | 130 | October 28, 1799 Total | 0.1274 | |
| 135 | April 24, 1800 Annular | 0.6125 | 140 | October 18, 1800 Total | −0.5787 | |
| 145 | April 13, 1801 Partial | 1.3152 | 150 | October 7, 1801 Partial | −1.3552 | |
This eclipse is a part ofSaros series 145, repeating every 18 years, 11 days, and containing 77 events. The series started with a partial solar eclipse onJanuary 4, 1639. It contains an annular eclipse on June 6, 1891; a hybrid eclipse onJune 17, 1909; and total eclipses fromJune 29, 1927 through September 9, 2648. The series ends at member 77 as a partial eclipse on April 17, 3009. 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 15 at 6 seconds (by default) on June 6, 1891, and the longest duration of totality will be produced by member 50 at 7 minutes, 12 seconds on June 25, 2522. All eclipses in this series occur at the Moon’sascending node of orbit.[4]
| Series members 10–32 occur between 1801 and 2200: | ||
|---|---|---|
| 10 | 11 | 12 |
April 13, 1801 |  April 24, 1819 |  May 4, 1837 |
| 13 | 14 | 15 |
 May 16, 1855 |  May 26, 1873 |  June 6, 1891 |
| 16 | 17 | 18 |
 June 17, 1909 |  June 29, 1927 |  July 9, 1945 |
| 19 | 20 | 21 |
 July 20, 1963 |  July 31, 1981 |  August 11, 1999 |
| 22 | 23 | 24 |
 August 21, 2017 |  September 2, 2035 |  September 12, 2053 |
| 25 | 26 | 27 |
 September 23, 2071 |  October 4, 2089 |  October 16, 2107 |
| 28 | 29 | 30 |
 October 26, 2125 |  November 7, 2143 |  November 17, 2161 |
| 31 | 32 | |
 November 28, 2179 |  December 9, 2197 | |
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 ascending node.
| 2 eclipse events between April 13, 1801 and September 5, 1812 | ||||
|---|---|---|---|---|
| April 13 | January 30 | November 18 | September 5 | |
| 145 | 147 | 149 | 151 | |
April 13, 1801 |  January 30, 1805 |  November 18, 1808 |  September 5, 1812 | |
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 1888 | ||||
|---|---|---|---|---|
April 13, 1801 (Saros 145) |  March 13, 1812 (Saros 146) |  February 11, 1823 (Saros 147) |  January 9, 1834 (Saros 148) |  December 9, 1844 (Saros 149) |
 November 9, 1855 (Saros 150) |  October 8, 1866 (Saros 151) |  September 7, 1877 (Saros 152) |  August 7, 1888 (Saros 153) | |
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 | ||
|---|---|---|
April 13, 1801 (Saros 145) |  March 24, 1830 (Saros 146) |  March 4, 1859 (Saros 147) |
 February 11, 1888 (Saros 148) |  January 23, 1917 (Saros 149) |  January 3, 1946 (Saros 150) |
 December 13, 1974 (Saros 151) |  November 23, 2003 (Saros 152) |  November 3, 2032 (Saros 153) |
 October 13, 2061 (Saros 154) |  September 23, 2090 (Saros 155) |  September 5, 2119 (Saros 156) |
 August 14, 2148 (Saros 157) |  July 25, 2177 (Saros 158) | |
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