A partial solar eclipse occurred at the Moon's descending node of orbit on Tuesday, September 8, 1801, with a magnitude of 0.1614. A solar eclipse occurs when the Moon passes between Earth and the Sun, 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 eastern Russia and western Alaska.[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]
| Equatorial Conjunction | 1801 September 08 at 04:23:25.3 UTC | |
| First Penumbral External Contact | 1801 September 08 at 04:53:32.8 UTC | |
| Ecliptic Conjunction | 1801 September 08 at 05:38:08.2 UTC | |
| Greatest Eclipse | 1801 September 08 at 05:54:39.3 UTC | |
| Last Penumbral External Contact | 1801 September 08 at 06:56:17.9 UTC |
| Eclipse Magnitude | 0.16147 | |
| Eclipse Obscuration | 0.07489 | |
| Gamma | 1.46568 | |
| Sun Right Ascension | 11h04m58.3s | |
| Sun Declination | +05°53'39.8" | |
| Sun Semi-Diameter | 15'53.2" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 11h07m32.9s | |
| Moon Declination | +07°04'46.3" | |
| Moon Semi-Diameter | 15'03.7" | |
| Moon Equatorial Horizontal Parallax | 0°55'16.6" | |
| ΔT | 12.8 s |
See also: Eclipse cycle. This eclipse is part of an eclipse 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 a fortnight. The first and last eclipse in this sequence is separated by one synodic month.
The partial solar eclipses on April 13, 1801 and October 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 of Saros series 112, repeating every 18 years, 11 days, and containing 72 events. The series started with a partial solar eclipse on July 31, 539 AD. It contains total eclipses from March 15, 918 AD through November 18, 1332; hybrid eclipses from November 30, 1350 through April 29, 1585; and annular eclipses from May 11, 1603 through June 23, 1675. The series ends at member 72 as a partial eclipse on September 19, 1819. Its eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
The longest duration of totality was produced by member 30 at 7 minutes, 20 seconds on June 9, 1062, and the longest duration of annularity was produced by member 64 at 1 minute, 1 second on June 23, 1675. All eclipses in this series occur at the Moon’s descending node of orbit.[3]
All eclipses in this table occur at the Moon's descending node.
