Solar eclipse of September 7, 1820
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| Annular eclipse | |
 Map | |
| Gamma | 0.8251 |
|---|---|
| Magnitude | 0.9329 |
| Maximum eclipse | |
| Duration | 349 s (5 min 49 s) |
| Coordinates | 51°36′N 8°42′E / 51.6°N 8.7°E |
| Max. width of band | 432 km (268 mi) |
| Times (UTC) | |
| Greatest eclipse | 13:59:58 |
| References | |
| Saros | 122 (47 of 70) |
| Catalog # (SE5000) | 9091 |
An annular solar eclipse occurred at the Moon's descending node of orbit on Thursday, September 7, 1820, with a magnitude of 0.9329. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring only about 5 hours before apogee (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 northern Canada, Greenland, western Norway, Denmark, the Netherlands, Germany, Switzerland, the Czech Republic, Austria, Italy, Slovenia, Croatia, Bosnia and Herzegovina, Montenegro, Albania, Greece, northeastern Libya, Egypt, Israel, Jordan, and Saudi Arabia. A partial solar eclipse was also visible for parts of northern North America, Europe, North Africa, the Middle East, and Central Asia.
This map was drawn in the book Elementa eclipsium, published in Prague in 1816, by Franz 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 by Friedrich Wilhelm Bessel.[2]
Eclipse details
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 |
Eclipse season
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.
| September 7 Descending node (new moon) | September 22 Ascending node (full moon) |
|---|---|
| |
| Annular solar eclipse Solar Saros 122 | Partial lunar eclipse Lunar Saros 134 |
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