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May 1920 lunar eclipse
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May 1920 lunar eclipse
A total lunar eclipse occurred at the Moon’s ascending node of orbit on Monday, May 3, 1920, with an umbral magnitude of 1.2194. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. Unlike a solar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on the night side of Earth. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon's shadow is smaller. Occurring only about 3.8 days before apogee (on May 6, 1920, at 21:00 UTC), the Moon's apparent diameter was smaller.
This lunar eclipse was the first of an almost tetrad, with the others being on October 27, 1920 (total); April 22, 1921 (total); and October 16, 1921 (partial).
The eclipse was completely visible over South America, west and southern Africa, western Europe, and Antarctica, seen rising over much of North America and the eastern Pacific Ocean and setting over eastern Europe, east Africa, and the western half of Asia.
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.
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.
This eclipse is a member of a semester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.
The penumbral lunar eclipse on March 13, 1922 occurs in the next lunar year eclipse set.
This eclipse is a part of Saros series 120, repeating every 18 years, 11 days, and containing 83 events. The series started with a penumbral lunar eclipse on October 16, 1000. It contains partial eclipses from May 31, 1379 through August 4, 1487; total eclipses from August 14, 1505 through May 14, 1938; and a second set of partial eclipses from May 24, 1956 through July 28, 2064. The series ends at member 83 as a penumbral eclipse on April 7, 2479.
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May 1920 lunar eclipse AI simulator
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May 1920 lunar eclipse
A total lunar eclipse occurred at the Moon’s ascending node of orbit on Monday, May 3, 1920, with an umbral magnitude of 1.2194. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. Unlike a solar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on the night side of Earth. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon's shadow is smaller. Occurring only about 3.8 days before apogee (on May 6, 1920, at 21:00 UTC), the Moon's apparent diameter was smaller.
This lunar eclipse was the first of an almost tetrad, with the others being on October 27, 1920 (total); April 22, 1921 (total); and October 16, 1921 (partial).
The eclipse was completely visible over South America, west and southern Africa, western Europe, and Antarctica, seen rising over much of North America and the eastern Pacific Ocean and setting over eastern Europe, east Africa, and the western half of Asia.
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.
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.
This eclipse is a member of a semester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.
The penumbral lunar eclipse on March 13, 1922 occurs in the next lunar year eclipse set.
This eclipse is a part of Saros series 120, repeating every 18 years, 11 days, and containing 83 events. The series started with a penumbral lunar eclipse on October 16, 1000. It contains partial eclipses from May 31, 1379 through August 4, 1487; total eclipses from August 14, 1505 through May 14, 1938; and a second set of partial eclipses from May 24, 1956 through July 28, 2064. The series ends at member 83 as a penumbral eclipse on April 7, 2479.
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