August 1933 lunar eclipse

A penumbral lunar eclipse occurred at the Moon’s ascending node of orbit on Saturday, August 5, 1933, with an umbral magnitude of −0.7336. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A penumbral lunar eclipse occurs when part or all of the Moon's near side passes into the Earth's penumbra. 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. Occurring about 2.1 days after perigee (on August 3, 1933, at 17:40 UTC), the Moon's apparent diameter was larger.

This eclipse was the third of four penumbral lunar eclipses in 1933, with the others occurring on February 10, March 12, and September 4.

Visibility

The eclipse was completely visible over much of Africa, eastern Europe, much of Asia, Australia, and Antarctica, seen rising over western Europe, west Africa, and eastern Brazil and setting over northeast Asia and the western Pacific Ocean.

Eclipse details

Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.

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. The first and last eclipse in this sequence is separated by one synodic month.

Related eclipses

Eclipses in 1933

• A penumbral lunar eclipse on February 10.
• An annular solar eclipse on February 24.
• A penumbral lunar eclipse on March 12.
• A penumbral lunar eclipse on August 5.
• An annular solar eclipse on August 21.
• A penumbral lunar eclipse on September 4.

Metonic

• Followed by: Lunar eclipse of May 25, 1937

Tzolkinex

• Preceded by: Lunar eclipse of June 25, 1926

Half-Saros

• Preceded by: Solar eclipse of July 31, 1924
• Followed by: Solar eclipse of August 12, 1942

Tritos

• Followed by: Lunar eclipse of July 6, 1944

Lunar Saros 108

• Preceded by: Lunar eclipse of July 26, 1915
• Followed by: Lunar eclipse of August 17, 1951

Inex

• Followed by: Lunar eclipse of July 17, 1962

Triad

• Preceded by: Lunar eclipse of October 4, 1846
• Followed by: Lunar eclipse of June 5, 2020

Lunar eclipses of 1933–1936

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 eclipses on March 12, 1933 and September 4, 1933 occur in the previous lunar year eclipse set.

Saros 108

This eclipse is a part of Saros series 108, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on July 8, 689 AD. It contains partial eclipses from February 9, 1050 through May 17, 1212; total eclipses from May 28, 1230 through September 23, 1428; and a second set of partial eclipses from October 5, 1446 through June 1, 1825. The series ends at member 72 as a penumbral eclipse on August 27, 1969.

The longest duration of totality was produced by member 35 at 105 minutes, 57 seconds on July 10, 1302. All eclipses in this series occur at the Moon’s ascending node of orbit.

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.

Tritos series

This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic 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.

Inex series

This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic 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.

Half-Saros cycle

A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros). This lunar eclipse is related to two total solar eclipses of Solar Saros 115.

See also

• List of lunar eclipses
• List of 20th-century lunar eclipses

Notes

External links

• Eclipse Predictions by Fred Espenak, NASA/GSFC