Solar eclipse of August 1, 1943

An annular solar eclipse occurred at the Moon's ascending node of orbit on Sunday, August 1, 1943, with a magnitude of 0.9409. 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 about 25 minutes before apogee (on August 1, 1943, at 4:40 UTC), the Moon's apparent diameter was near its minimum. Apogee did occur as the eclipse was just before its greatest eclipse.

Annularity was visible in the southern Indian Ocean, with the only land being Île Amsterdam in French Madagascar (now belonging to French Southern and Antarctic Lands). A partial solar eclipse was visible from Australia, Indonesia, Malaysia, eastern Madagascar, Antarctica's Wilkes Land.

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.

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.

Related eclipses

Eclipses in 1943

• A total solar eclipse on February 4.
• A partial lunar eclipse on February 20.
• An annular solar eclipse on August 1.
• A partial lunar eclipse on August 15.

Metonic

• Preceded by: Solar eclipse of October 12, 1939
• Followed by: Solar eclipse of May 20, 1947

Tzolkinex

• Preceded by: Solar eclipse of June 19, 1936
• Followed by: Solar eclipse of September 12, 1950

Half-Saros

• Preceded by: Lunar eclipse of July 26, 1934
• Followed by: Lunar eclipse of August 5, 1952

Tritos

• Preceded by: Solar eclipse of August 31, 1932
• Followed by: Solar eclipse of June 30, 1954

Solar Saros 125

• Preceded by: Solar eclipse of July 20, 1925
• Followed by: Solar eclipse of August 11, 1961

Inex

• Preceded by: Solar eclipse of August 21, 1914
• Followed by: Solar eclipse of July 10, 1972

Triad

• Preceded by: Solar eclipse of September 29, 1856
• Followed by: Solar eclipse of June 1, 2030

Solar eclipses of 1942–1946

This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.

The partial solar eclipses on March 16, 1942 and September 10, 1942 occur in the previous lunar year eclipse set, and the partial solar eclipses on May 30, 1946 and November 23, 1946 occur in the next lunar year eclipse set.

Saros 125

This eclipse is a part of Saros series 125, repeating every 18 years, 11 days, and containing 73 events. The series started with a partial solar eclipse on February 4, 1060. It contains total eclipses from June 13, 1276 through July 16, 1330; hybrid eclipses on July 26, 1348 and August 7, 1366; and annular eclipses from August 17, 1384 through August 22, 1979. The series ends at member 73 as a partial eclipse on April 9, 2358. 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 14 at 1 minutes, 11 seconds on June 25, 1294, and the longest duration of annularity was produced by member 48 at 7 minutes, 23 seconds on July 10, 1907. All eclipses in this series occur at the Moon’s ascending node of orbit.

Metonic series

The metonic 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.

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.

Notes

• Eclipse Predictions by Fred Espenak, NASA/GSFC