Solar eclipse of January 14, 1945

An annular solar eclipse occurred at the Moon's descending node of orbit on Sunday, January 14, 1945, with a magnitude of 0.997. 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. The Moon's apparent diameter was near the average diameter because it occurred 8.3 days after apogee (on January 5, 1945, at 20:40 UTC) and 3.5 days before perigee (on January 17, 1945, at 17:50 UTC).

Annularity was visible from Eastern Cape in South Africa, and northeastern Tasmania Island and Furneaux Group in Australia. A partial eclipse was visible for parts of Southern Africa, Antarctica, Australia, and Oceania.

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 1945

• An annular solar eclipse on January 14.
• A partial lunar eclipse on June 25.
• A total solar eclipse on July 9.
• A total lunar eclipse on December 19.

Metonic

• Preceded by: Solar eclipse of March 27, 1941
• Followed by: Solar eclipse of November 1, 1948

Tzolkinex

• Preceded by: Solar eclipse of December 2, 1937
• Followed by: Solar eclipse of February 25, 1952

Half-Saros

• Preceded by: Lunar eclipse of January 8, 1936
• Followed by: Lunar eclipse of January 19, 1954

Tritos

• Preceded by: Solar eclipse of February 14, 1934
• Followed by: Solar eclipse of December 14, 1955

Solar Saros 140

• Preceded by: Solar eclipse of January 3, 1927
• Followed by: Solar eclipse of January 25, 1963

Inex

• Preceded by: Solar eclipse of February 3, 1916
• Followed by: Solar eclipse of December 24, 1973

Triad

• Preceded by: Solar eclipse of March 15, 1858
• Followed by: Solar eclipse of November 14, 2031

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 140

This eclipse is a part of Saros series 140, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on April 16, 1512. It contains total eclipses from July 21, 1656 through November 9, 1836; hybrid eclipses from November 20, 1854 through December 23, 1908; and annular eclipses from January 3, 1927 through December 7, 2485. The series ends at member 71 as a partial eclipse on June 1, 2774. 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 11 at 4 minutes, 10 seconds on August 12, 1692, and the longest duration of annularity will be produced by member 53 at 7 minutes, 35 seconds on November 15, 2449. All eclipses in this series occur at the Moon’s descending 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 descending 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