Solar eclipse of June 26, 1824

A total solar eclipse occurred at the Moon's descending node of orbit between Saturday, June 26 and Sunday, June 27, 1824, with a magnitude of 1.0578. 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. A total solar eclipse occurs when the Moon's apparent diameter is larger than the Sun's, blocking all direct sunlight, turning day into darkness. Totality occurs in a narrow path across Earth's surface, with the partial solar eclipse visible over a surrounding region thousands of kilometres wide. Occurring about 1.9 days before perigee (on June 28, 1824, at 20:40 UTC), the Moon's apparent diameter was larger.

The path of totality was visible from parts of modern-day China, South Korea, North Korea, and Japan. A partial solar eclipse was also visible for parts of East Asia, Southeast Asia, Hawaii, and North America.

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 1824

• An annular solar eclipse on January 1.
• A partial lunar eclipse on January 16.
• A total solar eclipse on June 26.
• A partial lunar eclipse on July 11.
• A penumbral lunar eclipse on December 6.
• An annular solar eclipse on December 20.

Metonic

• Preceded by: Solar eclipse of September 7, 1820
• Followed by: Solar eclipse of April 14, 1828

Tzolkinex

• Preceded by: Solar eclipse of May 16, 1817
• Followed by: Solar eclipse of August 7, 1831

Half-Saros

• Preceded by: Lunar eclipse of June 21, 1815
• Followed by: Lunar eclipse of July 2, 1833

Tritos

• Preceded by: Solar eclipse of July 27, 1813
• Followed by: Solar eclipse of May 27, 1835

Solar Saros 124

• Preceded by: Solar eclipse of June 16, 1806
• Followed by: Solar eclipse of July 8, 1842

Inex

• Preceded by: Solar eclipse of July 16, 1795
• Followed by: Solar eclipse of June 6, 1853

Triad

• Preceded by: Solar eclipse of August 26, 1737
• Followed by: Solar eclipse of April 28, 1911

Solar eclipses of 1823–1826

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 February 11, 1823 and August 6, 1823 occur in the previous lunar year eclipse set, and the partial solar eclipse on October 31, 1826 occurs in the next lunar year eclipse set.

Saros 124

This eclipse is a part of Saros series 124, repeating every 18 years, 11 days, and containing 73 events. The series started with a partial solar eclipse on March 6, 1049. It contains total eclipses from June 12, 1211 through September 22, 1968, and a hybrid eclipse on October 3, 1986. There are no annular eclipses in this set. The series ends at member 73 as a partial eclipse on May 11, 2347. 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 39 at 5 minutes, 46 seconds on May 3, 1734. 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.