A total solar eclipse will occur at the Moon's descending node of orbit on Wednesday, September 3, 2081, with a magnitude of 1.072. 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 5 hours before perigee (on September 3, 2081, at 14:05 UTC), the Moon's apparent diameter will be larger.
The path of totality will be visible from parts of Guernsey, Jersey, France, Germany, Switzerland, Liechtenstein, Austria, Italy, Slovenia, Croatia, Hungary, Bosnia and Herzegovina, Serbia, Romania, Bulgaria, Turkey, Syria, Iraq, Kuwait, far western Iran, Bahrain, Qatar, the United Arab Emirates, eastern Saudi Arabia, Oman, the Maldives, and southern Indonesia. A partial solar eclipse will also be visible for parts of Greenland, Europe, North Africa, Northeast Africa, the Middle East, Central Asia, South Asia, and Southeast Asia.
Contents
Major cities
Paris
Basel
Zurich
Innsbruck
Ljubljana
Zagreb
Istanbul
Ankara
Baghdad
Basra
Kuwait City
Manama
Doha
Abu Dhabi
Male
Mapped using timeanddate.
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 2081
An annular solar eclipse on March 10.
A partial lunar eclipse on March 25.
A total solar eclipse on September 3.
A penumbral lunar eclipse on September 18.
Metonic
Preceded by: Solar eclipse of November 15, 2077
Followed by: Solar eclipse of June 22, 2085
Tzolkinex
Preceded by: Solar eclipse of July 24, 2074
Followed by: Solar eclipse of October 14, 2088
Half-Saros
Preceded by: Lunar eclipse of August 28, 2072
Followed by: Lunar eclipse of September 8, 2090
Tritos
Preceded by: Solar eclipse of October 4, 2070
Followed by: Solar eclipse of August 3, 2092
Solar Saros 136
Preceded by: Solar eclipse of August 24, 2063
Followed by: Solar eclipse of September 14, 2099
Inex
Preceded by: Solar eclipse of September 22, 2052
Followed by: Solar eclipse of August 15, 2110
Triad
Preceded by: Solar eclipse of November 3, 1994
Followed by: Solar eclipse of July 5, 2168
Solar eclipses of 2080–2083
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 eclipse on July 15, 2083 occurs in the next lunar year eclipse set.
Saros 136
This eclipse is a part of Saros series 136, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on June 14, 1360. It contains annular eclipses from September 8, 1504 through November 12, 1594; hybrid eclipses from November 22, 1612 through January 17, 1703; and total eclipses from January 27, 1721 through May 13, 2496. The series ends at member 71 as a partial eclipse on July 30, 2622. 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 annularity was produced by member 9 at 32 seconds on September 8, 1504, and the longest duration of totality was produced by member 34 at 7 minutes, 7.74 seconds on June 20, 1955. 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.