- Source: Solar eclipse of September 9, 1904
A total solar eclipse occurred at the Moon's ascending node of orbit on Friday, September 9, 1904, with a magnitude of 1.0709. 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 1.5 hours after perigee (on September 9, 1904, at 19:10 UTC), the Moon's apparent diameter was larger.
Totality was visible from German New Guinea (the part now belonging to Marshall Islands) on September 10 and Chile on September 9. A partial eclipse was visible for parts of Oceania and Western South America.
The event is mentioned in James Joyce's novel Ulysses.
Observations
The National Astronomical Observatory of Chile established an observation station in Taltal, Antofagasta, but the eclipse was clouded out and could not be seen. In the capital city Santiago, a partial eclipse was seen just before sunset.
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 1904
=A penumbral lunar eclipse on March 2.
An annular solar eclipse on March 17.
A penumbral lunar eclipse on March 31.
A total solar eclipse on September 9.
A penumbral lunar eclipse on September 24.
= Metonic
=Preceded by: Solar eclipse of November 22, 1900
Followed by: Solar eclipse of June 28, 1908
= Tzolkinex
=Preceded by: Solar eclipse of July 29, 1897
Followed by: Solar eclipse of October 22, 1911
= Half-Saros
=Preceded by: Lunar eclipse of September 4, 1895
Followed by: Lunar eclipse of September 15, 1913
= Tritos
=Preceded by: Solar eclipse of October 9, 1893
Followed by: Solar eclipse of August 10, 1915
= Solar Saros 133
=Preceded by: Solar eclipse of August 29, 1886
Followed by: Solar eclipse of September 21, 1922
= Inex
=Preceded by: Solar eclipse of September 29, 1875
Followed by: Solar eclipse of August 21, 1933
= Triad
=Preceded by: Solar eclipse of November 9, 1817
Followed by: Solar eclipse of July 11, 1991
= Solar eclipses of 1902–1906
=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 May 7, 1902 and October 31, 1902 occur in the previous lunar year eclipse set, and the partial solar eclipse on July 21, 1906 occurs in the next lunar year eclipse set.
= Saros 133
=This eclipse is a part of Saros series 133, repeating every 18 years, 11 days, and containing 72 events. The series started with a partial solar eclipse on July 13, 1219. It contains annular eclipses from November 20, 1435 through January 13, 1526; a hybrid eclipse on January 24, 1544; and total eclipses from February 3, 1562 through June 21, 2373. The series ends at member 72 as a partial eclipse on September 5, 2499. 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 25 at 1 minutes, 14 seconds on November 30, 1453, and the longest duration of totality was produced by member 61 at 6 minutes, 50 seconds on August 7, 1850. 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
References
Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
Google interactive map
Besselian elements
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- Solar eclipse of July 11, 1991
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- September 1904
- Inex
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