• Source: Solar eclipse of June 20, 1955

A total solar eclipse occurred at the Moon's descending node of orbit on Monday, June 20, 1955, with a magnitude of 1.0776. 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 14.5 hours after perigee (on June 19, 1955, at 14:40 UTC), the Moon's apparent diameter was larger.
With a maximum duration of 7 minutes 7.74 seconds, this is the longest solar eclipse of Saros series 136, as well as the longest total solar eclipse since the 11th century, and until the 22nd century, because greatest eclipse occurred near the equator.
Totality began over the Indian Ocean, British Seychelles (today's Seychelles) and Maldives, crossing Ceylon (name changed to Sri Lanka later) including the capital city Colombo, Andaman Islands, Burma, Thailand including the capital city Bangkok, Cambodia, Laos, South Vietnam (now belonging to Vietnam), Paracel Islands and Scarborough Shoal (near the greatest eclipse), moving across the Philippines including the capital city Manila, Kayangel Atoll in the Trust Territory of the Pacific Islands (now belonging to Palau), Nukumanu Islands in the Territory of Papua New Guinea (today's Papua New Guinea), towards northern Ontong Java Atoll in British Solomon Islands (today's Solomon Islands) ending over Southwestern Pacific Ocean. A partial eclipse was visible for parts of South Asia, Southeast Asia, East Asia, Australia, and Oceania.
This was the second of four central solar eclipses visible from Bangkok from 1948 to 1958, where it is extremely rare for a large city to witness four central solar eclipses within 10 years.




Observations


The Tokyo Astronomical Observatory (now incorporated into the National Astronomical Observatory of Japan) of the University of Tokyo sent an expedition to Ceylon, but observation failed due to bad weather conditions. The Hydrographic Office of Japan (now Hydrographic and Oceanographic Department of Japan Coast Guard) sent a team to the western coast of Bình Thuận, Bình Sơn district, Quảng Ngãi province, South Vietnam. The whole process was not affected by any clouds or fog. The team said that totality of this eclipse was particularly dark compared with previous total solar eclipses observed, and the long duration of totality was also one of the reasons. The team took many images of solar corona successfully. A small team from the United States observed the total eclipse from Thailand. Some members of the Thai royal family also saw the eclipse from Phra Nakhon Si Ayutthaya province, north of the capital city Bangkok. In addition, Radio Thailand also broadcast a special program on the total solar eclipse nationally, which was the first such broadcast in Thailand.




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 1955

=
A penumbral lunar eclipse on January 8.
A penumbral lunar eclipse on June 5.
A total solar eclipse on June 20.
A partial lunar eclipse on November 29.
An annular solar eclipse on December 14.




= Metonic

=
Preceded by: Solar eclipse of September 1, 1951
Followed by: Solar eclipse of April 8, 1959




= Tzolkinex

=
Preceded by: Solar eclipse of May 9, 1948
Followed by: Solar eclipse of July 31, 1962




= Half-Saros

=
Preceded by: Lunar eclipse of June 14, 1946
Followed by: Lunar eclipse of June 25, 1964




= Tritos

=
Preceded by: Solar eclipse of July 20, 1944
Followed by: Solar eclipse of May 20, 1966




= Solar Saros 136

=
Preceded by: Solar eclipse of June 8, 1937
Followed by: Solar eclipse of June 30, 1973




= Inex

=
Preceded by: Solar eclipse of July 9, 1926
Followed by: Solar eclipse of May 30, 1984




= Triad

=
Preceded by: Solar eclipse of August 18, 1868
Followed by: Solar eclipse of April 20, 2042




= Solar eclipses of 1953–1956

=
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 14, 1953 and August 9, 1953 occur in the previous 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.




Notes






References


Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
Google interactive map
Besselian elements
Photometry of the Solar Corona at the Eclipse on June 20, 1955, Publications of the Astronomical Society of Japan, vol. 8, p.126 (1956).
Nasa.gov

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