• Source: Solar eclipse of March 7, 1970

A total solar eclipse occurred at the Moon's ascending node of orbit on Saturday, March 7, 1970, with a magnitude of 1.0414. 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 1.3 days after perigee (on March 6, 1970, at 10:30 UTC), this eclipse occurred when the Moon's apparent diameter was larger.
The greatest eclipse occurred over Mexico at 11:38 am CST, with totality lasting 3 minutes and 27.65 seconds. Totality over the U.S. lasted up to 3 minutes and 10 seconds. The media declared Perry as the first municipality in Florida to be in the eclipse direct path.
Inclement weather obstructed the viewing from that location and most of the eclipse path through the remainder of the southern states. There was not an eclipse with a greater duration of totality over the contiguous U.S. until April 8, 2024, a period of 54 years.
Totality was visible across southern Mexico and the Gulf of Mexico, Florida, Georgia, South Carolina, North Carolina, Virginia, Maryland, and Nantucket, Massachusetts in the United States, northeast to the Maritimes of eastern Canada, and northern Miquelon-Langlade in the French overseas collectivity of Saint Pierre and Miquelon. A partial eclipse was visible for parts of Hawaii, North America, Central America, the Caribbean, and northern South America.




Scientific effects


This eclipse slowed a radio transmission of atomic time from North Carolina to Washington, D.C.




Observations


An observation team from the Swiss Federal Observatory observed the total eclipse in Nejapa and Miahuatlán, Mexico. The weather conditions were good at both locations. Miahuatlán offered particularly good observation conditions with an altitude of 1,620 metres above sea level, high air quality and solar zenith angle of 63° at the time of the eclipse. The team took images of the corona and analyzed them with a polarizing filter. Austrian-American physicist Erwin Saxl and American physicist Mildred Allen reported anomalous changes in the period of a torsion pendulum when observing a partial solar eclipse with a magnitude of 0.954 from Harvard, Massachusetts, called the "Saxl Effect".




In popular culture



CBS showed the first color broadcast of a total eclipse.
This eclipse might be referenced in the second episode of the first season of The Mary Tyler Moore Show when a guest of Mary's accidentally exposes a roll of film that Howard Arnell, an ex-boyfriend of Mary's, says, "It's just the pictures I took of the total eclipse of the sun."
The eclipse may be referenced in the hit popular song “You're So Vain” by Carly Simon, although in context, the lyrics more closely align with a different eclipse two years later.




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 1970

=
A partial lunar eclipse on February 21.
A total solar eclipse on March 7.
A partial lunar eclipse on August 17.
An annular solar eclipse on August 31.




= Metonic

=
Preceded by: Solar eclipse of May 20, 1966
Followed by: Solar eclipse of December 24, 1973




= Tzolkinex

=
Preceded by: Solar eclipse of January 25, 1963
Followed by: Solar eclipse of April 18, 1977




= Half-Saros

=
Preceded by: Lunar eclipse of March 2, 1961
Followed by: Lunar eclipse of March 13, 1979




= Tritos

=
Preceded by: Solar eclipse of April 8, 1959
Followed by: Solar eclipse of February 4, 1981




= Solar Saros 139

=
Preceded by: Solar eclipse of February 25, 1952
Followed by: Solar eclipse of March 18, 1988




= Inex

=
Preceded by: Solar eclipse of March 27, 1941
Followed by: Solar eclipse of February 16, 1999




= Triad

=
Preceded by: Solar eclipse of May 6, 1883
Followed by: Solar eclipse of January 5, 2057




= Solar eclipses of 1968–1971

=
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 22, 1971 occurs in the next lunar year eclipse set.




= Saros 139

=
This eclipse is a part of Saros series 139, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on May 17, 1501. It contains hybrid eclipses from August 11, 1627 through December 9, 1825 and total eclipses from December 21, 1843 through March 26, 2601. There are no annular eclipses in this set. The series ends at member 71 as a partial eclipse on July 3, 2763. 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 will be produced by member 61 at 7 minutes, 29.22 seconds on July 16, 2186. This date is the longest solar eclipse computed between 4000 BC and AD 6000. 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
Maps:

GoogleMap of totality and partiality limits
News:

ABC NEWS 3:40 – March 7, 1970: Total Solar Eclipse The region near Nejapa, Mexico, is first to experience total darkness in midday.
Photos and observations

Russia expedition
Foto Solar eclipse of March 7, 1970
Solar Eclipse Photo Gallery 1 1970–1984, Photographs by Fred Espenak, from Windsor, NC
Observations of coronal polarization at the solar eclipse of 7 March, 1970 Polarigraphic observations of the 7 March 1970 eclipse were made at Miahuatlán (Mexico)
Solar Eclipse of March 7, 1970 Williamston, NC by Gerard M Foley

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