Solar eclipse of July 11, 1991

Last updated
Solar eclipse of July 11, 1991
Eclipse CR 1991 a zoom.jpg
Totality from Playas del Coco, Costa Rica
SE1991Jul11T.png
Map
Type of eclipse
NatureTotal
Gamma −0.0041
Magnitude 1.08
Maximum eclipse
Duration413 s (6 min 53 s)
Coordinates 22°00′N105°12′W / 22°N 105.2°W / 22; -105.2
Max. width of band258 km (160 mi)
Times (UTC)
(P1) Partial begin16:28:46
(U1) Total begin17:21:41
Greatest eclipse19:07:01
(U4) Total end20:50:28
(P4) Partial end21:43:24
References
Saros 136 (36 of 71)
Catalog # (SE5000) 9489

A total solar eclipse occurred at the Moon's descending node of orbit on Thursday, July 11, 1991, [1] with a magnitude of 1.08. 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 8 hours after perigee (on July 11, 1991, at 11:00 UTC), the Moon's apparent diameter was larger. [2]

Contents

The eclipse lasted for 6 minutes and 53.08 seconds at the point of maximum eclipse. There will not be a longer total eclipse until June 13, 2132. This was the largest total solar eclipse of Solar Saros series 136. This eclipse was the most central total eclipse in 800 years, with a gamma of −0.00412. There will not be a more central eclipse for another 800 years. Its magnitude was also greater than any eclipse since the 6th century.

Totality began over the Pacific Ocean and Hawaii, moving across Mexico, down through the Central American countries of Guatemala, El Salvador, Honduras, Nicaragua, Costa Rica and Panama, across Colombia and ending over Brazil. A partial eclipse was visible for parts of southern Canada, the United States, Mexico, Central America, the Caribbean, and South America.

Observations

An observation team funded by the National Natural Science Foundation of China made near-infrared spectroscopic observations in the southern suburbs of La Paz, Baja California Sur, Mexico. Weather was clear on the eclipse day in La Paz. The team captured dozens of frames of the slitless spectrum of the upper layer of photosphere and chromosphere, and the slit spectrum outside the solar surface. They also captured images of the chromosphere and solar prominences. Among the professional observation teams from various countries to La Paz, six used the new CCD sensors for the first time in solar eclipse observation. Among them, the Chinese and Japanese team used it to observe long-wavelength spectra. [3] A team of 320 people from NASA's Johnson Space Center made observation in Mazatlán, Mexico. The local weather was not ideal in the days before the eclipse, but got slightly better as the eclipse day approached. Some people went to San Blas, Nayarit for better weather conditions. In the end, a hole in the clouds appeared in El Cid in western Mazatlan, through which the corona and prominences was visible. Other observers 1 to 5 miles away were clouded out. In San Blas, the corona and prominences were still visible, even though the clouds became thicker during totality. [4] Scientists from the Royal Observatory of Belgium, the Institute of Geodesy and Geophysics of the Chinese Academy of Sciences, and the Institute of Geophysics of the National Autonomous University of Mexico made observations in Mexico City to study the change in gravity during a total solar eclipse. [5]

Alleged ancient Maya prediction

The American ethnographer and anthropologist Victoria Bricker and her late husband and colleague Harvey Bricker, claim in their book "Astronomy in the Maya Codices" that by decoding pre-Columbian glyphs from the four Maya codices they discovered that pre-16th century Maya astronomers predicted the solar eclipse of July 11, 1991. [6] In their 2011 volume, the husband-wife Brickers team explain how they translated the dates from the Maya calendar, then used modern scientific knowledge of planetary orbits to line up the data from the Maya prediction with the Gregorian calendar. [7] Reviewers disputed the claim in 2014, concluding that, "loose hieroglyphic readings and accommodating pattern matching occurs throughout the book." [8]

The 1991 eclipse appears in the music video for Cosas del Amor , a duet by Vikki Carr and Ana Gabriel. [9]

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. [10]

July 11, 1991 Solar Eclipse Times
EventTime (UTC)
First Penumbral External Contact1991 July 11 at 16:29:42.3 UTC
First Umbral External Contact1991 July 11 at 17:22:36.8 UTC
First Central Line1991 July 11 at 17:24:13.8 UTC
First Umbral Internal Contact1991 July 11 at 17:25:50.7 UTC
First Penumbral Internal Contact1991 July 11 at 18:18:45.5 UTC
Greatest Duration1991 July 11 at 19:01:51.6 UTC
Greatest Eclipse1991 July 11 at 19:07:00.8 UTC
Ecliptic Conjunction1991 July 11 at 19:07:03.3 UTC
Equatorial Conjunction1991 July 11 at 19:07:07.0 UTC
Last Penumbral Internal Contact1991 July 11 at 19:55:15.7 UTC
Last Umbral Internal Contact1991 July 11 at 20:48:11.3 UTC
Last Central Line1991 July 11 at 20:49:47.8 UTC
Last Umbral External Contact1991 July 11 at 20:51:24.3 UTC
Last Penumbral External Contact1991 July 11 at 21:44:20.2 UTC
July 11, 1991 Solar Eclipse Parameters
ParameterValue
Eclipse Magnitude1.07997
Eclipse Obscuration1.16633
Gamma−0.00412
Sun Right Ascension07h22m12.8s
Sun Declination+22°05'48.5"
Sun Semi-Diameter15'43.9"
Sun Equatorial Horizontal Parallax08.7"
Moon Right Ascension07h22m12.5s
Moon Declination+22°05'33.9"
Moon Semi-Diameter16'42.1"
Moon Equatorial Horizontal Parallax1°01'17.7"
ΔT57.9 s

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. The first and last eclipse in this sequence is separated by one synodic month.

Eclipse season of June–July 1991
June 27
Ascending node (full moon)
 July 11
Descending node (new moon)
 July 26
Ascending node (full moon)
Lunar eclipse chart close-1991Jun27.png SE1991Jul11T.png Lunar eclipse chart close-1991Jul26.png
Penumbral lunar eclipse
Lunar Saros 110		 Total solar eclipse
Solar Saros 136		 Penumbral lunar eclipse
Lunar Saros 148

Eclipses in 1991

Metonic

Tzolkinex

Half-Saros

Tritos

Solar Saros 136

Inex

Triad

Solar eclipses of 1990–1992

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. [11]

Solar eclipse series sets from 1990 to 1992
Ascending node Descending node
SarosMapGammaSarosMapGamma
121 January 26, 1990
SE1990Jan26A.png
Annular		−0.9457126
1990.04 Pimennys (28866343838) (cropped).jpg
Partial in Finland 		July 22, 1990
SE1990Jul22T.png
Total		0.7597
131 January 15, 1991
SE1991Jan15A.png
Annular		−0.2727136
Eclipse CR 1991 a zoom.jpg
Totality in Playas del Coco,
Costa Rica 		July 11, 1991
SE1991Jul11T.png
Total		−0.0041
141 January 4, 1992
SE1992Jan04A.png
Annular		0.4091146 June 30, 1992
SE1992Jun30T.png
Total		−0.7512
151 December 24, 1992
SE1992Dec24P.png
Partial		1.0711

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. [12]

Series members 26–47 occur between 1801 and 2200:
262728
SE1811Mar24T.png
March 24, 1811		 SE1829Apr03T.png
April 3, 1829		 SE1847Apr15T.png
April 15, 1847
293031
SE1865Apr25T.gif
April 25, 1865 		SE1883May06T.png
May 6, 1883 		SE1901May18T.png
May 18, 1901
323334
SE1919May29T.png
May 29, 1919 		SE1937Jun08T.png
June 8, 1937 		SE1955Jun20T.png
June 20, 1955
353637
SE1973Jun30T.png
June 30, 1973 		SE1991Jul11T.png
July 11, 1991 		SE2009Jul22T.png
July 22, 2009
383940
SE2027Aug02T.png
August 2, 2027 		SE2045Aug12T.png
August 12, 2045 		SE2063Aug24T.png
August 24, 2063
414243
SE2081Sep03T.png
September 3, 2081 		SE2099Sep14T.png
September 14, 2099 		SE2117Sep26T.png
September 26, 2117
444546
SE2135Oct07T.png
October 7, 2135		 SE2153Oct17T.png
October 17, 2153		 SE2171Oct29T.png
October 29, 2171
47
SE2189Nov08T.png
November 8, 2189

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.

21 eclipse events between July 11, 1953 and July 11, 2029
July 10–11April 29–30February 15–16December 4September 21–23
116118120122124
SE1953Jul11P.png
July 11, 1953 		SE1957Apr30A.png
April 30, 1957 		SE1961Feb15T.png
February 15, 1961 		SE1964Dec04P.png
December 4, 1964 		SE1968Sep22T.png
September 22, 1968
126128130132134
SE1972Jul10T.png
July 10, 1972 		SE1976Apr29A.png
April 29, 1976 		SE1980Feb16T.png
February 16, 1980 		SE1983Dec04A.png
December 4, 1983 		SE1987Sep23A.png
September 23, 1987
136138140142144
SE1991Jul11T.png
July 11, 1991 		SE1995Apr29A.png
April 29, 1995 		SE1999Feb16A.png
February 16, 1999 		SE2002Dec04T.png
December 4, 2002 		SE2006Sep22A.png
September 22, 2006
146148150152154
SE2010Jul11T.png
July 11, 2010 		SE2014Apr29A.png
April 29, 2014 		SE2018Feb15P.png
February 15, 2018 		SE2021Dec04T.png
December 4, 2021 		SE2025Sep21P.png
September 21, 2025
156
SE2029Jul11P.png
July 11, 2029

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.

Series members between 1801 and 2200
SE1805Dec21A.gif
December 21, 1805
(Saros 119)		 SE1816Nov19T.gif
November 19, 1816
(Saros 120)		 SE1827Oct20H.gif
October 20, 1827
(Saros 121)		 SE1838Sep18A.gif
September 18, 1838
(Saros 122)		 SE1849Aug18T.gif
August 18, 1849
(Saros 123)
SE1860Jul18T.gif
July 18, 1860
(Saros 124)		 SE1871Jun18A.gif
June 18, 1871
(Saros 125)		 SE1882May17T.png
May 17, 1882
(Saros 126)		 SE1893Apr16T.png
April 16, 1893
(Saros 127)		 SE1904Mar17A.png
March 17, 1904
(Saros 128)
SE1915Feb14A.png
February 14, 1915
(Saros 129)		 SE1926Jan14T.png
January 14, 1926
(Saros 130)		 SE1936Dec13A.png
December 13, 1936
(Saros 131)		 SE1947Nov12A.png
November 12, 1947
(Saros 132)		 SE1958Oct12T.png
October 12, 1958
(Saros 133)
SE1969Sep11A.png
September 11, 1969
(Saros 134)		 SE1980Aug10A.png
August 10, 1980
(Saros 135)		 SE1991Jul11T.png
July 11, 1991
(Saros 136)		 SE2002Jun10A.png
June 10, 2002
(Saros 137)		 SE2013May10A.png
May 10, 2013
(Saros 138)
SE2024Apr08T.png
April 8, 2024
(Saros 139)		 SE2035Mar09A.png
March 9, 2035
(Saros 140)		 SE2046Feb05A.png
February 5, 2046
(Saros 141)		 SE2057Jan05T.png
January 5, 2057
(Saros 142)		 SE2067Dec06H.png
December 6, 2067
(Saros 143)
SE2078Nov04A.png
November 4, 2078
(Saros 144)		 SE2089Oct04T.png
October 4, 2089
(Saros 145)		 SE2100Sep04T.png
September 4, 2100
(Saros 146)		 SE2111Aug04A.png
August 4, 2111
(Saros 147)		 Saros148 27van75 SE2122Jul04T.jpg
July 4, 2122
(Saros 148)
SE2133Jun03T.png
June 3, 2133
(Saros 149)		 Saros150 24van71 SE2144May03A.jpg
May 3, 2144
(Saros 150)		 SE2155Apr02A.png
April 2, 2155
(Saros 151)		 Saros152 21van70 SE2166Mar02T.jpg
March 2, 2166
(Saros 152)		 Saros153 18van70 SE2177Jan29A.jpg
January 29, 2177
(Saros 153)
Saros154 16van71 SE2187Dec29A.jpg
December 29, 2187
(Saros 154)		 SE2198Nov28T.png
November 28, 2198
(Saros 155)

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.

Series members between 1801 and 2200
SE1817Nov09T.png
November 9, 1817
(Saros 130)		 SE1846Oct20A.png
October 20, 1846
(Saros 131)		 SE1875Sep29A.png
September 29, 1875
(Saros 132)
SE1904Sep09T.png
September 9, 1904
(Saros 133)		 SE1933Aug21A.png
August 21, 1933
(Saros 134)		 SE1962Jul31A.png
July 31, 1962
(Saros 135)
SE1991Jul11T.png
July 11, 1991
(Saros 136)		 SE2020Jun21A.png
June 21, 2020
(Saros 137)		 SE2049May31A.png
May 31, 2049
(Saros 138)
SE2078May11T.png
May 11, 2078
(Saros 139)		 SE2107Apr23A.png
April 23, 2107
(Saros 140)		 SE2136Apr01A.png
April 1, 2136
(Saros 141)
SE2165Mar12T.png
March 12, 2165
(Saros 142)		 SE2194Feb21A.png
February 21, 2194
(Saros 143)

Notes

  1. ↑ "July 11, 1991 Total Solar Eclipse". timeanddate. Retrieved 10 August 2024.
  2. ↑ "Moon Distances for London, United Kingdom, England". timeanddate. Retrieved 10 August 2024.
  3. ↑ You Jianxi, Lu Jing, Wang Chuanjin, Lu Baoluo, Ming Changrong (July 1994). "1991年7月1日墨西哥日全食红外光谱观测及初步结果". 天体物理学报 (Journal of Astrophysics) (in Chinese). 14 (3): 277–282.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  4. ↑ Paul D. Maley. "The Longest Total Solar Eclipse in Mexico – July 11, 1991". Archived from the original on 30 October 2020.
  5. ↑ B. Ducarme, H.-P. Sun, N. d'Oreye, M. Van Ruymbeke, J. Mena Jara (1999). "Interpretation of the tidal residuals during the 11 July 1991 total solar eclipse". Journal of Geodesy. 73: 53–57. Archived from the original on 1 September 2019.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  6. ↑ Solar System, Exploration. "Eclipses". solarsystem.nasa.gov. Nasa. Retrieved December 21, 2022.
  7. ↑ Kramer, Miriam (January 8, 2013). "Ancient Maya Predicted 1991 Solar Eclipse". Live Science. Retrieved April 13, 2023.
  8. ↑ Gerardo Aldana (March 2014). "ISIS: An International Review Devoted to the History of Science and to Cultural Influences". The University of Chicago Press Journals. 105 (1). doi:10.1086/676751. JSTOR   10.1086/676751 . Retrieved 21 April 2024.
  9. ↑ Kellner, Elena (7 November 1991). "ENTERTAINMENT". Los Angeles Times. Retrieved 5 June 2024.
  10. ↑ "Total Solar Eclipse of 1991 Jul 11". EclipseWise.com. Retrieved 10 August 2024.
  11. ↑ van Gent, R.H. "Solar- and Lunar-Eclipse Predictions from Antiquity to the Present". A Catalogue of Eclipse Cycles. Utrecht University. Retrieved 6 October 2018.
  12. ↑ "NASA - Catalog of Solar Eclipses of Saros 136". eclipse.gsfc.nasa.gov.

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A total solar eclipse occurred at the Moon's ascending node of orbit on Sunday, August 29, 1886, with a magnitude of 1.0735. 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 only about 4 hours after perigee, the Moon's apparent diameter was larger.

<span class="mw-page-title-main">Solar eclipse of May 17, 1882</span> Total eclipse

A total solar eclipse occurred at the Moon's descending node of orbit on Wednesday, May 17, 1882, with a magnitude of 1.0200. 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 4.2 days after perigee, the Moon's apparent diameter was larger.

<span class="mw-page-title-main">Solar eclipse of April 6, 1875</span> Total eclipse

A total solar eclipse occurred at the Moon's ascending node of orbit on Tuesday, April 6, 1875, with a magnitude of 1.0547. 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 1.2 days before perigee, the Moon's apparent diameter was larger.

<span class="mw-page-title-main">Solar eclipse of December 12, 1871</span> Total eclipse

A total solar eclipse occurred at the Moon's descending node of orbit on Tuesday, December 12, 1871, with a magnitude of 1.0465. 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 only about 10.5 hours before perigee, the Moon's apparent diameter was larger.

<span class="mw-page-title-main">Solar eclipse of March 25, 1857</span> Total eclipse

A total solar eclipse occurred at the Moon's ascending node of orbit between Wednesday, March 25 and Thursday, March 26, 1857, with a magnitude of 1.0534. 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 1.1 days before perigee, the Moon's apparent diameter was larger.

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