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Solar eclipse of May 18, 1920

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Solar eclipse of May 18, 1920
Map
Type of eclipse
NaturePartial
Gamma−1.0239
Magnitude0.9734
Maximum eclipse
Coordinates69°06′S 107°42′E / 69.1°S 107.7°E / -69.1; 107.7
Times (UTC)
Greatest eclipse6:14:55
References
Saros146 (22 of 76)
Catalog # (SE5000)9328

A partial solar eclipse occurred at the Moon's descending node of orbit on Tuesday, May 18, 1920,[1] with a magnitude of 0.9734. 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 partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth.

A partial eclipse was visible for parts of Australia and Antarctica.

Eclipse details

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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.[2]

May 18, 1920 Solar Eclipse Times
Event Time (UTC)
First Penumbral External Contact 1920 May 18 at 04:17:02.5 UTC
Equatorial Conjunction 1920 May 18 at 06:00:25.5 UTC
Greatest Eclipse 1920 May 18 at 06:14:55.0 UTC
Ecliptic Conjunction 1920 May 18 at 06:25:08.5 UTC
Last Penumbral External Contact 1920 May 18 at 08:12:51.9 UTC
May 18, 1920 Solar Eclipse Parameters
Parameter Value
Eclipse Magnitude 0.97341
Eclipse Obscuration 0.97587
Gamma −1.02391
Sun Right Ascension 03h38m46.6s
Sun Declination +19°29'30.0"
Sun Semi-Diameter 15'48.4"
Sun Equatorial Horizontal Parallax 08.7"
Moon Right Ascension 03h39m22.1s
Moon Declination +18°27'48.5"
Moon Semi-Diameter 16'36.5"
Moon Equatorial Horizontal Parallax 1°00'57.1"
ΔT 21.6 s

Eclipse season

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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.

Eclipse season of May 1920
May 3
Ascending node (full moon)
May 18
Descending node (new moon)
Total lunar eclipse
Lunar Saros 120
Partial solar eclipse
Solar Saros 146
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Eclipses in 1920

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Metonic

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Tzolkinex

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Half-Saros

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Tritos

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Solar Saros 146

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Inex

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Triad

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Solar eclipses of 1916–1920

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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.[3]

The solar eclipses on February 3, 1916 (total), July 30, 1916 (annular), January 23, 1917 (partial), and July 19, 1917 (partial) occur in the previous lunar year eclipse set.

Solar eclipse series sets from 1916 to 1920
Ascending node   Descending node
Saros Map Gamma Saros Map Gamma
111 December 24, 1916

Partial
−1.5321 116 June 19, 1917

Partial
1.2857
121 December 14, 1917

Annular
−0.9157 126 June 8, 1918

Total
0.4658
131 December 3, 1918

Annular
−0.2387 136

Totality in Príncipe
May 29, 1919

Total
−0.2955
141 November 22, 1919

Annular
0.4549 146 May 18, 1920

Partial
−1.0239
151 November 10, 1920

Partial
1.1287

Saros 146

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This eclipse is a part of Saros series 146, repeating every 18 years, 11 days, and containing 76 events. The series started with a partial solar eclipse on September 19, 1541. It contains total eclipses from May 29, 1938 through October 7, 2154; hybrid eclipses from October 17, 2172 through November 20, 2226; and annular eclipses from November 30, 2244 through August 10, 2659. The series ends at member 76 as a partial eclipse on December 29, 2893. 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 was produced by member 26 at 5 minutes, 21 seconds on June 30, 1992, and the longest duration of annularity will be produced by member 63 at 3 minutes, 30 seconds on August 10, 2659. All eclipses in this series occur at the Moon’s descending node of orbit.[4]

Series members 16–37 occur between 1801 and 2200:
16 17 18

March 13, 1812

March 24, 1830

April 3, 1848
19 20 21

April 15, 1866

April 25, 1884

May 7, 1902
22 23 24

May 18, 1920

May 29, 1938

June 8, 1956
25 26 27

June 20, 1974

June 30, 1992

July 11, 2010
28 29 30

July 22, 2028

August 2, 2046

August 12, 2064
31 32 33

August 24, 2082

September 4, 2100

September 15, 2118
34 35 36

September 26, 2136

October 7, 2154

October 17, 2172
37

October 29, 2190

Metonic series

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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.

22 eclipse events between March 5, 1848 and July 30, 1935
March 5–6 December 22–24 October 9–11 July 29–30 May 17–18
108 110 112 114 116

March 5, 1848

July 29, 1859

May 17, 1863
118 120 122 124 126

March 6, 1867

December 22, 1870

October 10, 1874

July 29, 1878

May 17, 1882
128 130 132 134 136

March 5, 1886

December 22, 1889

October 9, 1893

July 29, 1897

May 18, 1901
138 140 142 144 146

March 6, 1905

December 23, 1908

October 10, 1912

July 30, 1916

May 18, 1920
148 150 152 154

March 5, 1924

December 24, 1927

October 11, 1931

July 30, 1935

Tritos series

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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.

The partial solar eclipse on November 4, 2116 (part of Saros 164) is also a part of this series but is not included in the table below.

Series members between 1801 and 2029

March 24, 1811
(Saros 136)

February 21, 1822
(Saros 137)

January 20, 1833
(Saros 138)

December 21, 1843
(Saros 139)

November 20, 1854
(Saros 140)

October 19, 1865
(Saros 141)

September 17, 1876
(Saros 142)

August 19, 1887
(Saros 143)

July 18, 1898
(Saros 144)

June 17, 1909
(Saros 145)

May 18, 1920
(Saros 146)

April 18, 1931
(Saros 147)

March 16, 1942
(Saros 148)

February 14, 1953
(Saros 149)

January 14, 1964
(Saros 150)

December 13, 1974
(Saros 151)

November 12, 1985
(Saros 152)

October 12, 1996
(Saros 153)

September 11, 2007
(Saros 154)

August 11, 2018
(Saros 155)

July 11, 2029
(Saros 156)

Inex series

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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

August 5, 1804
(Saros 142)

July 17, 1833
(Saros 143)

June 27, 1862
(Saros 144)

June 6, 1891
(Saros 145)

May 18, 1920
(Saros 146)

April 28, 1949
(Saros 147)

April 7, 1978
(Saros 148)

March 19, 2007
(Saros 149)

February 27, 2036
(Saros 150)

February 5, 2065
(Saros 151)

January 16, 2094
(Saros 152)

December 28, 2122
(Saros 153)

December 8, 2151
(Saros 154)

November 17, 2180
(Saros 155)

Notes

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  1. ^ "May 18, 1920 Partial Solar Eclipse". timeanddate. Retrieved 1 August 2024.
  2. ^ "Partial Solar Eclipse of 1920 May 18". EclipseWise.com. Retrieved 1 August 2024.
  3. ^ 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.
  4. ^ "NASA - Catalog of Solar Eclipses of Saros 146". eclipse.gsfc.nasa.gov.

References

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