Solar eclipse of April 17, 1912

Last updated
Solar eclipse of April 17, 1912
SE1912Apr17H.png
Map
Type of eclipse
NatureHybrid
Gamma 0.528
Magnitude 1.0003
Maximum eclipse
Duration2 s (0 min 2 s)
Coordinates 38°24′N11°18′W / 38.4°N 11.3°W / 38.4; -11.3
Max. width of band1 km (0.62 mi)
Times (UTC)
Greatest eclipse11:34:22
References
Saros 137 (30 of 70)
Catalog # (SE5000) 9308

A total solar eclipse occurred at the Moon's ascending node of orbit on Wednesday, April 17, 1912, [1] [2] [3] with a magnitude of 1.0003. It was a hybrid event, starting and ending as an annular eclipse, with only a small portion of totality (only 1.3 km (0.808 mi or 4,265 feet) wide). 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 7.4 days after apogee (on April 10, 1912, at 0:50 UTC) and 5.5 days before perigee (on April 22, 1912, at 22:20 UTC), the Moon's apparent diameter was larger. [4]

Contents

Annularity was first visible from southeastern tip of Venezuela, northern tip of Brazil, British Guyana (today's Guyana), Dutch Guiana (today's Suriname) and Porto Santo Island in Madeira, Portugal, then totality from Portugal and Spain, with annularity continuing northeast across France (including northwestern suburbs of Paris), Belgium, Netherlands, Germany and Russian Empire (the parts now belonging to northern Latvia, southern Estonia and Russia). A partial eclipse was visible for parts of eastern South America, eastern North America, West Africa, Europe, and West Asia.

It was the 30th eclipse of the 137th Saros cycle, which began with a partial eclipse on May 25, 1389, and will conclude with a partial eclipse on June 28, 2633. This eclipse occurred two days after the RMS Titanic sank in the northwestern Atlantic Ocean under the darkness of new moon. [5]

Observations

Solar eclipse 1912Apr17 Flammarion.jpg
The Observatory of Paris had the Globule balloon aloft for the 17 April 1912 hybrid eclipse, reported by Camille Flammarion. [6]
Solar eclipse 1912 on cover of Le Petit Journal 21 April 1912.jpg
The Le Petit Journal cover, on 1912 April 21, shows eclipse watchers in 1912 along with the solar eclipse of May 22, 1724, the previous total solar eclipse visible from Paris, France [7]
EclipseBrasilPortugal1May1912.jpg
The 1 May 1912 edition of the luso-Brazilian Brasil-Portugal magazine publishes photographs of the eclipse, as it was seen in Lisbon. An editorial says: "One can tell, on that moment, the mathematical regularity that presides over everything that goes on above and the considerable achievements that the oldest of sciences — Astronomy — has been meeting. While some, strong spirits, point out the fact and point out how precise are scientific calculi, the others, believers, consider that what we can grasp is still too little and, not being able to conceive a Creation without a Creator, pay homage to science but continue to kneel before God. The reader can judge the interest that the phenomenon sparked among us by himself though the photographs that follow, where one can see it all; the wise and the godless, the noble and the commoners, women and men, everyone paid no attention to earthly matters and, for a moment, observed with better or worse instruments what was going on up above. It was even a momentaneous rest for politics."

Eugene Atget, Eclipse, 1912.jpg

During a hybrid solar eclipse, the apex of the moon's umbral cone was very close to the Earth's surface, and the magnitude was very large. The edges of the moon and the sun were very close to each other as seen from the Earth in both the total and annular portion of the path. A series of Baily's beads on the lunar limb provided an excellent opportunity to measure the size and shape of the Earth, as well as the mountains and valleys on the lunar limb. Measurements were made in Europe to locate precisely the limits of the umbral shadow by spreading people every 100 metres along a straight road. [8]

The hybrid solar eclipse of April 28, 1930, also belonging to Solar Saros 137, also occurred with a magnitude close to 1. Similar observations were made near Camptonville, California. Such observations were also made during two later annular solar eclipses of May 9, 1948 in Rebun Island, Japan and May 20, 1966 in Greece and Turkey, also belonging to the same solar Saros cycle. Similar measurements were also done in New York City during the total solar eclipse of January 24, 1925, which did not belong to the same Saros cycle 137 had a magnitude much larger than 1. [8]

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. [9]

April 17, 1912 Solar Eclipse Times
EventTime (UTC)
First Penumbral External Contact1912 April 17 at 08:53:53.3 UTC
First Umbral External Contact1912 April 17 at 10:00:21.2 UTC
First Central Line1912 April 17 at 10:00:52.4 UTC
Greatest Duration1912 April 17 at 10:00:52.4 UTC
First Umbral Internal Contact1912 April 17 at 10:01:23.5 UTC
Greatest Eclipse1912 April 17 at 11:34:21.9 UTC
Ecliptic Conjunction1912 April 17 at 11:40:06.1 UTC
Equatorial Conjunction1912 April 17 at 12:03:39.6 UTC
Last Umbral Internal Contact1912 April 17 at 13:07:04.3 UTC
Last Central Line1912 April 17 at 13:07:32.6 UTC
Last Umbral External Contact1912 April 17 at 13:08:00.8 UTC
Last Penumbral External Contact1912 April 17 at 14:14:32.4 UTC
April 17, 1912 Solar Eclipse Parameters
ParameterValue
Eclipse Magnitude1.00032
Eclipse Obscuration1.00064
Gamma0.52797
Sun Right Ascension01h40m32.0s
Sun Declination+10°26'25.1"
Sun Semi-Diameter15'55.5"
Sun Equatorial Horizontal Parallax08.8"
Moon Right Ascension01h39m36.3s
Moon Declination+10°53'32.1"
Moon Semi-Diameter15'42.9"
Moon Equatorial Horizontal Parallax0°57'40.6"
ΔT13.7 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.

Eclipse season of April 1912
April 1
Descending node (full moon)
April 17
Ascending node (new moon)
Lunar eclipse chart close-1912Apr01.png SE1912Apr17H.png
Partial lunar eclipse
Lunar Saros 111
Hybrid solar eclipse
Solar Saros 137

Eclipses in 1912

Metonic

Tzolkinex

Half-Saros

Tritos

Solar Saros 137

Inex

Triad

Solar eclipses of 1910–1913

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. [10]

The partial solar eclipse on August 31, 1913 occurs in the next lunar year eclipse set.

Solar eclipse series sets from 1910 to 1913
Ascending node Descending node
SarosMapGammaSarosMapGamma
117 May 9, 1910
SE1910May09T.png
Total
−0.9437122 November 2, 1910
SE1910Nov02P.png
Partial
1.0603
127 April 28, 1911
SE1911Apr28T.png
Total
−0.2294132 October 22, 1911
SE1911Oct22A.png
Annular
0.3224
137 April 17, 1912
SE1912Apr17H.png
Hybrid
0.528142 October 10, 1912
SE1912Oct10T.png
Total
−0.4149
147 April 6, 1913
SE1913Apr06P.png
Partial
1.3147152 September 30, 1913
SE1913Sep30P.png
Partial
−1.1005

Saros 137

This eclipse is a part of Saros series 137, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on May 25, 1389. It contains total eclipses from August 20, 1533 through December 6, 1695; the first set of hybrid eclipses from December 17, 1713 through February 11, 1804; the first set of annular eclipses from February 21, 1822 through March 25, 1876; the second set of hybrid eclipses from April 6, 1894 through April 28, 1930; and the second set of annular eclipses from May 9, 1948 through April 13, 2507. The series ends at member 70 as a partial eclipse on June 28, 2633. 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 11 at 2 minutes, 55 seconds on September 10, 1569, and the longest duration of annularity will be produced by member 59 at 7 minutes, 5 seconds on February 28, 2435. All eclipses in this series occur at the Moon’s ascending node of orbit. [11]

Series members 24–46 occur between 1801 and 2200:
242526
SE1804Feb11H.png
February 11, 1804
SE1822Feb21A.png
February 21, 1822
SE1840Mar04A.png
March 4, 1840
272829
SE1858Mar15A.png
March 15, 1858
SE1876Mar25A.png
March 25, 1876
SE1894Apr06H.png
April 6, 1894
303132
SE1912Apr17H.png
April 17, 1912
SE1930Apr28H.png
April 28, 1930
SE1948May09A.png
May 9, 1948
333435
SE1966May20A.png
May 20, 1966
SE1984May30A.png
May 30, 1984
SE2002Jun10A.png
June 10, 2002
363738
SE2020Jun21A.png
June 21, 2020
SE2038Jul02A.png
July 2, 2038
SE2056Jul12A.png
July 12, 2056
394041
SE2074Jul24A.png
July 24, 2074
SE2092Aug03A.png
August 3, 2092
SE2110Aug15A.png
August 15, 2110
424344
SE2128Aug25A.png
August 25, 2128
SE2146Sep06A.png
September 6, 2146
SE2164Sep16A.png
September 16, 2164
4546
SE2182Sep27A.png
September 27, 2182
SE2200Oct09A.png
October 9, 2200

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.

23 eclipse events between February 3, 1859 and June 29, 1946
February 1–3November 21–22September 8–10June 28–29April 16–18
109111113115117
SE1859Feb03P.png
February 3, 1859
SE1862Nov21P.gif
November 21, 1862
SE1870Jun28P.gif
June 28, 1870
SE1874Apr16T.gif
April 16, 1874
119121123125127
SE1878Feb02A.gif
February 2, 1878
SE1881Nov21A.gif
November 21, 1881
SE1885Sep08T.png
September 8, 1885
SE1889Jun28A.png
June 28, 1889
SE1893Apr16T.png
April 16, 1893
129131133135137
SE1897Feb01A.gif
February 1, 1897
SE1900Nov22A.gif
November 22, 1900
SE1904Sep09T.png
September 9, 1904
SE1908Jun28A.png
June 28, 1908
SE1912Apr17H.png
April 17, 1912
139141143145147
SE1916Feb03T.png
February 3, 1916
SE1919Nov22A.png
November 22, 1919
SE1923Sep10T.png
September 10, 1923
SE1927Jun29T.png
June 29, 1927
SE1931Apr18P.png
April 18, 1931
149151153155
SE1935Feb03P.png
February 3, 1935
SE1938Nov21P.png
November 21, 1938
SE1942Sep10P.png
September 10, 1942
SE1946Jun29P.png
June 29, 1946

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
SE1803Feb21T.png
February 21, 1803
(Saros 127)
SE1814Jan21A.gif
January 21, 1814
(Saros 128)
SE1824Dec20Am.gif
December 20, 1824
(Saros 129)
SE1835Nov20T.png
November 20, 1835
(Saros 130)
SE1846Oct20A.png
October 20, 1846
(Saros 131)
SE1857Sep18A.png
September 18, 1857
(Saros 132)
SE1868Aug18T.png
August 18, 1868
(Saros 133)
SE1879Jul19A.png
July 19, 1879
(Saros 134)
SE1890Jun17A.png
June 17, 1890
(Saros 135)
SE1901May18T.png
May 18, 1901
(Saros 136)
SE1912Apr17H.png
April 17, 1912
(Saros 137)
SE1923Mar17A.png
March 17, 1923
(Saros 138)
SE1934Feb14T.png
February 14, 1934
(Saros 139)
SE1945Jan14A.png
January 14, 1945
(Saros 140)
SE1955Dec14A.png
December 14, 1955
(Saros 141)
SE1966Nov12T.png
November 12, 1966
(Saros 142)
SE1977Oct12T.png
October 12, 1977
(Saros 143)
SE1988Sep11A.png
September 11, 1988
(Saros 144)
SE1999Aug11T.png
August 11, 1999
(Saros 145)
SE2010Jul11T.png
July 11, 2010
(Saros 146)
SE2021Jun10A.png
June 10, 2021
(Saros 147)
SE2032May09A.png
May 9, 2032
(Saros 148)
SE2043Apr09T.png
April 9, 2043
(Saros 149)
SE2054Mar09P.png
March 9, 2054
(Saros 150)
SE2065Feb05P.png
February 5, 2065
(Saros 151)
SE2076Jan06T.png
January 6, 2076
(Saros 152)
SE2086Dec06P.png
December 6, 2086
(Saros 153)
SE2097Nov04A.png
November 4, 2097
(Saros 154)
Saros155 11van71 SE2108Oct05T.jpg
October 5, 2108
(Saros 155)
Saros156 07van69 SE2119Sep05P.jpg
September 5, 2119
(Saros 156)
Saros157 05van70 SE2130Aug04P.jpg
August 4, 2130
(Saros 157)
Saros158 05van70 SE2141Jul03P.jpg
July 3, 2141
(Saros 158)
Saros159 02van70 SE2152Jun03P.jpg
June 3, 2152
(Saros 159)
Saros161 01van72 SE2174Apr01P.jpg
April 1, 2174
(Saros 161)

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
SE1825Jun16H.png
June 16, 1825
(Saros 134)
SE1854May26A.png
May 26, 1854
(Saros 135)
SE1883May06T.png
May 6, 1883
(Saros 136)
SE1912Apr17H.png
April 17, 1912
(Saros 137)
SE1941Mar27A.png
March 27, 1941
(Saros 138)
SE1970Mar07T.png
March 7, 1970
(Saros 139)
SE1999Feb16A.png
February 16, 1999
(Saros 140)
SE2028Jan26A.png
January 26, 2028
(Saros 141)
SE2057Jan05T.png
January 5, 2057
(Saros 142)
SE2085Dec16A.png
December 16, 2085
(Saros 143)
SE2114Nov27A.png
November 27, 2114
(Saros 144)
SE2143Nov07T.png
November 7, 2143
(Saros 145)
SE2172Oct17H.png
October 17, 2172
(Saros 146)

Notes

  1. "April 17, 1912 Total Solar Eclipse". timeanddate. Retrieved 31 July 2024.
  2. "TO'DAY'S ECLIPSE OF THE SUN". The Guardian. London, Greater London, England. 1912-04-17. p. 16. Retrieved 2023-11-04 via Newspapers.com.
  3. "Few saw eclipse". The Brooklyn Daily Eagle. Brooklyn, New York. 1912-04-17. p. 20. Retrieved 2023-11-04 via Newspapers.com.
  4. "Moon Distances for London, United Kingdom, England". timeanddate. Retrieved 31 July 2024.
  5. www.astronomeer.com: The "Titanic" eclipse of 17 April 1912 Archived 7 January 2009 at the Wayback Machine The last annular eclipse in the Netherlands was 17 April 1912, just two days after the Titanic hit an iceberg and sank.
  6. Archived 2009-05-30 at the Wayback Machine Societe Astronomique, pp. 234–248, 1912 – By Camille Flammarion (Translation from French by LRM) p. 240 "A balloon dirigible, having on board Admiral Fournier and Colonel Bourgeois permitted good perception of the moon's shadow at a speed of 800 m/sec ... From a captive balloon near Saint-Nom-de-la-Breteche, Captain Dupic made analogous observations which confirmed those made from the dirigible."
  7. 17th April 1912: Eclipse fever grips Europe Archived 2011-07-16 at the Wayback Machine
  8. 1 2 Xavier M. Jubier. "Eclipse hybride de Soleil du 17 avril 1912 en Europe (Hybrid Solar Eclipse of 1912 April 17 over Europe)". Archived from the original on 24 January 2019.
  9. "Hybrid Solar Eclipse of 1912 Apr 17". EclipseWise.com. Retrieved 31 July 2024.
  10. 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.
  11. "NASA - Catalog of Solar Eclipses of Saros 137". eclipse.gsfc.nasa.gov.

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<span class="mw-page-title-main">Solar eclipse of May 29, 1938</span> Total eclipse

A total solar eclipse occurred at the Moon's descending node of orbit on Sunday, May 29, 1938, with a magnitude of 1.0552. 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.

<span class="mw-page-title-main">Solar eclipse of March 17, 1923</span> 20th-century annular solar eclipse

An annular solar eclipse occurred at the Moon's descending node of orbit on Saturday, March 17, 1923, with a magnitude of 0.931. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Annularity was visible from Chile, Argentina, Falkland Islands including capital Stanley, Gough Island in Tristan da Cunha, South West Africa, Bechuanaland Protectorate (today's Botswana, Southern Rhodesia including capital Salisbury, Portuguese Mozambique, Nyasaland, French Madagascar.

<span class="mw-page-title-main">Solar eclipse of October 1, 1921</span> Total eclipse

A total solar eclipse occurred at the Moon's ascending node of orbit on Saturday, October 1, 1921, with a magnitude of 1.0293. 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.

<span class="mw-page-title-main">Solar eclipse of April 8, 1921</span> 20th-century annular solar eclipse

An annular solar eclipse occurred at the Moon's descending node of orbit on Friday, April 8, 1921, with a magnitude of 0.9753. 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. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Annularity was visible from northern Scotland, northwestern tip of Norway, and islands in the Arctic Ocean in Russian SFSR.

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