Solar eclipse of July 28, 1851

Last updated
Solar eclipse of July 28, 1851
1851 07 28 Berkowski.jpg
Berkowski made this first solar eclipse photograph at the Royal Observatory in Königsberg, Prussia (now Kaliningrad, Russia)
SE1851Jul28T.png
Map
Type of eclipse
NatureTotal
Gamma 0.7644
Magnitude 1.0577
Maximum eclipse
Duration221 s (3 min 41 s)
Coordinates 68°00′N19°36′W / 68°N 19.6°W / 68; -19.6
Max. width of band296 km (184 mi)
Times (UTC)
Greatest eclipse14:33:42
References
Saros 143 (14 of 72)
Catalog # (SE5000) 9167

A total solar eclipse occurred at the Moon's ascending node of orbit on Monday, July 28, 1851, with a magnitude of 1.0577. 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 1.5 days before perigee (on July 30, 1851, at 2:30 UTC), the Moon's apparent diameter was larger. [1]

Contents

The path of totality was visible from parts of modern-day Canada, Greenland, Iceland, Norway, Sweden, Denmark, Poland, Russia, southwestern Lithuania, Belarus, Ukraine, Moldova, Georgia, Armenia, and Azerbaijan. A partial solar eclipse was also visible for parts of North America, Europe, North Africa, Russia, the Middle East, and Central Asia.

This was the earliest scientifically useful photograph of a total solar eclipse, made by Julius Berkowski at the Royal Observatory in Königsberg, Prussia. It was the first occasion that an accurate photographic image of a solar eclipse was recorded.

Background

A solar eclipse occurs when the Moon passes between the Earth and the Sun, casting a shadow on Earth that temporarily obscures part or all of the Sun's disc. Eclipses can occur only when all three bodies are properly aligned. Partial eclipses, in which only a portion of the Sun's surface is obscured, are relatively common due to the width of the Moon's outer shadow, or penumbra, which may be several hundred miles wide. Total eclipses occur when the Moon's inner shadow, or umbra, reaches the surface of the Earth, completely obscuring the Sun over a much narrower portion of the ground. If the Moon is too far away at the time of an eclipse, its umbra may not reach the Earth's surface, and only a partial eclipse will be visible.

Before the advent of modern science, solar eclipses were often viewed with superstitious dread. However, eclipses are also of interest to science due to the various phenomena that can be observed when they occur. The Sun's outer atmosphere, or corona, is normally invisible due to the brightness of the solar disc, but becomes visible from Earth during a total eclipse. Until the twentieth century, solar eclipses provided the only opportunity for scientists to observe and study the Sun's corona. With the development of photography during the first half of the nineteenth century, it became theoretically possible to record a still image of the Sun during a total eclipse. A variety of processes were used for early photographs, of which the most successful was the daguerreotype.

Monday, July 28, 1851

From Paris Les parisiens pendant l'eclipse du 28 Juillet.jpg
From Paris

Photographing a rare event such as a total eclipse posed unique challenges for early photography, including the extreme contrast between the corona and the dark shadow of the Moon, as well as the unusual angle to which photographic equipment had to be oriented. Prior to the eclipse of July 28, 1851, no properly exposed photograph of the solar corona had yet been produced. For this occasion, the Royal Prussian Observatory at Königsberg (now Kaliningrad, Russia) commissioned one of the city's most skilled daguerreotypists, Johann Julius Friedrich Berkowski, to record a still image of the event. [2] The observers attached a small six-centimeter refracting telescope to a 15.8 centimeter Fraunhofer heliometer, and Berkowski made an eighty-four second exposure shortly after the beginning of totality. [3]

Among the other observers were British astronomers Robert Grant and William Swan, and Austrian astronomer Karl Ludwig von Littrow. They deduced that prominences were part of the Sun, because the Moon was seen to cover and uncover them as it moved in front of the Sun. [4] [ better source needed ]

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. [5]

July 28, 1851 Solar Eclipse Times
EventTime (UTC)
First Penumbral External Contact1851 July 28 at 12:15:06.1 UTC
First Umbral External Contact1851 July 28 at 13:24:53.6 UTC
First Central Line1851 July 28 at 13:26:48.7 UTC
First Umbral Internal Contact1851 July 28 at 13:28:45.8 UTC
Equatorial Conjunction1851 July 28 at 14:21:59.0 UTC
Greatest Eclipse1851 July 28 at 14:33:41.9 UTC
Greatest Duration1851 July 28 at 14:33:48.3 UTC
Ecliptic Conjunction1851 July 28 at 14:41:27.8 UTC
Last Umbral Internal Contact1851 July 28 at 15:38:44.7 UTC
Last Central Line1851 July 28 at 15:40:43.2 UTC
Last Umbral External Contact1851 July 28 at 15:42:39.8 UTC
Last Penumbral External Contact1851 July 28 at 16:52:19.9 UTC
July 28, 1851 Solar Eclipse Parameters
ParameterValue
Eclipse Magnitude1.05765
Eclipse Obscuration1.11863
Gamma0.76436
Sun Right Ascension08h28m49.7s
Sun Declination+19°03'55.7"
Sun Semi-Diameter15'45.2"
Sun Equatorial Horizontal Parallax08.7"
Moon Right Ascension08h29m18.2s
Moon Declination+19°49'34.3"
Moon Semi-Diameter16'29.2"
Moon Equatorial Horizontal Parallax1°00'30.3"
ΔT7.1 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 July 1851
July 13
Descending node (full moon)
July 28
Ascending node (new moon)
SE1851Jul28T.png
Partial lunar eclipse
Lunar Saros 117
Total solar eclipse
Solar Saros 143

Eclipses in 1851

Metonic

Tzolkinex

Half-Saros

Tritos

Solar Saros 143

Inex

Triad

Solar eclipses of 1848–1852

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. [6]

The partial solar eclipses on April 3, 1848 and September 27, 1848 occur in the previous lunar year eclipse set, and the solar eclipses on June 17, 1852 (partial) and December 11, 1852 (total) occur in the next lunar year eclipse set.

Solar eclipse series sets from 1848 to 1852
Descending node Ascending node
SarosMapGammaSarosMapGamma
108March 5, 1848
SE1848Mar05P.gif
Partial
1.3950113August 28, 1848
SE1848Aug28P.gif
Partial
−1.5475
118February 23, 1849
SE1849Feb23A.gif
Annular
0.7475123August 18, 1849
SE1849Aug18T.gif
Total
−0.7343
128February 12, 1850
SE1850Feb12A.gif
Annular
0.0503133August 7, 1850
SE1850Aug07T.gif
Total
0.0215
138February 1, 1851
SE1851Feb01A.gif
Annular
−0.6413143 July 28, 1851
SE1851Jul28T.png
Total
0.7644
148 January 21, 1852
SE1852Jan21P.png
Partial
−1.2948

Saros 143

This eclipse is a part of Saros series 143, repeating every 18 years, 11 days, and containing 72 events. The series started with a partial solar eclipse on March 7, 1617. It contains total eclipses from June 24, 1797 through October 24, 1995; hybrid eclipses from November 3, 2013 through December 6, 2067; and annular eclipses from December 16, 2085 through September 16, 2536. The series ends at member 72 as a partial eclipse on April 23, 2897. 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 16 at 3 minutes, 50 seconds on August 19, 1887, and the longest duration of annularity will be produced by member 51 at 4 minutes, 54 seconds on September 6, 2518. All eclipses in this series occur at the Moon’s ascending node of orbit. [7]

Series members 12–33 occur between 1801 and 2200:
121314
SE1815Jul06T.png
July 6, 1815
SE1833Jul17T.png
July 17, 1833
SE1851Jul28T.png
July 28, 1851
151617
SE1869Aug07T.png
August 7, 1869
SE1887Aug19T.png
August 19, 1887
SE1905Aug30T.png
August 30, 1905
181920
SE1923Sep10T.png
September 10, 1923
SE1941Sep21T.png
September 21, 1941
SE1959Oct02T.png
October 2, 1959
212223
SE1977Oct12T.png
October 12, 1977
SE1995Oct24T.png
October 24, 1995
SE2013Nov03H.png
November 3, 2013
242526
SE2031Nov14H.png
November 14, 2031
SE2049Nov25H.png
November 25, 2049
SE2067Dec06H.png
December 6, 2067
272829
SE2085Dec16A.png
December 16, 2085
SE2103Dec29A.png
December 29, 2103
SE2122Jan08A.png
January 8, 2122
303132
SE2140Jan20A.png
January 20, 2140
SE2158Jan30A.png
January 30, 2158
SE2176Feb10A.png
February 10, 2176
33
SE2194Feb21A.png
February 21, 2194

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.

24 eclipse events between March 4, 1802 and July 28, 1870
March 4December 20–21October 8–9July 27–28May 15–16
117119121123125
SE1802Mar04T.png
March 4, 1802
SE1805Dec21A.gif
December 21, 1805
SE1809Oct09T.gif
October 9, 1809
SE1813Jul27T.gif
July 27, 1813
SE1817May16A.gif
May 16, 1817
127129131133135
SE1821Mar04T.gif
March 4, 1821
SE1824Dec20Am.gif
December 20, 1824
SE1828Oct09A.gif
October 9, 1828
SE1832Jul27T.gif
July 27, 1832
SE1836May15A.gif
May 15, 1836
137139141143145
SE1840Mar04A.gif
March 4, 1840
SE1843Dec21T.gif
December 21, 1843
SE1847Oct09A.gif
October 9, 1847
SE1851Jul28T.png
July 28, 1851
SE1855May16P.gif
May 16, 1855
147149151153
SE1859Mar04P.gif
March 4, 1859
SE1862Dec21P.gif
December 21, 1862
SE1866Oct08P.gif
October 8, 1866
SE1870Jul28Pb.gif
July 28, 1870

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 1982
SE1807Nov29H.gif
November 29, 1807
(Saros 139)
SE1818Oct29T.gif
October 29, 1818
(Saros 140)
SE1829Sep28A.gif
September 28, 1829
(Saros 141)
SE1840Aug27T.gif
August 27, 1840
(Saros 142)
SE1851Jul28T.png
July 28, 1851
(Saros 143)
SE1862Jun27P.gif
June 27, 1862
(Saros 144)
SE1873May26P.gif
May 26, 1873
(Saros 145)
SE1884Apr25P.gif
April 25, 1884
(Saros 146)
SE1895Mar26P.gif
March 26, 1895
(Saros 147)
SE1906Feb23P.png
February 23, 1906
(Saros 148)
SE1917Jan23P.png
January 23, 1917
(Saros 149)
SE1927Dec24P.png
December 24, 1927
(Saros 150)
SE1938Nov21P.png
November 21, 1938
(Saros 151)
SE1949Oct21P.png
October 21, 1949
(Saros 152)
SE1960Sep20P.png
September 20, 1960
(Saros 153)
SE1971Aug20P.png
August 20, 1971
(Saros 154)
SE1982Jul20P.png
July 20, 1982
(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
SE1822Aug16T.gif
August 16, 1822
(Saros 142)
SE1851Jul28T.png
July 28, 1851
(Saros 143)
SE1880Jul07A.gif
July 7, 1880
(Saros 144)
SE1909Jun17H.png
June 17, 1909
(Saros 145)
SE1938May29T.png
May 29, 1938
(Saros 146)
SE1967May09P.png
May 9, 1967
(Saros 147)
SE1996Apr17P.png
April 17, 1996
(Saros 148)
SE2025Mar29P.png
March 29, 2025
(Saros 149)
SE2054Mar09P.png
March 9, 2054
(Saros 150)
SE2083Feb16P.png
February 16, 2083
(Saros 151)
Saros152 18van70 SE2112Jan29T.jpg
January 29, 2112
(Saros 152)
SE2141Jan08A.png
January 8, 2141
(Saros 153)
Saros154 15van71 SE2169Dec18A.jpg
December 18, 2169
(Saros 154)
SE2198Nov28T.png
November 28, 2198
(Saros 155)

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References

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