The Saros cycle is an eclipse cycle with a period of 223 synodic months (approximately 6585.3213 days, or nearly 18 years 11 1/3 days), that can be used to predict eclipses of the Sun and Moon. One cycle after an eclipse, the Sun, Earth, and Moon return to approximately the same relative geometry, and a nearly identical eclipse will occur. A series of eclipses that are separated by one Saros cycle is called a Saros series. Contents 1 History 2 Description 3 Saros series 3.1 Example: Lunar Saros 131 4 See also 5 References 6 External links History The earliest discovered historical record of the Saros cycle is by the Chaldeans (ancient Babylonian astronomers) in the last several centuries BC,123 and was later known to Hipparchus, Pliny4 and Ptolemy,5 but under different names. The Sumerian/Babylonian word "šár" was one of the ancient Mesopotamian units of measurement and as a number appears to have had a value of 3600.6 The name "saros" (Greek: σάρος) was first given to the eclipse cycle by Edmond Halley in 1691, who took it from the Suda, a Byzantine lexicon of the 11th century.7 The information in the Suda in turn was derived directly or otherwise from the Chronicle of Eusebius of Caesarea, which quoted Berossus. Although Halley's naming error was pointed out by Guillaume Le Gentil in 1756, the name continues to be used. Description The Saros cycle of 6585.322 days (14 normal years + 4 leap years + 11.322 days, or 13 normal years + 5 leap years + 10.322 days) is useful for predicting the times at which nearly identical eclipses will occur, and derives from three periodicities of the lunar orbit: the synodic month, the draconic month, and the anomalistic month. For an eclipse to occur, either the Moon must be located between the Earth and Sun (for a solar eclipse) or the Earth must be located between the Sun and Moon (for a lunar eclipse). This can happen only when the Moon is new or full, respectively, and repeat occurrences of these lunar phases are controlled by the Moon's synodic period, which is about 29.53 days. Most of the times during a full and new moon, however, the shadow of the Earth or Moon falls to the north or south of the other body. Thus, if an eclipse is to occur, the three bodies must also be nearly in a straight line. This condition occurs only when the Moon passes close to the ecliptic plane which is the case around the time when it passes through one of the two nodes of its orbit (the ascending or descending node). The period of time for two successive passes through the ecliptic plane at the same node is given by the draconic month, which is 27.21 days. So the conditions of an eclipse are met at a new or full moon around one of the nodes, which occurs every 5 or 6 months (the Sun, being in conjunction or opposition to the Moon, is also at a node of the Moon's orbit at that time - this happens twice in an eclipse year). However, if two eclipses are to have the same appearance and duration, then also the distance between the Earth and Moon must be the same for both events. The time it takes the Moon to orbit the Earth once and return to the same distance is given by the anomalistic month, which has a period of 27.55 days.

The origin of the Saros cycle comes from the recognition that 223 synodic months is approximately equal to 242 draconic months, which is approximately equal to 239 anomalistic months (this approximation is good to within about 2 hours). After one Saros cycle, the Moon will have completed roughly an integer number of synodic, draconic, and anomalistic months, and the Earth-Sun-Moon geometry will be nearly identical: the Moon will have the same phase, be at the same node, and have the same distance from the Earth. If one knew the date of an eclipse, then one Saros later, a nearly identical eclipse should occur. Mind that during that 18 year cycle, about 40 other solar and lunar eclipses take place, but with a somewhat different geometry. Note also that the Saros cycle (18.031 years) is not equal to an integer number of revolutions of the Moon with respect to the fixed stars (sidereal month of 27.32 days). Therefore, even though the relative geometry of the Earth-Sun-Moon system will be nearly identical after a Saros, the Moon will be in a different position with respect to the stars. This is due to the fact that the orbit of the Moon precesses. A complication with the Saros cycle is that its period is not an integer number of days, but contains a multiple of ⅓ of a day. Thus, as a result of the Earth's rotation, for each successive Saros cycle, an eclipse will occur about 8 hours later in the day. In the case of an eclipse of the Sun, this means that the region of visibility will shift westward by 120°, or one third of the way around the globe, and the two eclipses will thus not be visible from the same place on Earth. In the case of an eclipse of the Moon, the next eclipse might still be visible from the same location as long as the Moon is above the horizon. However, if one waits three Saros cycles, the local time of day of an eclipse will be nearly the same. This period of three Saros cycles (54 years 1 month, or almost 19756 full days), is known as a Triple Saros or exeligmos (Greek: "turn of the wheel"). Saros series Lunar eclipses occurring near the Moon's descending node are given odd Saros series numbers. The first eclipse in such series passes through the southern edge of the Earth's shadow, and the Moon's path is shifted northward each successive Saros cycle.

The Saros cycle is based on the recognition that 223 synodic months approximately equal to 242 draconic months and 239 anomalistic months. However, as this relationship is not perfect, the geometry of two eclipses separated by one Saros cycle will differ slightly. In particular, the place where the Sun and Moon come in conjunction shifts westward by about 0.5° with respect to the Moon's nodes every Saros cycle, and this gives rise to a series of eclipses, called a Saros series, that slowly change in appearance. Each Saros series starts with a partial eclipse, and each successive Saros cycle the path of the Moon is shifted either northward (when near the descending node) or southward (when near the ascending node). At some point, eclipses are no longer possible and the series terminates. Arbitrary dates were established by compilers of eclipse statistics. These extreme dates are 2000 BCE and 3000 CE. Saros series, of course, went on before and will continue after these dates. Since the first eclipse of 2000 BCE was not the first in its saros, it is necessary to extend the saros series numbers backwards beyond 0 to negative numbers to accommodate eclipses occurring in the years following 2000 BCE. The saros -13 is the first saros to appear in these data. For solar eclipses the statistics for the complete Saros series within the era between 2000 BCE and 3000 CE are given in this article's references.89 It takes between 1226 and 1550 years for the members of a saros series to traverse the Earth's surface from north to south (or vice-versa). These extremes allow from 69 to 87 eclipses in each series (most series have 71 or 72 eclipses). From 39 to 59 (mostly about 43) eclipses in a given series will be central (that is, total, annular, or hybrid annular-total). Solar eclipse series are not as long-lived.citation needed At any given time, approximately 40 different Saros series will be in progress. Saros series are numbered according to the type of eclipse (solar or lunar) and whether they occur at the Moon's ascending or descending node.1011 Odd numbers are used for solar eclipses occurring near the ascending node, whereas even numbers are given to descending node solar eclipses. For lunar eclipses, this numbering scheme is reversed. The ordering of these series is determined by the time at which each series peaks, which corresponds to when an eclipse is closest to one of the lunar nodes. For solar eclipses, (in 2003) the 39 series numbered between 117 and 155 are active, whereas for lunar eclipses, there are now 41 active Saros series. Example: Lunar Saros 131 Saros 131 lunar eclipse dates May 10, 1427 (Julian calendar) First penumbral (southern edge of shadow) ...6 intervening penumbral eclipses omitted... July 25, 1553 (Julian calendar) First partial ...19 intervening partial eclipses omitted... March 22, 1932 Final partial 12:32 UT April 2, 1950 First total 20:44 UT April 13, 1968 04:47 UT April 24, 1986 12:43 UT May 4, 2004 20:30 UT May 16, 2022 First central 04:11 UT May 26, 2040 11:45 UT June 6, 2058 19:14 UT June 17, 2076 Central 02:37 UT June 28, 2094 09:59 UT July 8, 2112 17:16 UT July 21, 2130 00:34 UT July 31, 2148 07:51 UT August 11, 2166 15:11 UT August 21, 2184 22:32 UT September 3, 2202 Last total 05:59 UT September 13, 2220 First partial ...18 intervening partial eclipses omitted... April 9, 2563 Last partial umbral ...7 intervening penumbral eclipses omitted... July 7, 2707 Last penumbral (northern edge of shadow)

As an example of a single Saros series, the accompanying table gives the dates of some of the 72 lunar eclipses for Saros series 131. This eclipse series began in AD 1427 with a partial eclipse at the southern edge of the Earth's shadow when the Moon was close to its descending node. Each successive Saros cycle, the Moon's orbital path is shifted northward with respect to the Earth's shadow, with the first total eclipse occurring in 1950. For the following 252 years, total eclipses occur, with the central eclipse being predicted to occur in 2078. The first partial eclipse after this is predicted to occur in the year 2220, and the final partial eclipse of the series will occur in 2707. The total lifetime of the lunar Saros series 131 is 1280 years. Because of the ⅓ fraction of days in a Saros cycle, the visibility of each eclipse will differ for an observer at a given locale. For the lunar Saros series 131, the first total eclipse of 1950 had its best visibility for viewers in Eastern Europe and the Middle East because mid-eclipse was at 20:44 UT. The following eclipse in the series occurred approximately 8 hours later in the day with mid-eclipse at 4:47 UT, and was best seen from North America and South America. The third total eclipse occurred approximately 8 hours later in the day than the second eclipse with mid-eclipse at 12:43 UT, and had its best visibility for viewers in the Western Pacific, East Asia, Australia and New Zealand. This cycle of visibility repeats from the initiation to termination of the series, with minor variations. See also List of Saros series for lunar eclipses Eclipse cycle Solar eclipse Lunar eclipse Metonic cycle References Cited references ^ Tablets 1414, 1415, 1416, 1417, 1419 of: T.G. Pinches, J.N. Strassmaier: Late Babylonian Astronomical and Related Texts. A.J. Sachs (ed.), Brown University Press 1955 ^ A.J. Sachs & H. Hunger (1987..1996): Astronomical Diaries and Related Texts from Babylonia, Vol.I..III. Österreichischen Akademie der Wissenschaften. ibid. H. Hunger (2001) Vol. V: Lunar and Planetary Texts ^ P.J. Huber & S de Meis (2004): Babylonian Eclipse Observations from 750 BC to 1 BC, par. 1.1. IsIAO/Mimesis, Milano ^ Naturalis Historia II.10[56] ^ Almagest IV.2 ^ Microsoft Encarta College Dictionary, 2001 ^ The Suda entry is online here. ^ Meeus, Jean (2004). Ch. 18 "About Saros and Inex series" in: Mathematical Astronomy Morsels III. Willmann-Bell, Richmond VA, USA.  ^ Espenak, Fred; Jean Meeus (October 2006). "Five Millennium Canon of Solar Eclipses, Section 4 (NASA TP-2006-214141)" (PDF). NASA STI Program Office. http://sunearth.gsfc.nasa.gov/eclipse/5MCSE/5MCSE-Text.pdf. Retrieved 2007-01-24.  ^ G. van den Bergh (1955). Periodicity and Variation of Solar (and Lunar) Eclipses (2 vols.). H.D. Tjeenk Willink & Zoon N.V., Haarlem.  ^ Bao-Lin Liu and Alan D. Fiala (1992). Canon of Lunar Eclipses, 1500 B.C. to A.D. 3000. Willmann-Bell, Richmond VA. 

General references Jean Meeus and Hermann Mucke (1983) Canon of Lunar Eclipses. Astronomisches Büro, Vienna Theodor von Oppolzer (1887). Canon der Finsternisse. Vienna Mathematical Astronomy Morsels, Jean Meeus, Willmann-Bell, Inc., 1997 (Chapter 9, p. 51, Table 9.A Some eclipse Periodicities) External links NASA - Eclipses and the Saros NASA - Catalog of Lunar Eclipses in Saros 0 NASA - Lunar Eclipses of Saros Series 1 to 180 NASA - Solar Eclipses of Saros Series 0 to 180 NASA - Summary of Lunar Eclipses in Saros Series -20 to 183 NASA - Summary of Solar Eclipses in Saros Series -13 to 190 Search among the 11,898 solar eclipses over five millennium and display interactive maps Search among the 12,064 lunar eclipses over five millennium and display interactive maps Eclipses and the Saros Cycle Eclipse Search -- here one can search 5,000 years of eclipse data by type, magnitude, Saros number or simply by year. Saros series 131 table v · d · eSolar eclipses Lists of eclipses Antiquity · 20th century BC • 19th century BC • 18th century BC • 17th century BC • 16th century BC • 15th century BC • 14th century BC • 13th century BC • 12th century BC • 11th century BC • 10th century BC • 9th century BC • 8th century BC • 7th century BC • 6th century BC • 5th century BC • 4th century BC • 3rd century BC • 2nd century BC • 1st century BC • 1st century · 2nd century · 3rd century · 4th century · 5th century · 6th century · 7th century · 8th century · 9th century · 10th century · 11th century · 12th century · 13th century · 14th century · 15th century · 16th century · 17th century · 18th century · 19th century · 20th century · 21st century · 22nd century · 23rd century · 24th century · 25th century · 26th century · 27th century · 28th century · 29th century · 30th century Eclipses seen from: China · the United Kingdom · Philippines Saros cycles: 110 · 111 · 112 · 113 · 114 · 115 · 116 · 117 · 118 · 119 · 120 · 121 · 122 · 123 · 124 · 125 · 126 · 127 · 128 · 129 · 130 · 131 · 132 · 133 · 134 · 135 · 136 · 137 · 138 · 139 · 140 · 141 · 142 · 143 · 144 · 145 · 146 · 147 · 148 · 149 · 150 · 151 · 152 · 153 · 154 · 155 · 156 · 157 · 158 · 159 · 160 · 161 · 162

Historical eclipses Mursili's eclipse (1312 BC) · Assyrian eclipse (763 BC) · Battle of Halys (585 BC) · Crucifixion darkness and eclipse Past Total/hybrid eclipses 1560 Aug 21 · 1598 Mar 7 · 1652 Apr 8 · 1654 Aug 12 · 1699 Sep 23 · 1715 May 3 · 1724 May 22 · 1766 Feb 9 · 1778 Jun 24 · 1780 Oct 27 · 1806 Jun 16 · 1816 Nov 19 · 1820 Sep 7 · 1824 Jun 26 · 1842 Jul 8 · 1851 Jul 28 · 1853 Nov 30 · 1857 Mar 25 · 1858 Sep 7 · 1860 Jul 18  · 1865 Apr 25 · 1867 Aug 29 · 1868 Aug 18 · 1869 Aug 7 · 1870 Dec 22 · 1871 Dec 12 · 1874 Apr 16 · 1875 Apr 6 · 1878 Jul 29 · 1882 May 17  · 1883 May 6  · 1885 Sep 8  · 1886 Aug 29  · 1887 Aug 19  · 1889 Jan 1 · 1889 Dec 22  · 1893 Apr 16  · 1896 Aug 9  · 1898 Jan 22  · 1900 May 28 · 1901 May 18 · 1903 Sep 21 · 1904 Sep 9 · 1905 Aug 30 · 1907 Jan 14 · 1908 Jan 3 · 1908 Dec 23 · 1909 Jun 17 · 1910 May 9 · 1911 Apr 28 · 1912 Apr 17 · 1912 Oct 10 · 1914 Aug 21 · 1916 Feb 3 · 1918 Jun 8 · 1919 May 29 · 1921 Oct 1 · 1922 Sep 21 · 1923 Sep 10 · 1925 Jan 24 · 1926 Jan 14 · 1927 Jun 29 · 1928 May 19 · 1929 May 9 · 1930 Apr 28 · 1930 Oct 21 · 1932 Aug 31 · 1934 Feb 14 · 1936 Jun 19 · 1937 Jun 8 · 1938 May 29 · 1939 Oct 12 · 1940 Oct 1 · 1941 Sep 21 · 1943 Feb 4 · 1944 Jan 25 · 1944 Jul 20 · 1945 Jul 9 · 1947 May 20 · 1948 Nov 1 · 1950 Sep 12 · 1952 Feb 25 · 1954 Jun 30 · 1955 Jun 20 · 1956 Jun 8 · 1957 Oct 23 · 1958 Oct 12 · 1959 Oct 2 · 1961 Feb 15 · 1962 Feb 5 · 1963 Jul 20 · 1965 May 30 · 1966 Nov 12 · 1967 Nov 2 · 1968 Sep 22 · 1970 Mar 7 · 1972 Jul 10 · 1973 Jun 30 · 1974 Jun 20 · 1976 Oct 23 · 1977 Oct 12 · 1979 Feb 26 · 1980 Feb 16 · 1981 Jul 31 · 1983 Jun 11 · 1984 Nov 22 · 1985 Nov 12 · 1986 Oct 3 · 1987 Mar 29 · 1988 Mar 18 · 1990 Jul 22 · 1991 Jul 11 · 1992 Jun 30 · 1994 Nov 3 · 1995 Oct 24 · 1997 Mar 9 · 1998 Feb 26 · 1999 Aug 11 · 2001 Jun 21 · 2002 Dec 4 · 2003 Nov 23 · 2005 Apr 8 · 2006 Mar 29 · 2008 Aug 1 · 2009 Jul 22 · 2010 Jul 11 Future Total/hybrid eclipses

2012 Nov 13 · 2013 Nov 3 · 2015 Mar 20 · 2016 Mar 9 · 2017 Aug 21 · 2019 Jul 2 · 2020 Dec 14 · 2021 Dec 4 · 2023 Apr 20 · 2024 Apr 8 · 2026 Aug 12 · 2027 Aug 2 · 2028 Jul 22 · 2030 Nov 25 · 2031 Nov 14 · 2033 Mar 30 · 2034 Mar 20 · 2035 Sep 2 · 2037 Jul 13 · 2038 Dec 26 · 2039 Dec 15 · 2041 Apr 30 · 2042 Apr 20 · 2043 Apr 9 · 2044 Aug 23 · 2045 Aug 12 · 2046 Aug 2 · 2048 Dec 5 · 2049 Nov 25 · 2050 May 20 · 2052 Mar 30 · 2053 Sep 12 · 2055 Jul 24 · 2057 Jan 5 · 2057 Dec 26 · 2059 May 11 · 2060 Apr 30 · 2061 Apr 20 · 2063 Aug 24 · 2064 Aug 12 · 2066 Dec 17 · 2067 Dec 6 · 2068 May 31 · 2070 Apr 11 · 2071 Sep 23 · 2072 Sep 12 · 2073 Aug 3 · 2075 Jan 16 · 2076 Jan 6 · 2077 May 22 · 2078 May 11 · 2079 May 1 · 2081 Sep 3 · 2082 Aug 24 · 2084 Dec 27 · 2086 Jun 11 · 2088 Apr 21 · 2089 Oct 4 · 2090 Sep 23 · 2091 Aug 15 · 2093 Jan 27 · 2094 Jan 16 · 2095 Jun 2 · 2096 May 22 · 2097 May 11 · 2099 Sep 14 · 2100 Sep 4 · 2114 Jun 3 · 2132 Jun 13 · 2150 Jun 25 · 2168 Jul 5 · 2186 Jul 16 Past Annular eclipses 1854 May 26 · 1879 Jan 22 · 1889 Jun 28 · 1901 Nov 11 · 1903 Mar 29 · 1904 Mar 17 · 1905 Mar 6 · 1907 Jul 10 · 1908 Jun 28 · 1911 Oct 22 · 1914 Feb 25 · 1915 Feb 14 · 1915 Aug 10 · 1916 Jul 30 · 1917 Dec 14 · 1918 Dec 3 · 1919 Nov 22 · 1921 Apr 8 · 1922 Mar 28 · 1923 Mar 17 · 1925 Jul 20 · 1926 Jul 9 · 1927 Jan 3 · 1929 Nov 1 · 1932 Mar 7 · 1933 Feb 24 · 1933 Aug 21 · 1934 Aug 10 · 1935 Dec 25 · 1936 Dec 13 · 1937 Dec 2 · 1939 Apr 19 · 1940 Apr 7 · 1941 Mar 27 · 1943 Aug 1 · 1945 Jan 14 · 1947 Nov 12 · 1948 May 9 · 1950 Mar 18 · 1951 Mar 7 · 1951 Sep 1 · 1952 Aug 20 · 1954 Jan 5 · 1954 Dec 25 · 1955 Dec 14 · 1957 Apr 30 · 1958 Apr 19 · 1959 Apr 8 · 1961 Aug 11 · 1962 Jul 31 · 1963 Jan 25 · 1965 Nov 23 · 1966 May 20 · 1969 Mar 18 · 1969 Sep 11 · 1970 Aug 31 · 1972 Jan 16 · 1973 Jan 4 · 1973 Dec 24 · 1976 Apr 29 · 1977 Apr 18 · 1979 Aug 22 · 1980 Aug 10 · 1981 Feb 4 · 1983 Dec 4 · 1984 May 30 · 1987 Sep 23 · 1988 Sep 11 · 1990 Jan 26 · 1991 Jan 15 · 1992 Jan 4 · 1994 May 10 · 1995 Apr 29 · 1998 Aug 22 · 1999 Feb 16 · 2001 Dec 14 · 2002 Jun 10 · 2003 May 31 · 2005 Oct 3 · 2006 Sep 22 · 2008 Feb 7 · 2009 Jan 26 · 2010 Jan 15 Future Annular eclipses

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