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Total eclipse From Wikipedia, the free encyclopedia
A total solar eclipse occurred at the Moon's ascending node of orbit between Tuesday, November 13 and Wednesday, November 14, 2012,[1][2][3] with a magnitude of 1.05. 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 12 hours before perigee (on November 14, 2012, at 10:20 UTC), the Moon's apparent diameter was larger.[4]
| Solar eclipse of November 13, 2012 | |
|---|---|
Totality as seen from Mount Carbine, Queensland | |
 Map | |
| Type of eclipse | |
| Nature | Total |
| Gamma | −0.3719 |
| Magnitude | 1.05 |
| Maximum eclipse | |
| Duration | 242 s (4 min 2 s) |
| Coordinates | 40°S 161.3°W |
| Max. width of band | 179 km (111 mi) |
| Times (UTC) | |
| (P1) Partial begin | 19:37:58 |
| (U1) Total begin | 20:35:08 |
| Greatest eclipse | 22:12:55 |
| (U4) Total end | 23:48:24 |
| (P4) Partial end | 0:45:34 |
| References | |
| Saros | 133 (45 of 72) |
| Catalog # (SE5000) | 9536 |
Because it crossed the International Date Line it began in local time on November 14 west of the date line over northern Australia, and ended in local time on November 13 east of the date line near the west coast of South America. Totality was visible from parts of Northern Australia. A partial eclipse was visible for parts of Australia, New Zealand, Oceania, West Antarctica, the Antarctic Peninsula, and southern South America.
For this eclipse, totality was visible from northern Australia to about 470 km north of the Chilean Juan Fernández Islands in the southern Pacific Ocean where totality ended. The most populous city to experience totality was Cairns, which had around 2 minutes of totality an hour after daybreak (06:39 AEST, 20:39 UTC) with the sun at an altitude of 14°.[5] Norfolk Island, a small Pacific island east of Australia, experienced a partial eclipse with a maximum eclipse of 98% of the sun obscured at 08:37 NFT and an altitude of 42°.
New Zealand experienced a partial eclipse. Auckland had 84.8% of the sun obscured, whereas Wellington, Christchurch and Dunedin respectively had 71.2%, 61.9% and 52.9% of the sun obscured. Maximum eclipse over New Zealand occurred around 10:30 NZDT (21:30 UTC), with Auckland at 10:27, Wellington at 10:34, Christchurch at 10:35 and Dunedin at 10:36.[6][7]
Most of Chile and parts of Argentina saw a partial eclipse at sunset. In some places over half the sun was obscured. In Chile, Talcahuano in Biobío saw 72% obscured, Castro in Los Lagos saw 56% obscured. Chilean coastal locations were ideally situated to observe an eclipsing sunset over the Pacific Ocean. Points further north, up to about Chañaral, saw the eclipse begin as the sun was setting.
West of the International Date Line the eclipse took place on the morning of November 14. The maximum eclipse totality, of duration 4 min 2 sec, occurred east of the International Date Line on November 13, approximately 2,000 km east of New Zealand, and 9,600 km west of Chile.
On the morning of November 14, skies in Auckland were cloudy, obscuring much of the eclipse, which peaked at 10:27 NZDT.[8] Cloud also obscured the moment of totality at Cairns, disappointing many tourists that had flocked to the area. Eclipse chasers along the northern beaches up through to Port Douglas generally got a clear view, however.
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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.[9]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 2012 November 13 at 19:39:04.9 UTC |
| First Umbral External Contact | 2012 November 13 at 20:36:15.3 UTC |
| First Central Line | 2012 November 13 at 20:37:12.9 UTC |
| First Umbral Internal Contact | 2012 November 13 at 20:38:10.6 UTC |
| First Penumbral Internal Contact | 2012 November 13 at 21:44:49.3 UTC |
| Ecliptic Conjunction | 2012 November 13 at 22:09:06.9 UTC |
| Greatest Eclipse | 2012 November 13 at 22:12:55.2 UTC |
| Greatest Duration | 2012 November 13 at 22:15:06.9 UTC |
| Equatorial Conjunction | 2012 November 13 at 22:19:11.7 UTC |
| Last Penumbral Internal Contact | 2012 November 13 at 22:40:51.6 UTC |
| Last Umbral Internal Contact | 2012 November 13 at 23:47:34.6 UTC |
| Last Central Line | 2012 November 13 at 23:48:32.9 UTC |
| Last Umbral External Contact | 2012 November 13 at 23:49:31.1 UTC |
| Last Penumbral External Contact | 2012 November 14 at 00:46:41.3 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.05004 |
| Eclipse Obscuration | 1.10259 |
| Gamma | −0.37189 |
| Sun Right Ascension | 15h18m06.7s |
| Sun Declination | -18°15'02.6" |
| Sun Semi-Diameter | 16'09.9" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 15h17m51.2s |
| Moon Declination | -18°37'29.5" |
| Moon Semi-Diameter | 16'42.4" |
| Moon Equatorial Horizontal Parallax | 1°01'19.0" |
| ΔT | 66.8 s |
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.
| November 13 Ascending node (new moon) | November 28 Descending node (full moon) |
|---|---|
|  |
| Total solar eclipse Solar Saros 133 | Penumbral lunar eclipse Lunar Saros 145 |
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 eclipses on January 4, 2011 and July 1, 2011 occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 2011 to 2014 | ||||||
|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
118.jpg) Partial in Tromsø, Norway |
June 1, 2011 Partial |
1.21300 | 123 Hinode XRT footage |
November 25, 2011 Partial |
−1.05359 | |
128 Annularity in Red Bluff, CA, USA |
May 20, 2012 Annular |
0.48279 | 133 Totality in Mount Carbine, Queensland, Australia |
November 13, 2012 Total |
−0.37189 | |
138 Annularity in Churchills Head, Australia |
May 10, 2013 Annular |
−0.26937 | 143 Partial in Libreville, Gabon |
November 3, 2013 Hybrid |
0.32715 | |
148.jpg) Partial in Adelaide, Australia |
April 29, 2014 Annular (non-central) |
−0.99996 | 153 Partial in Minneapolis, MN, USA |
October 23, 2014 Partial |
1.09078 | |
This eclipse is a part of Saros series 133, repeating every 18 years, 11 days, and containing 72 events. The series started with a partial solar eclipse on July 13, 1219. It contains annular eclipses from November 20, 1435 through January 13, 1526; a hybrid eclipse on January 24, 1544; and total eclipses from February 3, 1562 through June 21, 2373. The series ends at member 72 as a partial eclipse on September 5, 2499. 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 25 at 1 minutes, 14 seconds on November 30, 1453, and the longest duration of totality was produced by member 61 at 6 minutes, 50 seconds on August 7, 1850. All eclipses in this series occur at the Moon’s ascending node of orbit.[11]
| Series members 34–55 occur between 1801 and 2200: | ||
|---|---|---|
| 34 | 35 | 36 |
 July 17, 1814 |
 July 27, 1832 |
 August 7, 1850 |
| 37 | 38 | 39 |
 August 18, 1868 |
 August 29, 1886 |
 September 9, 1904 |
| 40 | 41 | 42 |
 September 21, 1922 |
 October 1, 1940 |
 October 12, 1958 |
| 43 | 44 | 45 |
 October 23, 1976 |
 November 3, 1994 |
November 13, 2012 |
| 46 | 47 | 48 |
 November 25, 2030 |
 December 5, 2048 |
 December 17, 2066 |
| 49 | 50 | 51 |
 December 27, 2084 |
 January 8, 2103 |
 January 19, 2121 |
| 52 | 53 | 54 |
 January 30, 2139 |
 February 9, 2157 |
 February 21, 2175 |
| 55 | ||
 March 3, 2193 | ||
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.
| 21 eclipse events between June 21, 1982 and June 21, 2058 | ||||
|---|---|---|---|---|
| June 21 | April 8–9 | January 26 | November 13–14 | September 1–2 |
| 117 | 119 | 121 | 123 | 125 |
 June 21, 1982 |
 April 9, 1986 |
 January 26, 1990 |
 November 13, 1993 |
 September 2, 1997 |
| 127 | 129 | 131 | 133 | 135 |
 June 21, 2001 |
 April 8, 2005 |
 January 26, 2009 |
November 13, 2012 |
 September 1, 2016 |
| 137 | 139 | 141 | 143 | 145 |
 June 21, 2020 |
 April 8, 2024 |
 January 26, 2028 |
 November 14, 2031 |
 September 2, 2035 |
| 147 | 149 | 151 | 153 | 155 |
 June 21, 2039 |
 April 9, 2043 |
 January 26, 2047 |
 November 14, 2050 |
 September 2, 2054 |
| 157 | ||||
 June 21, 2058 | ||||
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 | ||||
|---|---|---|---|---|
 June 26, 1805 (Saros 114) |
 May 27, 1816 (Saros 115) |
 April 26, 1827 (Saros 116) |
 March 25, 1838 (Saros 117) |
 February 23, 1849 (Saros 118) |
 January 23, 1860 (Saros 119) |
 December 22, 1870 (Saros 120) |
 November 21, 1881 (Saros 121) |
 October 20, 1892 (Saros 122) |
 September 21, 1903 (Saros 123) |
 August 21, 1914 (Saros 124) |
 July 20, 1925 (Saros 125) |
 June 19, 1936 (Saros 126) |
 May 20, 1947 (Saros 127) |
 April 19, 1958 (Saros 128) |
 March 18, 1969 (Saros 129) |
 February 16, 1980 (Saros 130) |
 January 15, 1991 (Saros 131) |
 December 14, 2001 (Saros 132) |
November 13, 2012 (Saros 133) |
 October 14, 2023 (Saros 134) |
 September 12, 2034 (Saros 135) |
 August 12, 2045 (Saros 136) |
 July 12, 2056 (Saros 137) |
 June 11, 2067 (Saros 138) |
 May 11, 2078 (Saros 139) |
 April 10, 2089 (Saros 140) |
 March 10, 2100 (Saros 141) |
 February 8, 2111 (Saros 142) |
 January 8, 2122 (Saros 143) |
 December 7, 2132 (Saros 144) |
 November 7, 2143 (Saros 145) |
 October 7, 2154 (Saros 146) |
 September 5, 2165 (Saros 147) |
 August 4, 2176 (Saros 148) |
 July 6, 2187 (Saros 149) |
 June 4, 2198 (Saros 150) | |||
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 | ||
|---|---|---|
 April 4, 1810 (Saros 126) |
 March 15, 1839 (Saros 127) |
 February 23, 1868 (Saros 128) |
 February 1, 1897 (Saros 129) |
 January 14, 1926 (Saros 130) |
 December 25, 1954 (Saros 131) |
 December 4, 1983 (Saros 132) |
November 13, 2012 (Saros 133) |
 October 25, 2041 (Saros 134) |
 October 4, 2070 (Saros 135) |
 September 14, 2099 (Saros 136) |
 August 25, 2128 (Saros 137) |
 August 5, 2157 (Saros 138) |
 July 16, 2186 (Saros 139) |
|
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