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20th-century annular solar eclipse From Wikipedia, the free encyclopedia
An annular solar eclipse occurred at the Moon's descending node of orbit on Thursday, September 11, 1969,[1] with a magnitude of 0.969. 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. Occurring about 5.2 days after apogee (on September 6, 1969, at 15:50 UTC), the Moon's apparent diameter was smaller.[2]
Annularity was visible from the Pacific Ocean, Peru, Bolivia and the southwestern tip of Brazilian state Mato Grosso. A partial eclipse was visible for parts of North America, Central America, the Caribbean, and western South America. Places west of the International Date Line witnessed the eclipse on Friday, September 12, 1969.
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.[3]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1969 September 11 at 17:02:10.6 UTC |
| First Umbral External Contact | 1969 September 11 at 18:05:48.3 UTC |
| First Central Line | 1969 September 11 at 18:07:22.6 UTC |
| First Umbral Internal Contact | 1969 September 11 at 18:08:57.1 UTC |
| Greatest Duration | 1969 September 11 at 18:58:29.1 UTC |
| First Penumbral Internal Contact | 1969 September 11 at 19:15:35.4 UTC |
| Equatorial Conjunction | 1969 September 11 at 19:45:07.4 UTC |
| Ecliptic Conjunction | 1969 September 11 at 19:56:27.0 UTC |
| Greatest Eclipse | 1969 September 11 at 19:58:58.7 UTC |
| Last Penumbral Internal Contact | 1969 September 11 at 20:42:42.5 UTC |
| Last Umbral Internal Contact | 1969 September 11 at 21:49:10.9 UTC |
| Last Central Line | 1969 September 11 at 21:50:42.6 UTC |
| Last Umbral External Contact | 1969 September 11 at 21:52:14.2 UTC |
| Last Penumbral External Contact | 1969 September 11 at 22:55:46.4 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.96904 |
| Eclipse Obscuration | 0.93904 |
| Gamma | 0.22014 |
| Sun Right Ascension | 11h19m09.2s |
| Sun Declination | +04°23'48.2" |
| Sun Semi-Diameter | 15'53.5" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 11h19m32.8s |
| Moon Declination | +04°34'30.9" |
| Moon Semi-Diameter | 15'10.1" |
| Moon Equatorial Horizontal Parallax | 0°55'40.1" |
| ΔT | 39.9 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. The first and last eclipse in this sequence is separated by one synodic month.
| August 27 Ascending node (full moon) | September 11 Descending node (new moon) | September 25 Ascending node (full moon) |
|---|---|---|
 | |  |
| Penumbral lunar eclipse Lunar Saros 108 | Annular solar eclipse Solar Saros 134 | Penumbral lunar eclipse Lunar Saros 146 |
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.[4]
The partial solar eclipse on July 22, 1971 occurs in the next lunar year eclipse set.
| Solar eclipse series sets from 1968 to 1971 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 119 | March 28, 1968 Partial |
−1.037 | 124 | September 22, 1968 Total |
0.9451 | |
| 129 | March 18, 1969 Annular |
−0.2704 | 134 | September 11, 1969 Annular |
0.2201 | |
139.jpg) Totality in Williamston, NC USA |
March 7, 1970 Total |
0.4473 | 144 | August 31, 1970 Annular |
−0.5364 | |
| 149 | February 25, 1971 Partial |
1.1188 | 154 | August 20, 1971 Partial |
−1.2659 | |
This eclipse is a part of Saros series 134, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on June 22, 1248. It contains total eclipses from October 9, 1428 through December 24, 1554; hybrid eclipses from January 3, 1573 through June 27, 1843; and annular eclipses from July 8, 1861 through May 21, 2384. The series ends at member 72 as a partial eclipse on August 6, 2510. 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 1 minutes, 30 seconds on October 9, 1428, and the longest duration of annularity will be produced by member 52 at 10 minutes, 55 seconds on January 10, 2168. All eclipses in this series occur at the Moon’s descending node of orbit.[5]
| Series members 32–53 occur between 1801 and 2200: | ||
|---|---|---|
| 32 | 33 | 34 |
 June 6, 1807 |
 June 16, 1825 |
 June 27, 1843 |
| 35 | 36 | 37 |
 July 8, 1861 |
 July 19, 1879 |
 July 29, 1897 |
| 38 | 39 | 40 |
 August 10, 1915 |
 August 21, 1933 |
 September 1, 1951 |
| 41 | 42 | 43 |
September 11, 1969 |
 September 23, 1987 |
 October 3, 2005 |
| 44 | 45 | 46 |
 October 14, 2023 |
 October 25, 2041 |
 November 5, 2059 |
| 47 | 48 | 49 |
 November 15, 2077 |
 November 27, 2095 |
 December 8, 2113 |
| 50 | 51 | 52 |
 December 19, 2131 |
 December 30, 2149 |
 January 10, 2168 |
| 53 | ||
 January 20, 2186 | ||
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 September 12, 1931 and July 1, 2011 | ||||
|---|---|---|---|---|
| September 11–12 | June 30–July 1 | April 17–19 | February 4–5 | November 22–23 |
| 114 | 116 | 118 | 120 | 122 |
 September 12, 1931 |
 June 30, 1935 |
 April 19, 1939 |
 February 4, 1943 |
 November 23, 1946 |
| 124 | 126 | 128 | 130 | 132 |
 September 12, 1950 |
 June 30, 1954 |
 April 19, 1958 |
 February 5, 1962 |
 November 23, 1965 |
| 134 | 136 | 138 | 140 | 142 |
September 11, 1969 |
 June 30, 1973 |
 April 18, 1977 |
 February 4, 1981 |
 November 22, 1984 |
| 144 | 146 | 148 | 150 | 152 |
 September 11, 1988 |
 June 30, 1992 |
 April 17, 1996 |
 February 5, 2000 |
 November 23, 2003 |
| 154 | 156 | |||
 September 11, 2007 |
 July 1, 2011 | |||
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 | ||||
|---|---|---|---|---|
 December 21, 1805 (Saros 119) |
 November 19, 1816 (Saros 120) |
 October 20, 1827 (Saros 121) |
 September 18, 1838 (Saros 122) |
 August 18, 1849 (Saros 123) |
 July 18, 1860 (Saros 124) |
 June 18, 1871 (Saros 125) |
 May 17, 1882 (Saros 126) |
 April 16, 1893 (Saros 127) |
 March 17, 1904 (Saros 128) |
 February 14, 1915 (Saros 129) |
 January 14, 1926 (Saros 130) |
 December 13, 1936 (Saros 131) |
 November 12, 1947 (Saros 132) |
 October 12, 1958 (Saros 133) |
September 11, 1969 (Saros 134) |
 August 10, 1980 (Saros 135) |
 July 11, 1991 (Saros 136) |
 June 10, 2002 (Saros 137) |
 May 10, 2013 (Saros 138) |
 April 8, 2024 (Saros 139) |
 March 9, 2035 (Saros 140) |
 February 5, 2046 (Saros 141) |
 January 5, 2057 (Saros 142) |
 December 6, 2067 (Saros 143) |
 November 4, 2078 (Saros 144) |
 October 4, 2089 (Saros 145) |
 September 4, 2100 (Saros 146) |
 August 4, 2111 (Saros 147) |
 July 4, 2122 (Saros 148) |
 June 3, 2133 (Saros 149) |
 May 3, 2144 (Saros 150) |
 April 2, 2155 (Saros 151) |
 March 2, 2166 (Saros 152) |
 January 29, 2177 (Saros 153) |
 December 29, 2187 (Saros 154) |
 November 28, 2198 (Saros 155) | |||
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 | ||
|---|---|---|
 December 20, 1824 (Saros 129) |
 November 30, 1853 (Saros 130) |
 November 10, 1882 (Saros 131) |
 October 22, 1911 (Saros 132) |
 October 1, 1940 (Saros 133) |
September 11, 1969 (Saros 134) |
 August 22, 1998 (Saros 135) |
 August 2, 2027 (Saros 136) |
 July 12, 2056 (Saros 137) |
 June 22, 2085 (Saros 138) |
 June 3, 2114 (Saros 139) |
 May 14, 2143 (Saros 140) |
 April 23, 2172 (Saros 141) |
||
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