| Total eclipse | |
 Map | |
| Gamma | 1.0007 |
|---|---|
| Magnitude | 1.0126 |
| Maximum eclipse | |
| Duration | - |
| Coordinates | 62°00′S27°48′W / 62°S 27.8°W /-62; -27.8 |
| Max. width of band | - km |
| Times (UTC) | |
| Greatest eclipse | 5:38:56 |
| References | |
| Saros | 152 (10 of 70) |
| Catalog # (SE5000) | 9437 |
A totalsolar eclipse occurred at the Moon'sdescending node of orbit on Thursday, November 2, 1967,[1] with amagnitude of 1.0126. Asolar eclipse occurs when theMoon passes betweenEarth and theSun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. A total solar eclipse occurs when the Moon'sapparent 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 4 hours afterperigee (on November 2, 1967, at 1:50 UTC), the Moon's apparent diameter was larger.[2]
It will be unusual in that while it is a total solar eclipse, it is not a central solar eclipse. Anon-central eclipse is one where the center-line of totality does not intersect the surface of the Earth (when thegamma is between 0.9972 and 1.0260). Instead, the center line passes just above the Earth's surface. This rare type occurs when totality is only visible at sunset or sunrise in a polar region.
While totality was not visible for any land masses, a partial eclipse was visible forSouthern Africa andAntarctica. This was the first of 55 umbral solar eclipses ofSolar Saros 152.
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 | 1967 November 2 at 03:39:02.7 UTC |
| First Umbral External Contact | 1967 November 2 at 05:26:47.4 UTC |
| Greatest Eclipse | 1967 November 2 at 05:38:56.2 UTC |
| Ecliptic Conjunction | 1967 November 2 at 05:48:56.9 UTC |
| Last Umbral External Contact | 1967 November 2 at 05:50:36.0 UTC |
| Equatorial Conjunction | 1967 November 2 at 06:25:04.9 UTC |
| Last Penumbral External Contact | 1967 November 2 at 07:38:31.3 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.01261 |
| Eclipse Obscuration | - |
| Gamma | −1.00067 |
| Sun Right Ascension | 14h26m52.0s |
| Sun Declination | -14°32'08.6" |
| Sun Semi-Diameter | 16'07.1" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 14h25m07.9s |
| Moon Declination | -15°28'04.1" |
| Moon Semi-Diameter | 16'44.2" |
| Moon Equatorial Horizontal Parallax | 1°01'25.4" |
| ΔT | 38.1 s |
This eclipse is part of aneclipse 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 afortnight.
| October 18 Ascending node (full moon) | November 2 Descending node (new moon) |
|---|---|
 | |
| Total lunar eclipse Lunar Saros 126 | Total solar eclipse Solar Saros 152 |
This eclipse is a member of asemester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternatingnodes of the Moon's orbit.[4]
The partial solar eclipses onJanuary 14, 1964 andJuly 9, 1964 occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 1964 to 1967 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 117 | June 10, 1964 Partial | −1.1393 | 122 | December 4, 1964 Partial | 1.1193 | |
| 127 | May 30, 1965 Total | −0.4225 | 132 | November 23, 1965 Annular | 0.3906 | |
| 137 | May 20, 1966 Annular | 0.3467 | 142 | November 12, 1966 Total | −0.33 | |
| 147 | May 9, 1967 Partial | 1.1422 | 152 | November 2, 1967 Total (non-central) | 1.0007 | |
This eclipse is a part ofSaros series 152, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on July 26, 1805. It contains total eclipses fromNovember 2, 1967 through September 14, 2490; hybrid eclipses from September 26, 2508 through October 17, 2544; and annular eclipses from October 29, 2562 through June 16, 2941. The series ends at member 70 as a partial eclipse on August 20, 3049. Its eclipses are tabulated in three columns; every third eclipse in the same column is oneexeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
The longest duration of totality will be produced by member 30 at 5 minutes, 16 seconds on June 9, 2328, and the longest duration of annularity will be produced by member 53 at 5 minutes, 20 seconds on February 16, 2743. All eclipses in this series occur at the Moon’sdescending node of orbit.[5]
| Series members 1–22 occur between 1805 and 2200: | ||
|---|---|---|
| 1 | 2 | 3 |
 July 26, 1805 |  August 6, 1823 |  August 16, 1841 |
| 4 | 5 | 6 |
 August 28, 1859 |  September 7, 1877 |  September 18, 1895 |
| 7 | 8 | 9 |
 September 30, 1913 |  October 11, 1931 |  October 21, 1949 |
| 10 | 11 | 12 |
November 2, 1967 |  November 12, 1985 |  November 23, 2003 |
| 13 | 14 | 15 |
 December 4, 2021 |  December 15, 2039 |  December 26, 2057 |
| 16 | 17 | 18 |
 January 6, 2076 |  January 16, 2094 |  January 29, 2112 |
| 19 | 20 | 21 |
 February 8, 2130 |  February 19, 2148 |  March 2, 2166 |
| 22 | ||
 March 12, 2184 | ||
Themetonic 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 March 27, 1884 and August 20, 1971 | ||||
|---|---|---|---|---|
| March 27–29 | January 14 | November 1–2 | August 20–21 | June 8 |
| 108 | 110 | 112 | 114 | 116 |
 March 27, 1884 |  August 20, 1895 |  June 8, 1899 | ||
| 118 | 120 | 122 | 124 | 126 |
 March 29, 1903 |  January 14, 1907 |  November 2, 1910 |  August 21, 1914 |  June 8, 1918 |
| 128 | 130 | 132 | 134 | 136 |
 March 28, 1922 |  January 14, 1926 |  November 1, 1929 |  August 21, 1933 |  June 8, 1937 |
| 138 | 140 | 142 | 144 | 146 |
 March 27, 1941 |  January 14, 1945 |  November 1, 1948 |  August 20, 1952 |  June 8, 1956 |
| 148 | 150 | 152 | 154 | |
 March 27, 1960 |  January 14, 1964 | November 2, 1967 |  August 20, 1971 | |
This eclipse is a part of atritos cycle, repeating at alternating nodes every 135synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic 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.
The partial solar eclipse onOctober 24, 2098 (part of Saros 164) is also a part of this series but is not included in the table below.
| Series members between 1801 and 2011 | ||||
|---|---|---|---|---|
 February 11, 1804 (Saros 137) |  January 10, 1815 (Saros 138) |  December 9, 1825 (Saros 139) |  November 9, 1836 (Saros 140) |  October 9, 1847 (Saros 141) |
 September 7, 1858 (Saros 142) |  August 7, 1869 (Saros 143) |  July 7, 1880 (Saros 144) |  June 6, 1891 (Saros 145) |  May 7, 1902 (Saros 146) |
 April 6, 1913 (Saros 147) |  March 5, 1924 (Saros 148) |  February 3, 1935 (Saros 149) |  January 3, 1946 (Saros 150) |  December 2, 1956 (Saros 151) |
November 2, 1967 (Saros 152) |  October 2, 1978 (Saros 153) |  August 31, 1989 (Saros 154) |  July 31, 2000 (Saros 155) |  July 1, 2011 (Saros 156) |
This eclipse is a part of the long periodinex cycle, repeating at alternating nodes, every 358synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with theanomalistic 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 | ||
|---|---|---|
 February 11, 1823 (Saros 147) |  January 21, 1852 (Saros 148) |  December 31, 1880 (Saros 149) |
 December 12, 1909 (Saros 150) |  November 21, 1938 (Saros 151) | November 2, 1967 (Saros 152) |
 October 12, 1996 (Saros 153) |  September 21, 2025 (Saros 154) |  September 2, 2054 (Saros 155) |
 August 13, 2083 (Saros 156) |  July 23, 2112 (Saros 157) |  July 3, 2141 (Saros 158) |
 June 14, 2170 (Saros 159) |  May 24, 2199 (Saros 160) | |
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