| Total eclipse | |||||||||||||||||
 The Moon's hourly motion shown right to left | |||||||||||||||||
| Date | October 18, 1967 | ||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Gamma | −0.3653 | ||||||||||||||||
| Magnitude | 1.1426 | ||||||||||||||||
| Saros cycle | 126 (43 of 72) | ||||||||||||||||
| Totality | 59 minutes, 45 seconds | ||||||||||||||||
| Partiality | 218 minutes, 52 seconds | ||||||||||||||||
| Penumbral | 367 minutes, 7 seconds | ||||||||||||||||
| |||||||||||||||||
A totallunar eclipse occurred at the Moon’sascending node of orbit on Wednesday, October 18, 1967,[1] with an umbralmagnitude of 1.1426. A lunar eclipse occurs when theMoon moves into theEarth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. Unlike asolar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on thenight side of Earth. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon'sshadow is smaller. Occurring only about 22 hours beforeapogee (on October 19, 1967, at 8:30 UTC), the Moon's apparent diameter was smaller.[2]
This lunar eclipse was the second of atetrad, with four total lunar eclipses in series, the others being onApril 24, 1967;April 13, 1968; andOctober 6, 1968.
The eclipse was completely visible overnortheast Asia, westernNorth America, and thePacific Ocean, seen rising overAsia andAustralia and setting over eastern North America andSouth America.[3]
 |
Shown below is a table displaying details about this particular lunar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Parameter | Value |
|---|---|
| Penumbral magnitude | 2.23368 |
| Umbral magnitude | 1.14258 |
| Gamma | −0.36529 |
| Sun right ascension | 13h30m10.8s |
| Sun declination | -09°26'26.5" |
| Sun semi-diameter | 16'03.3" |
| Sun equatorial horizontal parallax | 08.8" |
| Moon right ascension | 01h30m47.5s |
| Moon declination | +09°08'55.1" |
| Moon semi-diameter | 14'42.8" |
| Moon equatorial horizontal parallax | 0°54'00.0" |
| 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 lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternatingnodes of the Moon's orbit.[5]
The penumbral lunar eclipse onAugust 27, 1969 occurs in the next lunar year eclipse set.
| Lunar eclipse series sets from 1966 to 1969 | ||||||||
|---|---|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||||
| Saros | Date Viewing | Type Chart | Gamma | Saros | Date Viewing | Type Chart | Gamma | |
| 111 | 1966 May 04 | Penumbral | 1.0554 | 116 | 1966 Oct 29 | Penumbral | −1.0600 | |
| 121 | 1967 Apr 24 | Total | 0.2972 | 126 | 1967 Oct 18 | Total | −0.3653 | |
| 131 | 1968 Apr 13 | Total | −0.4173 | 136 | 1968 Oct 06 | Total | 0.3605 | |
| 141 | 1969 Apr 02 | Penumbral | −1.1765 | 146 | 1969 Sep 25 | Penumbral | 1.0656 | |
This eclipse is the third of fourMetonic cycle lunar eclipses on the same date, April 23–24, each separated by 19 years:
TheMetonic cycle repeats nearly exactly every 19 years and represents aSaros cycle plus one lunar year. Because it occurs on the same calendar date, the Earth's shadow will in nearly the same location relative to the background stars.
| Descending node | Ascending node | |||||
|---|---|---|---|---|---|---|
| Saros | Date | Type | Saros | Date | Type | |
| 111 | 1948 Apr 23 | Partial | 116 | 1948 Oct 18 | Penumbral | |
 |  | |||||
| 121 | 1967 Apr 24 | Total | 126 | 1967 Oct 18 | Total | |
| | |||||
| 131 | 1986 Apr 24 | Total | 136 | 1986 Oct 17 | Total | |
 |  | |||||
| 141 | 2005 Apr 24 | Penumbral | 146 | 2005 Oct 17 | Partial | |
 |  | |||||
This eclipse is a part ofSaros series 126, repeating every 18 years, 11 days, and containing 70 events. The series started with a penumbral lunar eclipse on July 18, 1228. It contains partial eclipses from March 24, 1625 through June 9, 1751; total eclipses from June 19, 1769 throughNovember 9, 2003; and a second set of partial eclipses fromNovember 19, 2021 through June 5, 2346. The series ends at member 70 as a penumbral eclipse on August 19, 2472.
The longest duration of totality was produced by member 36 at 106 minutes, 27 seconds onAugust 13, 1859. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Greatest | First | |||
|---|---|---|---|---|
| The greatest eclipse of the series occurred on1859 Aug 13, lasting 106 minutes, 27 seconds.[7] | Penumbral | Partial | Total | Central |
| 1228 Jul 18 | 1625 Mar 24 | 1769 Jun 19 | 1805 Jul 11 | |
| Last | ||||
| Central | Total | Partial | Penumbral | |
1931 Sep 26 | 2003 Nov 09 | 2346 Jun 05 | 2472 Aug 19 | |
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.
| Series members 33–54 occur between 1801 and 2200: | |||||
|---|---|---|---|---|---|
| 33 | 34 | 35 | |||
| 1805 Jul 11 | 1823 Jul 23 | 1841 Aug 02 | |||
| 36 | 37 | 38 | |||
| 1859 Aug 13 | 1877 Aug 23 | 1895 Sep 04 | |||
| 39 | 40 | 41 | |||
| 1913 Sep 15 | 1931 Sep 26 | 1949 Oct 07 | |||
 |  | |  |  |  |
| 42 | 43 | 44 | |||
| 1967 Oct 18 | 1985 Oct 28 | 2003 Nov 09 | |||
| |  |  | |  |
| 45 | 46 | 47 | |||
| 2021 Nov 19 | 2039 Nov 30 | 2057 Dec 11 | |||
 |  |  |  |  |  |
| 48 | 49 | 50 | |||
| 2075 Dec 22 | 2094 Jan 01 | 2112 Jan 14 | |||
| 51 | 52 | 53 | |||
| 2130 Jan 24 | 2148 Feb 04 | 2166 Feb 15 | |||
| 54 | |||||
| 2184 Feb 26 | |||||
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.
| Series members between 1801 and 2200 | |||||||||
|---|---|---|---|---|---|---|---|---|---|
| 1804 Jan 26 (Saros 111) | 1814 Dec 26 (Saros 112) | 1825 Nov 25 (Saros 113) | 1836 Oct 24 (Saros 114) | 1847 Sep 24 (Saros 115) | |||||
| 1858 Aug 24 (Saros 116) | 1869 Jul 23 (Saros 117) | 1880 Jun 22 (Saros 118) | 1891 May 23 (Saros 119) | 1902 Apr 22 (Saros 120) | |||||
 |  | ||||||||
| 1913 Mar 22 (Saros 121) | 1924 Feb 20 (Saros 122) | 1935 Jan 19 (Saros 123) | 1945 Dec 19 (Saros 124) | 1956 Nov 18 (Saros 125) | |||||
 |  |  |  |  |  |  |  |  |  |
| 1967 Oct 18 (Saros 126) | 1978 Sep 16 (Saros 127) | 1989 Aug 17 (Saros 128) | 2000 Jul 16 (Saros 129) | 2011 Jun 15 (Saros 130) | |||||
| |  |  |  |  |  |  |  |  |
| 2022 May 16 (Saros 131) | 2033 Apr 14 (Saros 132) | 2044 Mar 13 (Saros 133) | 2055 Feb 11 (Saros 134) | 2066 Jan 11 (Saros 135) | |||||
 |  |  |  |  |  |  |  |  |  |
| 2076 Dec 10 (Saros 136) | 2087 Nov 10 (Saros 137) | 2098 Oct 10 (Saros 138) | 2109 Sep 09 (Saros 139) | 2120 Aug 09 (Saros 140) | |||||
 |  |  |  |  |  | ||||
| 2131 Jul 10 (Saros 141) | 2142 Jun 08 (Saros 142) | 2153 May 08 (Saros 143) | 2164 Apr 07 (Saros 144) | 2175 Mar 07 (Saros 145) | |||||
| 2186 Feb 04 (Saros 146) | 2197 Jan 04 (Saros 147) | ||||||||
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 | |||||
|---|---|---|---|---|---|
| 1823 Jan 26 (Saros 121) | 1852 Jan 07 (Saros 122) | 1880 Dec 16 (Saros 123) | |||
| 1909 Nov 27 (Saros 124) | 1938 Nov 07 (Saros 125) | 1967 Oct 18 (Saros 126) | |||
 |  |  |  | | |
| 1996 Sep 27 (Saros 127) | 2025 Sep 07 (Saros 128) | 2054 Aug 18 (Saros 129) | |||
 |  |  |  |  |  |
| 2083 Jul 29 (Saros 130) | 2112 Jul 09 (Saros 131) | 2141 Jun 19 (Saros 132) | |||
 |  | ||||
| 2170 May 30 (Saros 133) | 2199 May 10 (Saros 134) | ||||
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (ahalf saros).[8] This lunar eclipse is related to two total solar eclipses ofSolar Saros 133.
| October 12, 1958 | October 23, 1976 |
|---|---|
 |  |
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