| Partial eclipse | |
 Map | |
| Gamma | −1.1393 |
|---|---|
| Magnitude | 0.7545 |
| Maximum eclipse | |
| Coordinates | 65°00′S135°54′E / 65°S 135.9°E /-65; 135.9 |
| Times (UTC) | |
| Greatest eclipse | 4:34:07 |
| References | |
| Saros | 117 (66 of 71) |
| Catalog # (SE5000) | 9430 |
A partialsolar eclipse occurred at the Moon'sascending node of orbit on Wednesday, June 10, 1964,[1] with amagnitude of 0.7545. 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 partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth.
This was the second of four partial solar eclipses in 1964, with the others occurring onJanuary 14,July 9, andDecember 4.
A partial eclipse was visible for parts ofAustralia and westernOceania.
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.[2]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1964 June 10 at 02:49:28.6 UTC |
| Equatorial Conjunction | 1964 June 10 at 04:13:17.5 UTC |
| Ecliptic Conjunction | 1964 June 10 at 04:22:52.0 UTC |
| Greatest Eclipse | 1964 June 10 at 04:34:07.0 UTC |
| Last Penumbral External Contact | 1964 June 10 at 06:18:54.5 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.75455 |
| Eclipse Obscuration | 0.70285 |
| Gamma | −1.13926 |
| Sun Right Ascension | 05h13m32.2s |
| Sun Declination | +23°00'50.0" |
| Sun Semi-Diameter | 15'45.1" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 05h14m24.9s |
| Moon Declination | +21°52'09.4" |
| Moon Semi-Diameter | 16'43.2" |
| Moon Equatorial Horizontal Parallax | 1°01'21.8" |
| ΔT | 35.3 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. The first and last eclipse in this sequence is separated by onesynodic month.
| June 10 Ascending node (new moon) | June 25 Descending node (full moon) | July 9 Ascending node (new moon) |
|---|---|---|
|  |  |
| Partial solar eclipse Solar Saros 117 | Total lunar eclipse Lunar Saros 129 | Partial solar eclipse Solar Saros 155 |
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.[3]
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 117, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on June 24, 792 AD. It contains annular eclipses from September 18, 936 AD through May 14, 1333; hybrid eclipses from May 25, 1351 through July 8, 1423; and total eclipses from July 18, 1441 throughMay 19, 1928. The series ends at member 71 as a partial eclipse onAugust 3, 2054. 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 annularity was produced by member 16 at 9 minutes, 26 seconds on December 3, 1062, and the longest duration of totality was produced by member 62 at 4 minutes, 19 seconds onApril 26, 1892. All eclipses in this series occur at the Moon’sascending node of orbit.[4]
| Series members 57–71 occur between 1801 and 2054: | ||
|---|---|---|
| 57 | 58 | 59 |
 March 4, 1802 |  March 14, 1820 |  March 25, 1838 |
| 60 | 61 | 62 |
 April 5, 1856 |  April 16, 1874 |  April 26, 1892 |
| 63 | 64 | 65 |
 May 9, 1910 |  May 19, 1928 |  May 30, 1946 |
| 66 | 67 | 68 |
June 10, 1964 |  June 21, 1982 |  July 1, 2000 |
| 69 | 70 | 71 |
 July 13, 2018 |  July 23, 2036 |  August 3, 2054 |
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 ascending node.
| 20 eclipse events between June 10, 1964 and August 21, 2036 | ||||
|---|---|---|---|---|
| June 10–11 | March 28–29 | January 14–16 | November 3 | August 21–22 |
| 117 | 119 | 121 | 123 | 125 |
June 10, 1964 |  March 28, 1968 |  January 16, 1972 |  November 3, 1975 |  August 22, 1979 |
| 127 | 129 | 131 | 133 | 135 |
 June 11, 1983 |  March 29, 1987 |  January 15, 1991 |  November 3, 1994 |  August 22, 1998 |
| 137 | 139 | 141 | 143 | 145 |
 June 10, 2002 |  March 29, 2006 |  January 15, 2010 |  November 3, 2013 |  August 21, 2017 |
| 147 | 149 | 151 | 153 | 155 |
 June 10, 2021 |  March 29, 2025 |  January 14, 2029 |  November 3, 2032 |  August 21, 2036 |
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 1866 and 2200 | ||||
|---|---|---|---|---|
 March 16, 1866 (Saros 108) |  December 13, 1898 (Saros 111) | |||
 September 12, 1931 (Saros 114) |  August 12, 1942 (Saros 115) |  July 11, 1953 (Saros 116) | June 10, 1964 (Saros 117) | |
 May 11, 1975 (Saros 118) |  April 9, 1986 (Saros 119) |  March 9, 1997 (Saros 120) |  February 7, 2008 (Saros 121) |  January 6, 2019 (Saros 122) |
 December 5, 2029 (Saros 123) |  November 4, 2040 (Saros 124) |  October 4, 2051 (Saros 125) |  September 3, 2062 (Saros 126) |  August 3, 2073 (Saros 127) |
 July 3, 2084 (Saros 128) |  June 2, 2095 (Saros 129) |  May 3, 2106 (Saros 130) |  April 2, 2117 (Saros 131) |  March 1, 2128 (Saros 132) |
 January 30, 2139 (Saros 133) |  December 30, 2149 (Saros 134) |  November 27, 2160 (Saros 135) |  October 29, 2171 (Saros 136) |  September 27, 2182 (Saros 137) |
 August 26, 2193 (Saros 138) | ||||
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 | ||
|---|---|---|
 September 19, 1819 (Saros 112) |  August 28, 1848 (Saros 113) |  August 9, 1877 (Saros 114) |
 July 21, 1906 (Saros 115) |  June 30, 1935 (Saros 116) | June 10, 1964 (Saros 117) |
 May 21, 1993 (Saros 118) |  April 30, 2022 (Saros 119) |  April 11, 2051 (Saros 120) |
 March 21, 2080 (Saros 121) |  March 1, 2109 (Saros 122) |  February 9, 2138 (Saros 123) |
 January 21, 2167 (Saros 124) |  December 31, 2195 (Saros 125) | |
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