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20th-century annular solar eclipse From Wikipedia, the free encyclopedia
An annular solar eclipse occurred at the Moon's ascending node of orbit on Tuesday, January 5, 1954,[1] with a magnitude of 0.972. 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. The Moon's apparent diameter was near the average diameter because it occurred 7.5 days after apogee (on December 28, 1953, at 15:10 UTC) and 5.3 days before perigee (on January 10, 1954, at 9:40 UTC).[2]
Annularity was visible from a part of Antarctica. A partial eclipse was visible for parts of Antarctica and Oceania.
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 | 1954 January 05 at 00:14:31.4 UTC |
| First Umbral External Contact | 1954 January 05 at 01:49:19.1 UTC |
| First Central Line | 1954 January 05 at 01:52:10.6 UTC |
| Greatest Duration | 1954 January 05 at 01:52:10.6 UTC |
| First Umbral Internal Contact | 1954 January 05 at 01:55:13.3 UTC |
| Equatorial Conjunction | 1954 January 05 at 02:10:41.6 UTC |
| Ecliptic Conjunction | 1954 January 05 at 02:21:50.0 UTC |
| Greatest Eclipse | 1954 January 05 at 02:32:00.6 UTC |
| Last Umbral Internal Contact | 1954 January 05 at 03:09:05.0 UTC |
| Last Central Line | 1954 January 05 at 03:12:04.6 UTC |
| Last Umbral External Contact | 1954 January 05 at 03:14:52.9 UTC |
| Last Penumbral External Contact | 1954 January 05 at 04:49:32.8 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.97203 |
| Eclipse Obscuration | 0.94484 |
| Gamma | −0.92960 |
| Sun Right Ascension | 19h01m47.3s |
| Sun Declination | -22°41'10.7" |
| Sun Semi-Diameter | 16'15.9" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 19h02m34.8s |
| Moon Declination | -23°33'33.5" |
| Moon Semi-Diameter | 15'43.5" |
| Moon Equatorial Horizontal Parallax | 0°57'42.6" |
| ΔT | 30.7 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.
| January 5 Ascending node (new moon) | January 19 Descending node (full moon) |
|---|---|
|  |
| Annular solar eclipse Solar Saros 121 | Total lunar eclipse Lunar Saros 133 |
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 eclipses on February 14, 1953 and August 9, 1953 occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 1953 to 1956 | ||||||
|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 116 | July 11, 1953 Partial |
1.4388 | 121 | January 5, 1954 Annular |
−0.9296 | |
| 126 | June 30, 1954 Total |
0.6135 | 131 | December 25, 1954 Annular |
−0.2576 | |
| 136 | June 20, 1955 Total |
−0.1528 | 141 | December 14, 1955 Annular |
0.4266 | |
| 146 | June 8, 1956 Total |
−0.8934 | 151 | December 2, 1956 Partial |
1.0923 | |
This eclipse is a part of Saros series 121, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on April 25, 944 AD. It contains total eclipses from July 10, 1070 through October 9, 1809; hybrid eclipses on October 20, 1827 and October 30, 1845; and annular eclipses from November 11, 1863 through February 28, 2044. The series ends at member 71 as a partial eclipse on June 7, 2206. 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 39 at 6 minutes, 20 seconds on June 21, 1629, and the longest duration of annularity will be produced by member 62 at 2 minutes, 27 seconds on February 28, 2044. All eclipses in this series occur at the Moon’s ascending node of orbit.[5]
| Series members 49–70 occur between 1801 and 2200: | ||
|---|---|---|
| 49 | 50 | 51 |
 October 9, 1809 |
 October 20, 1827 |
 October 30, 1845 |
| 52 | 53 | 54 |
 November 11, 1863 |
 November 21, 1881 |
 December 3, 1899 |
| 55 | 56 | 57 |
 December 14, 1917 |
 December 25, 1935 |
January 5, 1954 |
| 58 | 59 | 60 |
 January 16, 1972 |
 January 26, 1990 |
 February 7, 2008 |
| 61 | 62 | 63 |
 February 17, 2026 |
 February 28, 2044 |
 March 11, 2062 |
| 64 | 65 | 66 |
 March 21, 2080 |
 April 1, 2098 |
 April 13, 2116 |
| 67 | 68 | 69 |
 April 24, 2134 |
 May 4, 2152 |
 May 16, 2170 |
| 70 | ||
 May 26, 2188 | ||
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.
| 22 eclipse events between January 5, 1935 and August 11, 2018 | ||||
|---|---|---|---|---|
| January 4–5 | October 23–24 | August 10–12 | May 30–31 | March 18–19 |
| 111 | 113 | 115 | 117 | 119 |
 January 5, 1935 |
 August 12, 1942 |
 May 30, 1946 |
 March 18, 1950 | |
| 121 | 123 | 125 | 127 | 129 |
January 5, 1954 |
 October 23, 1957 |
 August 11, 1961 |
 May 30, 1965 |
 March 18, 1969 |
| 131 | 133 | 135 | 137 | 139 |
 January 4, 1973 |
 October 23, 1976 |
 August 10, 1980 |
 May 30, 1984 |
 March 18, 1988 |
| 141 | 143 | 145 | 147 | 149 |
 January 4, 1992 |
 October 24, 1995 |
 August 11, 1999 |
 May 31, 2003 |
 March 19, 2007 |
| 151 | 153 | 155 | ||
 January 4, 2011 |
 October 23, 2014 |
 August 11, 2018 | ||
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 | ||||
|---|---|---|---|---|
 March 14, 1801 (Saros 107) |
 February 12, 1812 (Saros 108) |
 January 12, 1823 (Saros 109) |
 November 10, 1844 (Saros 111) | |
 August 9, 1877 (Saros 114) |
 July 9, 1888 (Saros 115) |
 June 8, 1899 (Saros 116) | ||
 May 9, 1910 (Saros 117) |
 April 8, 1921 (Saros 118) |
 March 7, 1932 (Saros 119) |
 February 4, 1943 (Saros 120) |
January 5, 1954 (Saros 121) |
 December 4, 1964 (Saros 122) |
 November 3, 1975 (Saros 123) |
 October 3, 1986 (Saros 124) |
 September 2, 1997 (Saros 125) |
 August 1, 2008 (Saros 126) |
 July 2, 2019 (Saros 127) |
 June 1, 2030 (Saros 128) |
 April 30, 2041 (Saros 129) |
 March 30, 2052 (Saros 130) |
 February 28, 2063 (Saros 131) |
 January 27, 2074 (Saros 132) |
 December 27, 2084 (Saros 133) |
 November 27, 2095 (Saros 134) |
 October 26, 2106 (Saros 135) |
 September 26, 2117 (Saros 136) |
 August 25, 2128 (Saros 137) |
 July 25, 2139 (Saros 138) |
 June 25, 2150 (Saros 139) |
 May 25, 2161 (Saros 140) |
 April 23, 2172 (Saros 141) |
 March 23, 2183 (Saros 142) |
 February 21, 2194 (Saros 143) | |||
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 14, 1809 (Saros 116) |
 March 25, 1838 (Saros 117) |
 March 6, 1867 (Saros 118) |
 February 13, 1896 (Saros 119) |
 January 24, 1925 (Saros 120) |
January 5, 1954 (Saros 121) |
 December 15, 1982 (Saros 122) |
 November 25, 2011 (Saros 123) |
 November 4, 2040 (Saros 124) |
 October 15, 2069 (Saros 125) |
 September 25, 2098 (Saros 126) |
 September 6, 2127 (Saros 127) |
 August 16, 2156 (Saros 128) |
 July 26, 2185 (Saros 129) |
|
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