| Total eclipse | |
 Map | |
| Gamma | 0.8661 |
|---|---|
| Magnitude | 1.0304 |
| Maximum eclipse | |
| Duration | 152 s (2 min 32 s) |
| Coordinates | 40°30′N49°36′W / 40.5°N 49.6°W /40.5; -49.6 |
| Max. width of band | 206 km (128 mi) |
| Times (UTC) | |
| Greatest eclipse | 14:54:03 |
| References | |
| Saros | 120 (56 of 71) |
| Catalog # (SE5000) | 9339 |
A totalsolar eclipse occurred at the Moon'sdescending node of orbit on Saturday, January 24, 1925,[1] with amagnitude of 1.0304. 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 1.1 days afterperigee (on January 23, 1925, at 13:30 UTC), the Moon's apparent diameter was larger.[2]
Totality was visible from southwestern and southeasternOntario inCanada (includingToronto andNiagara Falls),Minnesota,Wisconsin,Michigan,Pennsylvania,New York (including the northern part ofNew York City),New Jersey,Connecticut,Rhode Island, andMassachusetts. A partial eclipse was visible for parts ofNorth America,Central America, theCaribbean, northernSouth America,West Africa, andWestern Europe.
It was seen inNew York City. It was reported that those north of96th Street inManhattan saw a total solar eclipse while those south of 96th Street saw a partial eclipse.[3]
Visual and radio observations were conducted by researchers working withScientific American.[4]
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.[5]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1925 January 24 at 12:41:48.8 UTC |
| First Umbral External Contact | 1925 January 24 at 14:01:18.9 UTC |
| First Central Line | 1925 January 24 at 14:02:31.1 UTC |
| First Umbral Internal Contact | 1925 January 24 at 14:03:44.6 UTC |
| Ecliptic Conjunction | 1925 January 24 at 14:45:16.3 UTC |
| Greatest Duration | 1925 January 24 at 14:53:02.2 UTC |
| Greatest Eclipse | 1925 January 24 at 14:54:03.1 UTC |
| Equatorial Conjunction | 1925 January 24 at 15:06:52.3 UTC |
| Last Umbral Internal Contact | 1925 January 24 at 15:44:13.9 UTC |
| Last Central Line | 1925 January 24 at 15:45:26.2 UTC |
| Last Umbral External Contact | 1925 January 24 at 15:46:37.2 UTC |
| Last Penumbral External Contact | 1925 January 24 at 17:06:14.1 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.03044 |
| Eclipse Obscuration | 1.06180 |
| Gamma | 0.86613 |
| Sun Right Ascension | 20h25m51.5s |
| Sun Declination | -19°13'44.3" |
| Sun Semi-Diameter | 16'14.7" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 20h25m20.3s |
| Moon Declination | -18°21'36.7" |
| Moon Semi-Diameter | 16'36.2" |
| Moon Equatorial Horizontal Parallax | 1°00'56.2" |
| ΔT | 23.6 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.
| January 24 Descending node (new moon) | February 8 Ascending node (full moon) |
|---|---|
|  |
| Annular solar eclipse Solar Saros 120 | Penumbral lunar eclipse Lunar Saros 132 |
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.[6]
The partial solar eclipses onMarch 5, 1924 andAugust 30, 1924 occur in the previous lunar year eclipse set, and the solar eclipses onMay 19, 1928 andNovember 12, 1928 occur in the next lunar year eclipse set.
| Solar eclipse series sets from 1924 to 1928 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 115 | July 31, 1924 Partial | −1.4459 | 120 | January 24, 1925 Total | 0.8661 | |
| 125 | July 20, 1925 Annular | −0.7193 | 130 Totality inSumatra, Indonesia | January 14, 1926 Total | 0.1973 | |
| 135 | July 9, 1926 Annular | 0.0538 | 140 | January 3, 1927 Annular | −0.4956 | |
| 145 | June 29, 1927 Total | 0.8163 | 150 | December 24, 1927 Partial | −1.2416 | |
| 155 | June 17, 1928 Partial | 1.5107 | ||||
This eclipse is a part ofSaros series 120, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on May 27, 933 AD. It contains annular eclipses from August 11, 1059 through April 26, 1492; hybrid eclipses from May 8, 1510 through June 8, 1564; and total eclipses from June 20, 1582 throughMarch 30, 2033. The series ends at member 71 as a partial eclipse on July 7, 2195. 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 11 at 6 minutes, 24 seconds on September 11, 1113, and the longest duration of totality was produced by member 60 at 2 minutes, 50 seconds onMarch 9, 1997. All eclipses in this series occur at the Moon’sdescending node of orbit.[7]
| Series members 50–71 occur between 1801 and 2195: | ||
|---|---|---|
| 50 | 51 | 52 |
 November 19, 1816 |  November 30, 1834 |  December 11, 1852 |
| 53 | 54 | 55 |
 December 22, 1870 |  January 1, 1889 |  January 14, 1907 |
| 56 | 57 | 58 |
January 24, 1925 |  February 4, 1943 |  February 15, 1961 |
| 59 | 60 | 61 |
 February 26, 1979 |  March 9, 1997 |  March 20, 2015 |
| 62 | 63 | 64 |
 March 30, 2033 |  April 11, 2051 |  April 21, 2069 |
| 65 | 66 | 67 |
 May 2, 2087 |  May 14, 2105 |  May 25, 2123 |
| 68 | 69 | 70 |
 June 4, 2141 |  June 16, 2159 |  June 26, 2177 |
| 71 | ||
 July 7, 2195 | ||
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 April 8, 1902 and August 31, 1989 | ||||
|---|---|---|---|---|
| April 7–8 | January 24–25 | November 12 | August 31–September 1 | June 19–20 |
| 108 | 110 | 112 | 114 | 116 |
 April 8, 1902 |  August 31, 1913 |  June 19, 1917 | ||
| 118 | 120 | 122 | 124 | 126 |
 April 8, 1921 | January 24, 1925 |  November 12, 1928 |  August 31, 1932 |  June 19, 1936 |
| 128 | 130 | 132 | 134 | 136 |
 April 7, 1940 |  January 25, 1944 |  November 12, 1947 |  September 1, 1951 |  June 20, 1955 |
| 138 | 140 | 142 | 144 | 146 |
 April 8, 1959 |  January 25, 1963 |  November 12, 1966 |  August 31, 1970 |  June 20, 1974 |
| 148 | 150 | 152 | 154 | |
 April 7, 1978 |  January 25, 1982 |  November 12, 1985 |  August 31, 1989 | |
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 | ||||
|---|---|---|---|---|
 January 1, 1805 (Saros 109) |  October 31, 1826 (Saros 111) |  August 28, 1848 (Saros 113) | ||
 July 29, 1859 (Saros 114) |  June 28, 1870 (Saros 115) |  May 27, 1881 (Saros 116) |  April 26, 1892 (Saros 117) |  March 29, 1903 (Saros 118) |
 February 25, 1914 (Saros 119) | January 24, 1925 (Saros 120) |  December 25, 1935 (Saros 121) |  November 23, 1946 (Saros 122) |  October 23, 1957 (Saros 123) |
 September 22, 1968 (Saros 124) |  August 22, 1979 (Saros 125) |  July 22, 1990 (Saros 126) |  June 21, 2001 (Saros 127) |  May 20, 2012 (Saros 128) |
 April 20, 2023 (Saros 129) |  March 20, 2034 (Saros 130) |  February 16, 2045 (Saros 131) |  January 16, 2056 (Saros 132) |  December 17, 2066 (Saros 133) |
 November 15, 2077 (Saros 134) |  October 14, 2088 (Saros 135) |  September 14, 2099 (Saros 136) |  August 15, 2110 (Saros 137) |  July 14, 2121 (Saros 138) |
 June 13, 2132 (Saros 139) |  May 14, 2143 (Saros 140) |  April 12, 2154 (Saros 141) |  March 12, 2165 (Saros 142) |  February 10, 2176 (Saros 143) |
 January 9, 2187 (Saros 144) |  December 9, 2197 (Saros 145) | |||
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 | ||
|---|---|---|
 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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