| Total eclipse | |
 Map | |
| Gamma | 0.8628 |
|---|---|
| Magnitude | 1.0281 |
| Maximum eclipse | |
| Duration | 145 s (2 min 25 s) |
| Coordinates | 38°18′N86°24′E / 38.3°N 86.4°E /38.3; 86.4 |
| Max. width of band | 189 km (117 mi) |
| Times (UTC) | |
| Greatest eclipse | 6:05:43 |
| References | |
| Saros | 120 (55 of 71) |
| Catalog # (SE5000) | 9297 |
A totalsolar eclipse occurred at the Moon'sdescending node of orbit on Monday, January 14, 1907,[1] with amagnitude of 1.0281. 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 1.2 days afterperigee (on January 13, 1906, at 2:20 UTC), the Moon's apparent diameter was larger.[2]
Totality was visible fromRussian Empire (the parts now belonging toRussia,Kazakhstan,Uzbekistan,Tajikistan andKyrgyzstan) andChina (nownorthwestern China,Mongolia and northern part ofnortheastern China).[3] A partial eclipse was visible for most ofAsia.
TheCamden Morning Post described its path as such:[4]
The shadow track begins on the banks of the Don, in Southern Russia, where the sun rises as totality is ending. It passes over the northern part of the Caspian Sea, where totality begins at sunrise, ant then over theAral Sea and throughRussian Turkestan,Samarkand being the principal town on the shadow track. Then it passes through thePamirs and into Central Asia, through thedesert of Gobi, ending finally on theRiver Amur, where totality commences at sunset.[4]
At the time, "some confusion" existed about the date of the event: "theastronomical day begins at noon, thecivil day at midnight, twelve hours earlier. Hence, according to the one system the eclipse will occur on Jan. 13, and according to the other on Jan. 14."[4]
The day of the eclipse, it was reported in theRoanoke Times that:
according to the cable dispatches, astronomers, physicists, photographers and scientists of all branches have pitched their camps to take observations. Near the city of Tashkent eminent groups of scientists under the patronage of universities and royal societies of France, Germany, Russia and other countries have set up their instruments with long, unpronouncable names in order to observe the eclipse.[5]
Apart from ground-based observations, the researchers also attempted to perform atmospheric studies with the aid ofweather balloons.[6] TheHamburg Observatory sent an expedition toSamarkand, to the south of Tashkent, which was expected to join up with the rest. The expedition from Paris was carried out by the Meudon Observatory, under M. Stefanik, and the British expedition by the British Astronomical Association.[4] According to journalist Mary Proctor, despite the recent construction of railways in the region, an attempt to join one of the expeditions and report on the eclipse from the location of observation had proven fruitless: "The Russian representatives in this country refused to take any responsibility if the writer ventured into Western Turkestan [...] According to information received from the Secretary of State, who lived in China twenty-three years, it would require a month to journey from Peking to Tsair-Osu. The desert of Gobi had to be crossed, and the journey made on horseback, an armed escort being necessary, as this region is also under Russian government."[4]
The Guardian reported that the eclipse was observed by "special scientific expeditions atSamarkand andTashkent, inRussian Turkestan"; aReuters correspondent telegraphed from Samarkand that the eclipse had been observed from the railway between the stations of Kuropatkin and Mijulnskaja, as snow fell.[3] Meanwhile, a visit by Afghan amirHabibullah Khan andLord Kitchener toAgra[7][8] took place under a "distinct three-quarter eclipse of the sun".[8] On the western edge of the path, the eclipse was observed fromYessentuki.[9]
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.[10]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1907 January 14 at 03:52:57.4 UTC |
| First Umbral External Contact | 1907 January 14 at 05:12:27.1 UTC |
| First Central Line | 1907 January 14 at 05:13:31.0 UTC |
| First Umbral Internal Contact | 1907 January 14 at 05:14:35.8 UTC |
| Ecliptic Conjunction | 1907 January 14 at 05:56:57.5 UTC |
| Greatest Duration | 1907 January 14 at 06:04:51.3 UTC |
| Greatest Eclipse | 1907 January 14 at 06:05:43.0 UTC |
| Equatorial Conjunction | 1907 January 14 at 06:12:01.9 UTC |
| Last Umbral Internal Contact | 1907 January 14 at 06:56:47.3 UTC |
| Last Central Line | 1907 January 14 at 06:57:50.7 UTC |
| Last Umbral External Contact | 1907 January 14 at 06:58:53.2 UTC |
| Last Penumbral External Contact | 1907 January 14 at 08:18:28.4 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.02812 |
| Eclipse Obscuration | 1.05702 |
| Gamma | 0.86277 |
| Sun Right Ascension | 19h39m03.3s |
| Sun Declination | -21°29'55.0" |
| Sun Semi-Diameter | 16'15.6" |
| Sun Equatorial Horizontal Parallax | 08.9" |
| Moon Right Ascension | 19h38m47.6s |
| Moon Declination | -20°37'40.5" |
| Moon Semi-Diameter | 16'34.8" |
| Moon Equatorial Horizontal Parallax | 1°00'50.9" |
| ΔT | 6.2 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 14 Descending node (new moon) | January 29 Ascending node (full moon) |
|---|---|
|  |
| Total solar eclipse Solar Saros 120 | Partial 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.[11]
The partial solar eclipses onFebruary 23, 1906 andAugust 20, 1906 occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 1906 to 1909 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 115 | July 21, 1906 Partial | −1.3637 | 120 | January 14, 1907 Total | 0.8628 | |
| 125 | July 10, 1907 Annular | −0.6313 | 130 | January 3, 1908 Total | 0.1934 | |
| 135 | June 28, 1908 Annular | 0.1389 | 140 | December 23, 1908 Hybrid | −0.4985 | |
| 145 | June 17, 1909 Hybrid | 0.8957 | 150 | December 12, 1909 Partial | −1.2456 | |
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.[12]
| 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 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.
| Series members between 1801 and 2200 | ||||
|---|---|---|---|---|
 October 19, 1808 (Saros 111) |  September 19, 1819 (Saros 112) |  August 18, 1830 (Saros 113) |  July 18, 1841 (Saros 114) |  June 17, 1852 (Saros 115) |
 May 17, 1863 (Saros 116) |  April 16, 1874 (Saros 117) |  March 16, 1885 (Saros 118) |  February 13, 1896 (Saros 119) | January 14, 1907 (Saros 120) |
 December 14, 1917 (Saros 121) |  November 12, 1928 (Saros 122) |  October 12, 1939 (Saros 123) |  September 12, 1950 (Saros 124) |  August 11, 1961 (Saros 125) |
 July 10, 1972 (Saros 126) |  June 11, 1983 (Saros 127) |  May 10, 1994 (Saros 128) |  April 8, 2005 (Saros 129) |  March 9, 2016 (Saros 130) |
 February 6, 2027 (Saros 131) |  January 5, 2038 (Saros 132) |  December 5, 2048 (Saros 133) |  November 5, 2059 (Saros 134) |  October 4, 2070 (Saros 135) |
 September 3, 2081 (Saros 136) |  August 3, 2092 (Saros 137) |  July 4, 2103 (Saros 138) |  June 3, 2114 (Saros 139) |  May 3, 2125 (Saros 140) |
 April 1, 2136 (Saros 141) |  March 2, 2147 (Saros 142) |  January 30, 2158 (Saros 143) |  December 29, 2168 (Saros 144) |  November 28, 2179 (Saros 145) |
 October 29, 2190 (Saros 146) | ||||
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 | ||
|---|---|---|
 March 14, 1820 (Saros 117) |  February 23, 1849 (Saros 118) |  February 2, 1878 (Saros 119) |
January 14, 1907 (Saros 120) |  December 25, 1935 (Saros 121) |  December 4, 1964 (Saros 122) |
 November 13, 1993 (Saros 123) |  October 25, 2022 (Saros 124) |  October 4, 2051 (Saros 125) |
 September 13, 2080 (Saros 126) |  August 26, 2109 (Saros 127) |  August 5, 2138 (Saros 128) |
 July 16, 2167 (Saros 129) |  June 26, 2196 (Saros 130) | |
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