| Partial eclipse | |
 Map | |
| Gamma | 1.2857 |
|---|---|
| Magnitude | 0.4729 |
| Maximum eclipse | |
| Coordinates | 66°12′N150°06′E / 66.2°N 150.1°E /66.2; 150.1 |
| Times (UTC) | |
| Greatest eclipse | 13:16:21 |
| References | |
| Saros | 116 (67 of 70) |
| Catalog # (SE5000) | 9322 |
A partialsolar eclipse occurred at the Moon'sdescending node of orbit on Tuesday, June 19, 1917,[1] with amagnitude of 0.4729. 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 solar eclipses in 1917, with the others occurring onJanuary 23,July 19, andDecember 14.
A partial eclipse was visible for parts of northernNorth America,Northern Europe, andNorth Asia.
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 | 1917 June 19 at 11:36:05.9 UTC |
| Ecliptic Conjunction | 1917 June 19 at 13:02:07.8 UTC |
| Equatorial Conjunction | 1917 June 19 at 13:04:46.6 UTC |
| Greatest Eclipse | 1917 June 19 at 13:16:20.5 UTC |
| Last Penumbral External Contact | 1917 June 19 at 14:56:44.7 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.47297 |
| Eclipse Obscuration | 0.35726 |
| Gamma | 1.28565 |
| Sun Right Ascension | 05h49m46.5s |
| Sun Declination | +23°25'46.5" |
| Sun Semi-Diameter | 15'44.3" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 05h50m11.1s |
| Moon Declination | +24°36'49.5" |
| Moon Semi-Diameter | 15'08.6" |
| Moon Equatorial Horizontal Parallax | 0°55'34.6" |
| ΔT | 19.6 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. The first and last eclipse in this sequence is separated by onesynodic month.
| June 19 Descending node (new moon) | July 4 Ascending node (full moon) | July 19 Descending node (new moon) |
|---|---|---|
|  |  |
| Partial solar eclipse Solar Saros 116 | Total lunar eclipse Lunar Saros 128 | Partial solar eclipse Solar Saros 154 |
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 solar eclipses onFebruary 3, 1916 (total),July 30, 1916 (annular),January 23, 1917 (partial), andJuly 19, 1917 (partial) occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 1916 to 1920 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 111 | December 24, 1916 Partial | −1.5321 | 116 | June 19, 1917 Partial | 1.2857 | |
| 121 | December 14, 1917 Annular | −0.9157 | 126 | June 8, 1918 Total | 0.4658 | |
| 131 | December 3, 1918 Annular | −0.2387 | 136 Totality inPríncipe | May 29, 1919 Total | −0.2955 | |
| 141 | November 22, 1919 Annular | 0.4549 | 146 | May 18, 1920 Partial | −1.0239 | |
| 151 | November 10, 1920 Partial | 1.1287 | ||||
This eclipse is a part ofSaros series 116, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on June 23, 727 AD. It contains annular eclipses from October 10, 907 AD through May 6, 1845. There are no hybrid or total eclipses in this set. The series ends at member 70 as a partial eclipse onJuly 22, 1971. 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 51 at 12 minutes, 2 seconds on December 25, 1628. All eclipses in this series occur at the Moon’sdescending node of orbit.[4]
| Series members 61–70 occur between 1801 and 1971: | ||
|---|---|---|
| 61 | 62 | 63 |
 April 14, 1809 |  April 26, 1827 |  May 6, 1845 |
| 64 | 65 | 66 |
 May 17, 1863 |  May 27, 1881 |  June 8, 1899 |
| 67 | 68 | 69 |
June 19, 1917 |  June 30, 1935 |  July 11, 1953 |
| 70 | ||
 July 22, 1971 | ||
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 | ||||
|---|---|---|---|---|
 March 25, 1819 (Saros 107) |  February 23, 1830 (Saros 108) |  January 22, 1841 (Saros 109) |  November 21, 1862 (Saros 111) | |
 August 20, 1895 (Saros 114) |  July 21, 1906 (Saros 115) | June 19, 1917 (Saros 116) | ||
 May 19, 1928 (Saros 117) |  April 19, 1939 (Saros 118) |  March 18, 1950 (Saros 119) |  February 15, 1961 (Saros 120) |  January 16, 1972 (Saros 121) |
 December 15, 1982 (Saros 122) |  November 13, 1993 (Saros 123) |  October 14, 2004 (Saros 124) |  September 13, 2015 (Saros 125) |  August 12, 2026 (Saros 126) |
 July 13, 2037 (Saros 127) |  June 11, 2048 (Saros 128) |  May 11, 2059 (Saros 129) |  April 11, 2070 (Saros 130) |  March 10, 2081 (Saros 131) |
 February 7, 2092 (Saros 132) |  January 8, 2103 (Saros 133) |  December 8, 2113 (Saros 134) |  November 6, 2124 (Saros 135) |  October 7, 2135 (Saros 136) |
 September 6, 2146 (Saros 137) |  August 5, 2157 (Saros 138) |  July 5, 2168 (Saros 139) |  June 5, 2179 (Saros 140) |  May 4, 2190 (Saros 141) |
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 8, 1801 (Saros 112) |  August 18, 1830 (Saros 113) |  July 29, 1859 (Saros 114) |
 July 9, 1888 (Saros 115) | June 19, 1917 (Saros 116) |  May 30, 1946 (Saros 117) |
 May 11, 1975 (Saros 118) |  April 19, 2004 (Saros 119) |  March 30, 2033 (Saros 120) |
 March 11, 2062 (Saros 121) |  February 18, 2091 (Saros 122) |  January 30, 2120 (Saros 123) |
 January 9, 2149 (Saros 124) |  December 20, 2177 (Saros 125) | |
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