| Annular eclipse | |
 Map | |
| Gamma | 0.1299 |
|---|---|
| Magnitude | 0.9367 |
| Maximum eclipse | |
| Duration | 487 s (8 min 7 s) |
| Coordinates | 5°36′N94°42′E / 5.6°N 94.7°E /5.6; 94.7 |
| Max. width of band | 237 km (147 mi) |
| Times (UTC) | |
| Greatest eclipse | 5:40:44 |
| References | |
| Saros | 128 (52 of 73) |
| Catalog # (SE5000) | 9290 |
An annularsolar eclipse occurred at the Moon'sdescending node of orbit on Thursday, March 17, 1904,[1][2][3][4][5] with amagnitude of 0.9367. Asolar eclipse occurs when theMoon passes betweenEarth and theSun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon'sapparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like anannulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. Occurring about 3 days afterapogee (on March 14, 1904, at 6:00 UTC), the Moon's apparent diameter was smaller.[6]
The path of annularity covered southernGerman East Africa (now southernTanzania), northeastern tip ofPortuguese East Africa (nowMozambique), northernGrande Comore Island inFrench Comoros (nowComoros), southernBritish Seychelles (nowSeychelles), Archipelago ofAgaléga which is located far away from the main island ofBritish Mauritius (nowMauritius), most of theBritish Indian Ocean Territory (excluding the southern part ofDiego Garcia), northwesternSumatra in theDutch East Indies (nowIndonesia), southern Siam (now renamed asThailand),French Indochina (the part now belonging toCambodia, the southern tip ofLaos and southernVietnam, including the major cityPhnom Penh, now capital of Cambodia), all of theParacel Islands, the northern tip of theAmerican Philippines (nowPhilippines) andJapanese remote islands ofIwo Jima,South Iwo Jima andMinamitorishima.
In addition, a partial solar eclipse was seen within a much larger area, including the eastern half ofAfrica, southernWest Asia, southernAfghanistan,South Asia except the northernmost tip ofBritish Raj (now the northernmost tip ofPakistan), most ofChina except the northwest border,Korean Peninsula, Japan,Southeast Asia, the extreme northern coast ofAustralia, northwesternMelanesia, central and westernMicronesia, and southeasternRussian Empire.
N. Donitch of the Royal Russian Academy of Sciences (the predecessor of today's Russian Academy of Sciences) traveled to Phnom Penh (now capital of Cambodia) via Saigon (nowHo Chi Minh City, Vietnam) in French Indochina and made observations there. The weather was clear on the eclipse day, with only some fog in the morning. Donitch used aspectrometer and recorded changes in the temperature in about 2.5 hours, which dropped for about 3 °C.[7]
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.[8]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1904 March 17 at 02:36:24.1 UTC |
| First Umbral External Contact | 1904 March 17 at 03:41:08.2 UTC |
| First Central Line | 1904 March 17 at 03:43:53.3 UTC |
| First Umbral Internal Contact | 1904 March 17 at 03:46:38.6 UTC |
| First Penumbral Internal Contact | 1904 March 17 at 04:52:21.2 UTC |
| Greatest Duration | 1904 March 17 at 05:37:38.0 UTC |
| Ecliptic Conjunction | 1904 March 17 at 05:39:11.3 UTC |
| Greatest Eclipse | 1904 March 17 at 05:40:44.1 UTC |
| Equatorial Conjunction | 1904 March 17 at 05:45:36.1 UTC |
| Last Penumbral Internal Contact | 1904 March 17 at 06:28:59.4 UTC |
| Last Umbral Internal Contact | 1904 March 17 at 07:34:47.3 UTC |
| Last Central Line | 1904 March 17 at 07:37:30.8 UTC |
| Last Umbral External Contact | 1904 March 17 at 07:40:14.2 UTC |
| Last Penumbral External Contact | 1904 March 17 at 08:44:57.8 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.93675 |
| Eclipse Obscuration | 0.87751 |
| Gamma | 0.12993 |
| Sun Right Ascension | 23h46m07.3s |
| Sun Declination | -01°30'13.7" |
| Sun Semi-Diameter | 16'04.1" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 23h45m58.8s |
| Moon Declination | -01°23'30.5" |
| Moon Semi-Diameter | 14'49.6" |
| Moon Equatorial Horizontal Parallax | 0°54'24.9" |
| ΔT | 2.9 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.
| March 2 Ascending node (full moon) | March 17 Descending node (new moon) | March 31 Ascending node (full moon) |
|---|---|---|
 | |  |
| Penumbral lunar eclipse Lunar Saros 102 | Annular solar eclipse Solar Saros 128 | Penumbral lunar eclipse Lunar Saros 140 |
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.[9]
The partial solar eclipses onMay 7, 1902 andOctober 31, 1902 occur in the previous lunar year eclipse set, and the partial solar eclipse onJuly 21, 1906 occurs in the next lunar year eclipse set.
| Solar eclipse series sets from 1902 to 1906 | ||||||
|---|---|---|---|---|---|---|
| Descending node | Ascending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 108 | April 8, 1902 Partial | 1.5024 | 113 | October 1, 1902 | ||
| 118 | March 29, 1903 Annular | 0.8413 | 123 | September 21, 1903 Total | −0.8967 | |
| 128 | March 17, 1904 Annular | 0.1299 | 133 | September 9, 1904 Total | −0.1625 | |
| 138 | March 6, 1905 Annular | −0.5768 | 143 | August 30, 1905 Total | 0.5708 | |
| 148 | February 23, 1906 Partial | −1.2479 | 153 | August 20, 1906 Partial | 1.3731 | |
This eclipse is a part ofSaros series 128, repeating every 18 years, 11 days, and containing 73 events. The series started with a partial solar eclipse on August 29, 984 AD. It contains total eclipses from May 16, 1417 through June 18, 1471; hybrid eclipses from June 28, 1489 through July 31, 1543; and annular eclipses from August 11, 1561 through July 25, 2120. The series ends at member 73 as a partial eclipse on November 1, 2282. 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 totality was produced by member 27 at 1 minutes, 45 seconds on June 7, 1453, and the longest duration of annularity was produced by member 48 at 8 minutes, 35 seconds on February 1, 1832. All eclipses in this series occur at the Moon’sdescending node of orbit.[10]
| Series members 47–68 occur between 1801 and 2200: | ||
|---|---|---|
| 47 | 48 | 49 |
 January 21, 1814 |  February 1, 1832 |  February 12, 1850 |
| 50 | 51 | 52 |
 February 23, 1868 |  March 5, 1886 | March 17, 1904 |
| 53 | 54 | 55 |
 March 28, 1922 |  April 7, 1940 |  April 19, 1958 |
| 56 | 57 | 58 |
 April 29, 1976 |  May 10, 1994 |  May 20, 2012 |
| 59 | 60 | 61 |
 June 1, 2030 |  June 11, 2048 |  June 22, 2066 |
| 62 | 63 | 64 |
 July 3, 2084 |  July 15, 2102 |  July 25, 2120 |
| 65 | 66 | 67 |
 August 5, 2138 |  August 16, 2156 |  August 27, 2174 |
| 68 | ||
 September 6, 2192 | ||
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 16, 1866 and August 9, 1953 | ||||
|---|---|---|---|---|
| March 16–17 | January 1–3 | October 20–22 | August 9–10 | May 27–29 |
| 108 | 110 | 112 | 114 | 116 |
 March 16, 1866 |  August 9, 1877 |  May 27, 1881 | ||
| 118 | 120 | 122 | 124 | 126 |
 March 16, 1885 |  January 1, 1889 |  October 20, 1892 |  August 9, 1896 |  May 28, 1900 |
| 128 | 130 | 132 | 134 | 136 |
March 17, 1904 |  January 3, 1908 |  October 22, 1911 |  August 10, 1915 |  May 29, 1919 |
| 138 | 140 | 142 | 144 | 146 |
 March 17, 1923 |  January 3, 1927 |  October 21, 1930 |  August 10, 1934 |  May 29, 1938 |
| 148 | 150 | 152 | 154 | |
 March 16, 1942 |  January 3, 1946 |  October 21, 1949 |  August 9, 1953 | |
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 | ||||
|---|---|---|---|---|
 December 21, 1805 (Saros 119) |  November 19, 1816 (Saros 120) |  October 20, 1827 (Saros 121) |  September 18, 1838 (Saros 122) |  August 18, 1849 (Saros 123) |
 July 18, 1860 (Saros 124) |  June 18, 1871 (Saros 125) |  May 17, 1882 (Saros 126) |  April 16, 1893 (Saros 127) | March 17, 1904 (Saros 128) |
 February 14, 1915 (Saros 129) |  January 14, 1926 (Saros 130) |  December 13, 1936 (Saros 131) |  November 12, 1947 (Saros 132) |  October 12, 1958 (Saros 133) |
 September 11, 1969 (Saros 134) |  August 10, 1980 (Saros 135) |  July 11, 1991 (Saros 136) |  June 10, 2002 (Saros 137) |  May 10, 2013 (Saros 138) |
 April 8, 2024 (Saros 139) |  March 9, 2035 (Saros 140) |  February 5, 2046 (Saros 141) |  January 5, 2057 (Saros 142) |  December 6, 2067 (Saros 143) |
 November 4, 2078 (Saros 144) |  October 4, 2089 (Saros 145) |  September 4, 2100 (Saros 146) |  August 4, 2111 (Saros 147) |  July 4, 2122 (Saros 148) |
 June 3, 2133 (Saros 149) |  May 3, 2144 (Saros 150) |  April 2, 2155 (Saros 151) |  March 2, 2166 (Saros 152) |  January 29, 2177 (Saros 153) |
 December 29, 2187 (Saros 154) |  November 28, 2198 (Saros 155) | |||
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 | ||
|---|---|---|
 May 16, 1817 (Saros 125) |  April 25, 1846 (Saros 126) |  April 6, 1875 (Saros 127) |
March 17, 1904 (Saros 128) |  February 24, 1933 (Saros 129) |  February 5, 1962 (Saros 130) |
 January 15, 1991 (Saros 131) |  December 26, 2019 (Saros 132) |  December 5, 2048 (Saros 133) |
 November 15, 2077 (Saros 134) |  October 26, 2106 (Saros 135) |  October 7, 2135 (Saros 136) |
 September 16, 2164 (Saros 137) |  August 26, 2193 (Saros 138) | |
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