| Total eclipse | |
 Map | |
| Gamma | −0.2887 |
|---|---|
| Magnitude | 1.0562 |
| Maximum eclipse | |
| Duration | 307 s (5 min 7 s) |
| Coordinates | 1°36′N92°42′E / 1.6°N 92.7°E /1.6; 92.7 |
| Max. width of band | 193 km (120 mi) |
| Times (UTC) | |
| Greatest eclipse | 6:10:34 |
| References | |
| Saros | 127 (53 of 82) |
| Catalog # (SE5000) | 9349 |
A totalsolar eclipse occurred at the Moon'sascending node of orbit on Thursday, May 9, 1929,[1] with amagnitude of 1.0562. 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 1.7 days beforeperigee (on May 10, 1929, at 21:00 UTC), the Moon's apparent diameter was larger.[2]
Totality was visible fromDutch East Indies (today'sIndonesia),Federated Malay States (now belonging toMalaysia),Siam (name changed to Thailand later),French Indochina (the part now belonging toVietnam),Spratly Islands,Philippines, andSouth Seas Mandate inJapan (the part now belonging toFS Micronesia). A partial eclipse was visible for parts ofSoutheast Africa,South Asia,Southeast Asia,East Asia, andAustralia..
A team of British and German scientists observed the total eclipse inPattani province in southern Siam. KingRama VII and QueenRambai Barni also visited the observation camp set up by foreign scientists and observed the eclipse together in Pattani. This was the last time that Siam (Thailand) received a large-scale solar eclipse observation team so far. The other teams Thailand received later, including the American team for the totalsolar eclipse of June 20, 1955 were much smaller.[3]
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.[4]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1929 May 9 at 03:32:58.0 UTC |
| First Umbral External Contact | 1929 May 9 at 04:29:32.5 UTC |
| First Central Line | 1929 May 9 at 04:30:38.2 UTC |
| First Umbral Internal Contact | 1929 May 9 at 04:31:43.9 UTC |
| First Penumbral Internal Contact | 1929 May 9 at 05:32:55.2 UTC |
| Equatorial Conjunction | 1929 May 9 at 05:58:29.8 UTC |
| Ecliptic Conjunction | 1929 May 9 at 06:07:34.8 UTC |
| Greatest Eclipse | 1929 May 9 at 06:10:34.1 UTC |
| Greatest Duration | 1929 May 9 at 06:17:47.1 UTC |
| Last Penumbral Internal Contact | 1929 May 9 at 06:48:30.3 UTC |
| Last Umbral Internal Contact | 1929 May 9 at 07:49:29.9 UTC |
| Last Central Line | 1929 May 9 at 07:50:37.4 UTC |
| Last Umbral External Contact | 1929 May 9 at 07:51:44.7 UTC |
| Last Penumbral External Contact | 1929 May 9 at 08:48:11.5 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.05622 |
| Eclipse Obscuration | 1.11560 |
| Gamma | −0.28869 |
| Sun Right Ascension | 03h02m38.7s |
| Sun Declination | +17°14'10.1" |
| Sun Semi-Diameter | 15'50.3" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 03h03m05.7s |
| Moon Declination | +16°58'00.8" |
| Moon Semi-Diameter | 16'27.7" |
| Moon Equatorial Horizontal Parallax | 1°00'24.9" |
| ΔT | 24.0 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.
| May 9 Ascending node (new moon) | May 23 Descending node (full moon) |
|---|---|
|  |
| Total solar eclipse Solar Saros 127 | Penumbral lunar eclipse Lunar Saros 139 |
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.[5]
The partial solar eclipse onJune 17, 1928 occurs in the previous lunar year eclipse set, and the partial solar eclipse onSeptember 12, 1931 occurs in the next lunar year eclipse set.
| Solar eclipse series sets from 1928 to 1931 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 117 | May 19, 1928 Total (non-central) | 1.0048 | 122 | November 12, 1928 Partial | 1.0861 | |
| 127 | May 9, 1929 Total | −0.2887 | 132 | November 1, 1929 Annular | 0.3514 | |
| 137 | April 28, 1930 Hybrid | 0.473 | 142 | October 21, 1930 Total | −0.3804 | |
| 147 | April 18, 1931 Partial | 1.2643 | 152 | October 11, 1931 Partial | −1.0607 | |
This eclipse is a part ofSaros series 127, repeating every 18 years, 11 days, and containing 82 events. The series started with a partial solar eclipse on October 10, 991 AD. It contains total eclipses from May 14, 1352 throughAugust 15, 2091. There are no annular or hybrid eclipses in this set. The series ends at member 82 as a partial eclipse on March 21, 2452. 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 31 at 5 minutes, 40 seconds on August 30, 1532. All eclipses in this series occur at the Moon’sascending node of orbit.[6]
| Series members 46–68 occur between 1801 and 2200: | ||
|---|---|---|
| 46 | 47 | 48 |
 February 21, 1803 |  March 4, 1821 |  March 15, 1839 |
| 49 | 50 | 51 |
 March 25, 1857 |  April 6, 1875 |  April 16, 1893 |
| 52 | 53 | 54 |
 April 28, 1911 | May 9, 1929 |  May 20, 1947 |
| 55 | 56 | 57 |
 May 30, 1965 |  June 11, 1983 |  June 21, 2001 |
| 58 | 59 | 60 |
 July 2, 2019 |  July 13, 2037 |  July 24, 2055 |
| 61 | 62 | 63 |
 August 3, 2073 |  August 15, 2091 |  August 26, 2109 |
| 64 | 65 | 66 |
 September 6, 2127 |  September 16, 2145 |  September 28, 2163 |
| 67 | 68 | |
 October 8, 2181 |  October 19, 2199 | |
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 ascending node.
| 22 eclipse events between December 13, 1898 and July 20, 1982 | ||||
|---|---|---|---|---|
| December 13–14 | October 1–2 | July 20–21 | May 9 | February 24–25 |
| 111 | 113 | 115 | 117 | 119 |
 December 13, 1898 |  July 21, 1906 |  May 9, 1910 |  February 25, 1914 | |
| 121 | 123 | 125 | 127 | 129 |
 December 14, 1917 |  October 1, 1921 |  July 20, 1925 | May 9, 1929 |  February 24, 1933 |
| 131 | 133 | 135 | 137 | 139 |
 December 13, 1936 |  October 1, 1940 |  July 20, 1944 |  May 9, 1948 |  February 25, 1952 |
| 141 | 143 | 145 | 147 | 149 |
 December 14, 1955 |  October 2, 1959 |  July 20, 1963 |  May 9, 1967 |  February 25, 1971 |
| 151 | 153 | 155 | ||
 December 13, 1974 |  October 2, 1978 |  July 20, 1982 | ||
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 | ||||
|---|---|---|---|---|
 April 14, 1809 (Saros 116) |  March 14, 1820 (Saros 117) |  February 12, 1831 (Saros 118) |  January 11, 1842 (Saros 119) |  December 11, 1852 (Saros 120) |
 November 11, 1863 (Saros 121) |  October 10, 1874 (Saros 122) |  September 8, 1885 (Saros 123) |  August 9, 1896 (Saros 124) |  July 10, 1907 (Saros 125) |
 June 8, 1918 (Saros 126) | May 9, 1929 (Saros 127) |  April 7, 1940 (Saros 128) |  March 7, 1951 (Saros 129) |  February 5, 1962 (Saros 130) |
 January 4, 1973 (Saros 131) |  December 4, 1983 (Saros 132) |  November 3, 1994 (Saros 133) |  October 3, 2005 (Saros 134) |  September 1, 2016 (Saros 135) |
 August 2, 2027 (Saros 136) |  July 2, 2038 (Saros 137) |  May 31, 2049 (Saros 138) |  April 30, 2060 (Saros 139) |  March 31, 2071 (Saros 140) |
 February 27, 2082 (Saros 141) |  January 27, 2093 (Saros 142) |  December 29, 2103 (Saros 143) |  November 27, 2114 (Saros 144) |  October 26, 2125 (Saros 145) |
 September 26, 2136 (Saros 146) |  August 26, 2147 (Saros 147) |  July 25, 2158 (Saros 148) |  June 25, 2169 (Saros 149) |  May 24, 2180 (Saros 150) |
 April 23, 2191 (Saros 151) | ||||
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 | ||
|---|---|---|
 July 27, 1813 (Saros 123) |  July 8, 1842 (Saros 124) |  June 18, 1871 (Saros 125) |
 May 28, 1900 (Saros 126) | May 9, 1929 (Saros 127) |  April 19, 1958 (Saros 128) |
 March 29, 1987 (Saros 129) |  March 9, 2016 (Saros 130) |  February 16, 2045 (Saros 131) |
 January 27, 2074 (Saros 132) |  January 8, 2103 (Saros 133) |  December 19, 2131 (Saros 134) |
 November 27, 2160 (Saros 135) |  November 8, 2189 (Saros 136) | |
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