| Total eclipse | |
 Map | |
| Gamma | −0.4947 |
|---|---|
| Magnitude | 1.0524 |
| Maximum eclipse | |
| Duration | 311 s (5 min 11 s) |
| Coordinates | 6°12′S114°12′E / 6.2°S 114.2°E /-6.2; 114.2 |
| Max. width of band | 199 km (124 mi) |
| Times (UTC) | |
| Greatest eclipse | 4:43:33 |
| References | |
| Saros | 127 (56 of 82) |
| Catalog # (SE5000) | 9472 |
A totalsolar eclipse occurred at the Moon'sascending node of orbit on Saturday, June 11, 1983,[1] with amagnitude of 1.0524. 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 2.1 days beforeperigee (on June 13, 1983, at 6:50 UTC), the Moon's apparent diameter was larger.[2]
The path of totality went throughChristmas Island,Indonesia,Papua New Guinea, and terminated inVanuatu. The maximum eclipse occurred off the Indonesian island ofMadura. Major Indonesian cities witnessed totality, includingYogyakarta,Semarang,Surabaya, andMakassar, in addition toPort Moresby in Papua New Guinea. A partial eclipse was visible for parts ofMadagascar,Southeast Asia,Australia, and westernOceania.
To avoid blindness, Indonesian dictator presidentSuharto prohibited local people from observing the eclipse directly through then Information MinisterHarmoko, only allowing foreigners to observe from faraway places. Besides the requirements of closing and draping over all windows and airshafts, children were asked to hide themselves in cupboards and below desks as the eclipsing sun's rays were said to be more dangerous to children than to adults. They were allowed to watch a live broadcast of the eclipse occurring overBorobudur Temple inMagelang,Central Java, on state-owned TV channelTVRI. Because of the difference in restriction's intensity between regions, some locals did observe it.[3]
The Chinese Eclipse Observation Team formed byBeijing Astronomical Observatory (now incorporated into theNational Astronomical Observatories of China),Purple Mountain Observatory and Nanjing Astronomical Instrument Factory conducted observation in Port Moresby. Observation in Port Moresby was successful due to the cloudless weather during the eclipse, compared with the cloudy weather in Yogyakarta where teams from many countries went. The Chinese team didspectrum observations of thechromosphere andcorona, the broadband coronaluminosity andpolarization, and the coloured photography of the whole eclipse process.[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 | 1983 June 11 at 02:10:25.6 UTC |
| First Umbral External Contact | 1983 June 11 at 03:11:02.4 UTC |
| First Central Line | 1983 June 11 at 03:12:11.5 UTC |
| First Umbral Internal Contact | 1983 June 11 at 03:13:20.8 UTC |
| Equatorial Conjunction | 1983 June 11 at 04:34:18.1 UTC |
| Ecliptic Conjunction | 1983 June 11 at 04:38:24.4 UTC |
| Greatest Eclipse | 1983 June 11 at 04:43:33.5 UTC |
| Greatest Duration | 1983 June 11 at 04:47:29.5 UTC |
| Last Umbral Internal Contact | 1983 June 11 at 06:13:50.0 UTC |
| Last Central Line | 1983 June 11 at 06:15:01.3 UTC |
| Last Umbral External Contact | 1983 June 11 at 06:16:12.4 UTC |
| Last Penumbral External Contact | 1983 June 11 at 07:16:41.1 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.05240 |
| Eclipse Obscuration | 1.10755 |
| Gamma | −0.49475 |
| Sun Right Ascension | 05h15m15.1s |
| Sun Declination | +23°02'34.8" |
| Sun Semi-Diameter | 15'45.1" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 05h15m37.5s |
| Moon Declination | +22°33'26.4" |
| Moon Semi-Diameter | 16'20.3" |
| Moon Equatorial Horizontal Parallax | 0°59'57.8" |
| ΔT | 53.3 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.
| June 11 Ascending node (new moon) | June 25 Descending node (full moon) |
|---|---|
|  |
| Total solar eclipse Solar Saros 127 | Partial 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.[6]
The partial solar eclipses onJanuary 25, 1982 andJuly 20, 1982 occur in the previous lunar year eclipse set.
| Solar eclipse series sets from 1982 to 1985 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 117 | June 21, 1982 Partial | −1.2102 | 122 | December 15, 1982 Partial | 1.1293 | |
| 127 | June 11, 1983 Total | −0.4947 | 132 | December 4, 1983 Annular | 0.4015 | |
| 137 | May 30, 1984 Annular | 0.2755 | 142 Partial inGisborne, New Zealand | November 22, 1984 Total | −0.3132 | |
| 147 | May 19, 1985 Partial | 1.072 | 152 | November 12, 1985 Total | −0.9795 | |
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.[7]
| 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.
| 20 eclipse events between June 10, 1964 and August 21, 2036 | ||||
|---|---|---|---|---|
| June 10–11 | March 28–29 | January 14–16 | November 3 | August 21–22 |
| 117 | 119 | 121 | 123 | 125 |
 June 10, 1964 |  March 28, 1968 |  January 16, 1972 |  November 3, 1975 |  August 22, 1979 |
| 127 | 129 | 131 | 133 | 135 |
June 11, 1983 |  March 29, 1987 |  January 15, 1991 |  November 3, 1994 |  August 22, 1998 |
| 137 | 139 | 141 | 143 | 145 |
 June 10, 2002 |  March 29, 2006 |  January 15, 2010 |  November 3, 2013 |  August 21, 2017 |
| 147 | 149 | 151 | 153 | 155 |
 June 10, 2021 |  March 29, 2025 |  January 14, 2029 |  November 3, 2032 |  August 21, 2036 |
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 | ||
|---|---|---|
 October 9, 1809 (Saros 121) |  September 18, 1838 (Saros 122) |  August 29, 1867 (Saros 123) |
 August 9, 1896 (Saros 124) |  July 20, 1925 (Saros 125) |  June 30, 1954 (Saros 126) |
June 11, 1983 (Saros 127) |  May 20, 2012 (Saros 128) |  April 30, 2041 (Saros 129) |
 April 11, 2070 (Saros 130) |  March 21, 2099 (Saros 131) |  March 1, 2128 (Saros 132) |
 February 9, 2157 (Saros 133) |  January 20, 2186 (Saros 134) | |
Photos:
.jpg)
