| Annular eclipse | |
 Map | |
| Gamma | 0.2755 |
|---|---|
| Magnitude | 0.998 |
| Maximum eclipse | |
| Duration | 11 s (0 min 11 s) |
| Coordinates | 37°30′N76°42′W / 37.5°N 76.7°W /37.5; -76.7 |
| Max. width of band | 7 km (4.3 mi) |
| Times (UTC) | |
| Greatest eclipse | 16:45:41 |
| References | |
| Saros | 137 (34 of 70) |
| Catalog # (SE5000) | 9474 |
An annularsolar eclipse occurred at the Moon'sascending node of orbit on Wednesday, May 30, 1984,[1] with amagnitude of 0.998. 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). The Moon's apparent diameter was near the average diameter because it occurred 6.6 days afterapogee (on May 24, 1984, at 2:00 UTC) and 7.8 days beforeperigee (on June 7, 1984, at 12:20 UTC).[2]
This was the first annularsolar eclipse visible in theUnited States in33 years.
Annularity was visible inMexico,Louisiana,Mississippi,Alabama,Georgia,South Carolina,North Carolina andVirginia in theUnited States, theAzores Islands,Morocco andAlgeria. A partial eclipse was visible for parts ofHawaii,North America,Central America, theCaribbean, northernSouth America,Western Europe, andNorthwest Africa.
During this eclipse, the apex of the Moon's umbral cone was very close to the Earth's surface, and the magnitude was very large. The edges of the Moon and the Sun were very close to each other as seen from the Earth. Images of thechromosphere andBaily's beads on thelunar limb, which are usually only visible during a total solar eclipse, could also be taken. A team of theUniversity of Florida took images, about half of which being those of the chromosphere and the other half thephotosphere, inGreenville, South Carolina.[3][4]Jay Pasachoff led a team fromWilliams College,Massachusetts toPicayune, Mississippi.[5]
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.[6]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1984 May 30 at 13:55:14.3 UTC |
| First Umbral External Contact | 1984 May 30 at 14:57:46.9 UTC |
| First Central Line | 1984 May 30 at 14:58:22.6 UTC |
| Greatest Duration | 1984 May 30 at 14:58:22.6 UTC |
| First Umbral Internal Contact | 1984 May 30 at 14:58:58.3 UTC |
| First Penumbral Internal Contact | 1984 May 30 at 16:06:12.7 UTC |
| Greatest Eclipse | 1984 May 30 at 16:45:41.5 UTC |
| Ecliptic Conjunction | 1984 May 30 at 16:48:44.8 UTC |
| Equatorial Conjunction | 1984 May 30 at 16:53:32.9 UTC |
| Last Penumbral Internal Contact | 1984 May 30 at 17:25:00.1 UTC |
| Last Umbral Internal Contact | 1984 May 30 at 18:32:21.8 UTC |
| Last Central Line | 1984 May 30 at 18:32:54.6 UTC |
| Last Umbral External Contact | 1984 May 30 at 18:33:27.3 UTC |
| Last Penumbral External Contact | 1984 May 30 at 19:35:58.9 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.99801 |
| Eclipse Obscuration | 0.99602 |
| Gamma | 0.27552 |
| Sun Right Ascension | 04h31m02.1s |
| Sun Declination | +21°52'05.5" |
| Sun Semi-Diameter | 15'46.4" |
| Sun Equatorial Horizontal Parallax | 08.7" |
| Moon Right Ascension | 04h30m45.4s |
| Moon Declination | +22°07'14.4" |
| Moon Semi-Diameter | 15'30.3" |
| Moon Equatorial Horizontal Parallax | 0°56'54.1" |
| ΔT | 54.0 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. The first and last eclipse in this sequence is separated by onesynodic month.
| May 15 Descending node (full moon) | May 30 Ascending node (new moon) | June 13 Descending node (full moon) |
|---|---|---|
 | |  |
| Penumbral lunar eclipse Lunar Saros 111 | Annular solar eclipse Solar Saros 137 | Penumbral lunar eclipse Lunar Saros 149 |
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.[7]
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 137, repeating every 18 years, 11 days, and containing 70 events. The series started with a partial solar eclipse on May 25, 1389. It contains total eclipses from August 20, 1533 through December 6, 1695; the first set of hybrid eclipses from December 17, 1713 through February 11, 1804; the first set of annular eclipses from February 21, 1822 through March 25, 1876; the second set of hybrid eclipses from April 6, 1894 throughApril 28, 1930; and the second set of annular eclipses fromMay 9, 1948 through April 13, 2507. The series ends at member 70 as a partial eclipse on June 28, 2633. 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 11 at 2 minutes, 55 seconds on September 10, 1569, and the longest duration of annularity will be produced by member 59 at 7 minutes, 5 seconds on February 28, 2435. All eclipses in this series occur at the Moon’sascending node of orbit.[8]
| Series members 24–46 occur between 1801 and 2200: | ||
|---|---|---|
| 24 | 25 | 26 |
 February 11, 1804 |  February 21, 1822 |  March 4, 1840 |
| 27 | 28 | 29 |
 March 15, 1858 |  March 25, 1876 |  April 6, 1894 |
| 30 | 31 | 32 |
 April 17, 1912 |  April 28, 1930 |  May 9, 1948 |
| 33 | 34 | 35 |
 May 20, 1966 | May 30, 1984 |  June 10, 2002 |
| 36 | 37 | 38 |
 June 21, 2020 |  July 2, 2038 |  July 12, 2056 |
| 39 | 40 | 41 |
 July 24, 2074 |  August 3, 2092 |  August 15, 2110 |
| 42 | 43 | 44 |
 August 25, 2128 |  September 6, 2146 |  September 16, 2164 |
| 45 | 46 | |
 September 27, 2182 |  October 9, 2200 | |
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 January 5, 1935 and August 11, 2018 | ||||
|---|---|---|---|---|
| January 4–5 | October 23–24 | August 10–12 | May 30–31 | March 18–19 |
| 111 | 113 | 115 | 117 | 119 |
 January 5, 1935 |  August 12, 1942 |  May 30, 1946 |  March 18, 1950 | |
| 121 | 123 | 125 | 127 | 129 |
 January 5, 1954 |  October 23, 1957 |  August 11, 1961 |  May 30, 1965 |  March 18, 1969 |
| 131 | 133 | 135 | 137 | 139 |
 January 4, 1973 |  October 23, 1976 |  August 10, 1980 | May 30, 1984 |  March 18, 1988 |
| 141 | 143 | 145 | 147 | 149 |
 January 4, 1992 |  October 24, 1995 |  August 11, 1999 |  May 31, 2003 |  March 19, 2007 |
| 151 | 153 | 155 | ||
 January 4, 2011 |  October 23, 2014 |  August 11, 2018 | ||
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 9, 1809 (Saros 121) |  September 7, 1820 (Saros 122) |  August 7, 1831 (Saros 123) |  July 8, 1842 (Saros 124) |  June 6, 1853 (Saros 125) |
 May 6, 1864 (Saros 126) |  April 6, 1875 (Saros 127) |  March 5, 1886 (Saros 128) |  February 1, 1897 (Saros 129) |  January 3, 1908 (Saros 130) |
 December 3, 1918 (Saros 131) |  November 1, 1929 (Saros 132) |  October 1, 1940 (Saros 133) |  September 1, 1951 (Saros 134) |  July 31, 1962 (Saros 135) |
 June 30, 1973 (Saros 136) | May 30, 1984 (Saros 137) |  April 29, 1995 (Saros 138) |  March 29, 2006 (Saros 139) |  February 26, 2017 (Saros 140) |
 January 26, 2028 (Saros 141) |  December 26, 2038 (Saros 142) |  November 25, 2049 (Saros 143) |  October 24, 2060 (Saros 144) |  September 23, 2071 (Saros 145) |
 August 24, 2082 (Saros 146) |  July 23, 2093 (Saros 147) |  June 22, 2104 (Saros 148) |  May 24, 2115 (Saros 149) |  April 22, 2126 (Saros 150) |
 March 21, 2137 (Saros 151) |  February 19, 2148 (Saros 152) |  January 19, 2159 (Saros 153) |  December 18, 2169 (Saros 154) |  November 17, 2180 (Saros 155) |
 October 18, 2191 (Saros 156) | ||||
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 28, 1810 (Saros 131) |  September 7, 1839 (Saros 132) |  August 18, 1868 (Saros 133) |
 July 29, 1897 (Saros 134) |  July 9, 1926 (Saros 135) |  June 20, 1955 (Saros 136) |
May 30, 1984 (Saros 137) |  May 10, 2013 (Saros 138) |  April 20, 2042 (Saros 139) |
 March 31, 2071 (Saros 140) |  March 10, 2100 (Saros 141) |  February 18, 2129 (Saros 142) |
 January 30, 2158 (Saros 143) |  January 9, 2187 (Saros 144) | |
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