| Annular eclipse | |
 Map | |
| Gamma | 0.2787 |
|---|---|
| Magnitude | 0.9634 |
| Maximum eclipse | |
| Duration | 229 s (3 min 49 s) |
| Coordinates | 14°18′N138°24′E / 14.3°N 138.4°E /14.3; 138.4 |
| Max. width of band | 137 km (85 mi) |
| Times (UTC) | |
| Greatest eclipse | 3:12:22 |
| References | |
| Saros | 134 (42 of 71) |
| Catalog # (SE5000) | 9481 |
An annularsolar eclipse occurred at the Moon'sdescending node of orbit on Wednesday, September 23, 1987,[1] with amagnitude of 0.9634. 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 only 5 days afterapogee (on September 18, 1987, at 4:00 UTC), the Moon's apparent diameter was smaller.[2]
Annularity was visible in theSoviet Union (today'sKazakhstan),China (includingShanghai), southwesternMongolia,Okinawa Islands ofJapan exceptKume Island and the southwestern tip ofKerama Islands, theFederal States of Micronesia,Papua New Guinea,Solomon Islands, Rotuma Islands ofFiji,Wallis Islands andWest Samoa (the name changed to Samoa later). A partial eclipse was visible for parts ofSouth Asia,Southeast Asia,East Asia,Australia,Oceania, andHawaii.
Five radio observation stations were present in China at the time of the eclipse, two of which were within the annularity, inÜrümqi andShanghai respectively. A partial solar eclipse was observed from the other three, including one inNanjing where the eclipse was close to annularity, and the rest two inBeijing andKunming. The Department of Mathematics and Physics of theChinese Academy of Sciences and the Chinese Astronomical Society held a meeting in Kunming in December 1986, deciding that on-site observation would be conducted at each station, among which theShanghai Astronomical Observatory was considered to have the best location with a larger magnitude of the eclipse, longer duration and largersolar zenith angle. The Shanghai Astronomical Observatory conducted observations with seven different wave bands using a 25-metre radio telescope.[3] TheYunnan Astronomical Observatory located in Kunming also conducted a multi-band joint observation of the partial solar eclipse.[4]
The Chinese Research Institute of Radio Wave Propagation conducted observations with a high-frequency skywave radar located inXinxiang on the southern limit of annularity. Uneven structure and motion were observed in theionosphere, the highest operating frequency was found changed during the eclipse, and large-scale fluctuations continued after the eclipse.[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 | 1987 September 23 at 00:15:50.5 UTC |
| First Umbral External Contact | 1987 September 23 at 01:20:19.5 UTC |
| First Central Line | 1987 September 23 at 01:22:07.2 UTC |
| First Umbral Internal Contact | 1987 September 23 at 01:23:55.0 UTC |
| First Penumbral Internal Contact | 1987 September 23 at 02:33:48.6 UTC |
| Greatest Duration | 1987 September 23 at 02:45:44.7 UTC |
| Equatorial Conjunction | 1987 September 23 at 02:54:28.0 UTC |
| Ecliptic Conjunction | 1987 September 23 at 03:09:08.4 UTC |
| Greatest Eclipse | 1987 September 23 at 03:12:21.6 UTC |
| Last Penumbral Internal Contact | 1987 September 23 at 03:51:20.8 UTC |
| Last Umbral Internal Contact | 1987 September 23 at 05:01:01.1 UTC |
| Last Central Line | 1987 September 23 at 05:02:46.3 UTC |
| Last Umbral External Contact | 1987 September 23 at 05:04:31.2 UTC |
| Last Penumbral External Contact | 1987 September 23 at 06:08:54.0 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 0.96337 |
| Eclipse Obscuration | 0.92807 |
| Gamma | 0.27869 |
| Sun Right Ascension | 11h58m25.1s |
| Sun Declination | +00°10'17.1" |
| Sun Semi-Diameter | 15'56.2" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 11h58m55.2s |
| Moon Declination | +00°23'45.5" |
| Moon Semi-Diameter | 15'07.6" |
| Moon Equatorial Horizontal Parallax | 0°55'30.9" |
| ΔT | 55.7 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.
| September 23 Descending node (new moon) | October 7 Ascending node (full moon) |
|---|---|
|  |
| Annular solar eclipse Solar Saros 134 | Penumbral lunar eclipse Lunar Saros 146 |
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]
| Solar eclipse series sets from 1986 to 1989 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 119 | April 9, 1986 Partial | −1.0822 | 124 | October 3, 1986 Hybrid | 0.9931 | |
| 129 | March 29, 1987 Hybrid | −0.3053 | 134 | September 23, 1987 Annular | 0.2787 | |
| 139 | March 18, 1988 Total | 0.4188 | 144 | September 11, 1988 Annular | −0.4681 | |
| 149 | March 7, 1989 Partial | 1.0981 | 154 | August 31, 1989 Partial | −1.1928 | |
This eclipse is a part ofSaros series 134, repeating every 18 years, 11 days, and containing 71 events. The series started with a partial solar eclipse on June 22, 1248. It contains total eclipses from October 9, 1428 through December 24, 1554; hybrid eclipses from January 3, 1573 through June 27, 1843; and annular eclipses from July 8, 1861 through May 21, 2384. The series ends at member 72 as a partial eclipse on August 6, 2510. 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 1 minutes, 30 seconds on October 9, 1428, and the longest duration of annularity will be produced by member 52 at 10 minutes, 55 seconds on January 10, 2168. All eclipses in this series occur at the Moon’sdescending node of orbit.[8]
| Series members 32–53 occur between 1801 and 2200: | ||
|---|---|---|
| 32 | 33 | 34 |
 June 6, 1807 |  June 16, 1825 |  June 27, 1843 |
| 35 | 36 | 37 |
 July 8, 1861 |  July 19, 1879 |  July 29, 1897 |
| 38 | 39 | 40 |
 August 10, 1915 |  August 21, 1933 |  September 1, 1951 |
| 41 | 42 | 43 |
 September 11, 1969 | September 23, 1987 |  October 3, 2005 |
| 44 | 45 | 46 |
 October 14, 2023 |  October 25, 2041 |  November 5, 2059 |
| 47 | 48 | 49 |
 November 15, 2077 |  November 27, 2095 |  December 8, 2113 |
| 50 | 51 | 52 |
 December 19, 2131 |  December 30, 2149 |  January 10, 2168 |
| 53 | ||
 January 20, 2186 | ||
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.
| 21 eclipse events between July 11, 1953 and July 11, 2029 | ||||
|---|---|---|---|---|
| July 10–11 | April 29–30 | February 15–16 | December 4 | September 21–23 |
| 116 | 118 | 120 | 122 | 124 |
 July 11, 1953 |  April 30, 1957 |  February 15, 1961 |  December 4, 1964 |  September 22, 1968 |
| 126 | 128 | 130 | 132 | 134 |
 July 10, 1972 |  April 29, 1976 |  February 16, 1980 |  December 4, 1983 | September 23, 1987 |
| 136 | 138 | 140 | 142 | 144 |
 July 11, 1991 |  April 29, 1995 |  February 16, 1999 |  December 4, 2002 |  September 22, 2006 |
| 146 | 148 | 150 | 152 | 154 |
 July 11, 2010 |  April 29, 2014 |  February 15, 2018 |  December 4, 2021 |  September 21, 2025 |
| 156 | ||||
 July 11, 2029 | ||||
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 4, 1802 (Saros 117) |  February 1, 1813 (Saros 118) |  January 1, 1824 (Saros 119) |  November 30, 1834 (Saros 120) |  October 30, 1845 (Saros 121) |
 September 29, 1856 (Saros 122) |  August 29, 1867 (Saros 123) |  July 29, 1878 (Saros 124) |  June 28, 1889 (Saros 125) |  May 28, 1900 (Saros 126) |
 April 28, 1911 (Saros 127) |  March 28, 1922 (Saros 128) |  February 24, 1933 (Saros 129) |  January 25, 1944 (Saros 130) |  December 25, 1954 (Saros 131) |
 November 23, 1965 (Saros 132) |  October 23, 1976 (Saros 133) | September 23, 1987 (Saros 134) |  August 22, 1998 (Saros 135) |  July 22, 2009 (Saros 136) |
 June 21, 2020 (Saros 137) |  May 21, 2031 (Saros 138) |  April 20, 2042 (Saros 139) |  March 20, 2053 (Saros 140) |  February 17, 2064 (Saros 141) |
 January 16, 2075 (Saros 142) |  December 16, 2085 (Saros 143) |  November 15, 2096 (Saros 144) |  October 16, 2107 (Saros 145) |  September 15, 2118 (Saros 146) |
 August 15, 2129 (Saros 147) |  July 14, 2140 (Saros 148) |  June 14, 2151 (Saros 149) |  May 14, 2162 (Saros 150) |  April 12, 2173 (Saros 151) |
 March 12, 2184 (Saros 152) |  February 10, 2195 (Saros 153) | |||
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 | ||
|---|---|---|
 January 21, 1814 (Saros 128) |  December 31, 1842 (Saros 129) |  December 12, 1871 (Saros 130) |
 November 22, 1900 (Saros 131) |  November 1, 1929 (Saros 132) |  October 12, 1958 (Saros 133) |
September 23, 1987 (Saros 134) |  September 1, 2016 (Saros 135) |  August 12, 2045 (Saros 136) |
 July 24, 2074 (Saros 137) |  July 4, 2103 (Saros 138) |  June 13, 2132 (Saros 139) |
 May 25, 2161 (Saros 140) |  May 4, 2190 (Saros 141) | |
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