Solar eclipse of March 29, 1987
Template:Short description Script error: No such module "Solar eclipse". A total solar eclipse occurred at the Moon's ascending node of orbit on Sunday, March 29, 1987,[1] with a magnitude of 1.0013. It was a hybrid event, with only a fraction of its path as total, and longer sections at the start and end as an annular eclipse. The eclipse lasted a maximum of only 7.57 seconds. A solar eclipse occurs when the Moon passes between Earth and the Sun, thereby totally or partly obscuring the image of the Sun for a viewer on Earth. An annular solar eclipse occurs when the Moon's apparent diameter is smaller than the Sun's, blocking most of the Sun's light and causing the Sun to look like an annulus (ring). An annular eclipse appears as a partial eclipse over a region of the Earth thousands of kilometres wide. The Moon's apparent diameter was larger because it occurred 4.7 days after perigee (on March 24, 1987, at 19:00 UTC) and 7.8 days before apogee (on April 6, 1987, at 7:40 UTC).[2]
Totality of this eclipse was not visible on any land, while annularity was visible in southern Argentina, Gabon, Equatorial Guinea, Cameroon, Central African Republic, Sudan (part of the path of annularity crossed today's South Sudan), Ethiopia, Djibouti and Somaliland. A partial eclipse was visible for parts of southern and central South America, Antarctica, Africa, and the Middle East.
Eclipse details
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.[3]
| Event | Time (UTC) |
|---|---|
| First Penumbral External Contact | 1987 March 29 at 10:03:29.8 UTC |
| First Umbral External Contact | 1987 March 29 at 11:05:14.4 UTC |
| First Central Line | 1987 March 29 at 11:05:40.9 UTC |
| Greatest Duration | 1987 March 29 at 11:05:40.9 UTC |
| First Umbral Internal Contact | 1987 March 29 at 11:06:07.5 UTC |
| First Penumbral Internal Contact | 1987 March 29 at 12:14:03.2 UTC |
| Equatorial Conjunction | 1987 March 29 at 12:31:19.9 UTC |
| Ecliptic Conjunction | 1987 March 29 at 12:46:28.0 UTC |
| Greatest Eclipse | 1987 March 29 at 12:49:47.3 UTC |
| Last Penumbral Internal Contact | 1987 March 29 at 13:25:55.5 UTC |
| Last Umbral Internal Contact | 1987 March 29 at 14:33:36.4 UTC |
| Last Central Line | 1987 March 29 at 14:34:05.6 UTC |
| Last Umbral External Contact | 1987 March 29 at 14:34:34.9 UTC |
| Last Penumbral External Contact | 1987 March 29 at 15:36:18.1 UTC |
| Parameter | Value |
|---|---|
| Eclipse Magnitude | 1.00134 |
| Eclipse Obscuration | 1.00267 |
| Gamma | −0.30531 |
| Sun Right Ascension | 00h30m29.5s |
| Sun Declination | +03°17'32.1" |
| Sun Semi-Diameter | 16'01.1" |
| Sun Equatorial Horizontal Parallax | 08.8" |
| Moon Right Ascension | 00h31m03.7s |
| Moon Declination | +03°02'04.7" |
| Moon Semi-Diameter | 15'47.7" |
| Moon Equatorial Horizontal Parallax | 0°57'58.2" |
| ΔT | 55.4 s |
Eclipse season
Script error: No such module "Labelled list hatnote". This eclipse is part of an eclipse 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 a fortnight.
| March 29 Ascending node (new moon) |
April 14 Descending node (full moon) |
|---|---|
| File:SE1987Mar29H.png | File:Lunar eclipse chart close-1987Apr14.png |
| Hybrid solar eclipse Solar Saros 129 |
Penumbral lunar eclipse Lunar Saros 141 |
Related eclipses
Eclipses in 1987
- A hybrid solar eclipse on March 29.
- A penumbral lunar eclipse on April 14.
- An annular solar eclipse on September 23.
- A penumbral lunar eclipse on October 7.
Metonic
- Preceded by: Solar eclipse of June 11, 1983
- Followed by: Solar eclipse of January 15, 1991
Tzolkinex
- Preceded by: Solar eclipse of February 16, 1980
- Followed by: Solar eclipse of May 10, 1994
Half-Saros
- Preceded by: Lunar eclipse of March 24, 1978
- Followed by: Lunar eclipse of April 4, 1996
Tritos
- Preceded by: Solar eclipse of April 29, 1976
- Followed by: Solar eclipse of February 26, 1998
Solar Saros 129
- Preceded by: Solar eclipse of March 18, 1969
- Followed by: Solar eclipse of April 8, 2005
Inex
- Preceded by: Solar eclipse of April 19, 1958
- Followed by: Solar eclipse of March 9, 2016
Triad
- Preceded by: Solar eclipse of May 28, 1900
- Followed by: Solar eclipse of January 27, 2074
Solar eclipses of 1986–1989
This eclipse is a member of a semester series. An eclipse in a semester series of solar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[4]
| Solar eclipse series sets from 1986 to 1989 | ||||||
|---|---|---|---|---|---|---|
| Ascending node | Descending node | |||||
| Saros | Map | Gamma | Saros | Map | Gamma | |
| 119 | April 9, 1986 File:SE1986Apr09P.png Partial |
−1.0822 | 124 | October 3, 1986 File:SE1986Oct03H.png Hybrid |
0.9931 | |
| 129 | March 29, 1987 File:SE1987Mar29H.png Hybrid |
−0.3053 | 134 | September 23, 1987 File:SE1987Sep23A.png Annular |
0.2787 | |
| 139 | March 18, 1988 File:SE1988Mar18T.png Total |
0.4188 | 144 | September 11, 1988 File:SE1988Sep11A.png Annular |
−0.4681 | |
| 149 | March 7, 1989 File:SE1989Mar07P.png Partial |
1.0981 | 154 | August 31, 1989 File:SE1989Aug31P.png Partial |
−1.1928 | |
Saros 129
This eclipse is a part of Saros series 129, repeating every 18 years, 11 days, and containing 80 events. The series started with a partial solar eclipse on October 3, 1103. It contains annular eclipses from May 6, 1464 through March 18, 1969; hybrid eclipses from March 29, 1987 through April 20, 2023; and total eclipses from April 30, 2041 through July 26, 2185. The series ends at member 80 as a partial eclipse on February 21, 2528. Its eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
The longest duration of annularity was produced by member 34 at 5 minutes, 10 seconds on October 4, 1698, and the longest duration of totality will be produced by member 58 at 3 minutes, 43 seconds on June 25, 2131. All eclipses in this series occur at the Moon’s ascending node of orbit.[5]
Metonic series
The metonic 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 |
| File:SE1964Jun10P.png June 10, 1964 |
File:SE1968Mar28P.png March 28, 1968 |
File:SE1972Jan16A.png January 16, 1972 |
File:SE1975Nov03P.png November 3, 1975 |
File:SE1979Aug22A.png August 22, 1979 |
| 127 | 129 | 131 | 133 | 135 |
| File:SE1983Jun11T.png June 11, 1983 |
File:SE1987Mar29H.png March 29, 1987 |
File:SE1991Jan15A.png January 15, 1991 |
File:SE1994Nov03T.png November 3, 1994 |
File:SE1998Aug22A.png August 22, 1998 |
| 137 | 139 | 141 | 143 | 145 |
| File:SE2002Jun10A.png June 10, 2002 |
File:SE2006Mar29T.png March 29, 2006 |
File:SE2010Jan15A.png January 15, 2010 |
File:SE2013Nov03H.png November 3, 2013 |
File:SE2017Aug21T.png August 21, 2017 |
| 147 | 149 | 151 | 153 | 155 |
| File:SE2021Jun10A.png June 10, 2021 |
File:SE2025Mar29P.png March 29, 2025 |
File:SE2029Jan14P.png January 14, 2029 |
File:SE2032Nov03P.png November 3, 2032 |
File:SE2036Aug21P.png August 21, 2036 |
Tritos series
Template:Solar Tritos series 2009 January 26
Inex series
Template:Solar Inex series 2016 March 9
Notes
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References
- Earth visibility chart and eclipse statistics Eclipse Predictions by Fred Espenak, NASA/GSFC
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