A total solar eclipse occurred at the Moon's ascending node of orbit between Thursday, March 17 and Friday, March 18, 1988,[1] with a magnitude of 1.0464. 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. A total solar eclipse occurs when the Moon's apparent 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 only 1.1 days after perigee (on March 16, 1988, at 20:30 UTC), the Moon's apparent diameter was larger.[2]
Totality was visible in Indonesia and southern Philippines. A partial eclipse was visible for parts of South Asia, Southeast Asia, East Asia, Northeast Asia, Australia, and Alaska.
The tourism office of the General Santos City government in the Philippines promoted it as a big tourism event. Hordes of scientists, astronomers, journalists, TV crews and tourists from all over the globe observed the totality from there. Then President of the Philippines Corazon Aquino also joined in to experience the event.[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]
| First Penumbral External Contact | 1988 March 17 at 23:24:58.4 UTC | |
| First Umbral External Contact | 1988 March 18 at 00:23:32.6 UTC | |
| First Central Line | 1988 March 18 at 00:24:27.6 UTC | |
| First Umbral Internal Contact | 1988 March 18 at 00:25:22.6 UTC | |
| First Penumbral Internal Contact | 1988 March 18 at 01:38:59.5 UTC | |
| Greatest Duration | 1988 March 18 at 01:57:26.1 UTC | |
| Greatest Eclipse | 1988 March 18 at 01:58:56.4 UTC | |
| Ecliptic Conjunction | 1988 March 18 at 02:03:15.6 UTC | |
| Equatorial Conjunction | 1988 March 18 at 02:23:10.7 UTC | |
| Last Penumbral Internal Contact | 1988 March 18 at 02:18:20.1 UTC | |
| Last Umbral Internal Contact | 1988 March 18 at 03:32:16.8 UTC | |
| Last Central Line | 1988 March 18 at 03:33:10.6 UTC | |
| Last Umbral External Contact | 1988 March 18 at 03:34:04.3 UTC | |
| Last Penumbral External Contact | 1988 March 18 at 04:32:47.6 UTC |
| Eclipse Magnitude | 1.04640 | |
| Eclipse Obscuration | 1.09496 | |
| Gamma | 0.41879 | |
| Sun Right Ascension | 23h51m32.0s | |
| Sun Declination | -00°55'03.0" | |
| Sun Semi-Diameter | 16'04.1" | |
| Sun Equatorial Horizontal Parallax | 08.8" | |
| Moon Right Ascension | 23h50m42.6s | |
| Moon Declination | -00°32'52.0" | |
| Moon Semi-Diameter | 16'33.4" | |
| Moon Equatorial Horizontal Parallax | 1°00'45.8" | |
| ΔT | 55.9 s |
See also: Eclipse cycle. 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.
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