An annular solar eclipse occurred at the Moon's ascending node of orbit on Sunday, June 28, 1908,[1] [2] [3] [4] with a magnitude of 0.9655. 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. Occurring about 4 days before apogee (on July 2, 1908, at 16:30 UTC), the Moon's apparent diameter was smaller.[5]
The annular eclipse was visible in North America, including a part of central Mexico around Mexico City; Orlando; and Daytona Beach, Florida in the United States. In Africa, it included Rosso, Mauritania, the northernmost part of Senegal, Bamako and the southwestern French Sudan (now Mali), the southwesternmost part of Upper Volta (now Burkina Faso) and northern British Gold Coast (now Ghana). A partial eclipse was visible for parts of northern South America, most of North America, the Caribbean, West Africa, North Africa, and Western Europe.
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]
| First Penumbral External Contact | 1908 June 28 at 13:29:11.1 UTC | |
| First Umbral External Contact | 1908 June 28 at 14:33:04.2 UTC | |
| First Central Line | 1908 June 28 at 14:34:43.5 UTC | |
| First Umbral Internal Contact | 1908 June 28 at 14:36:22.8 UTC | |
| First Penumbral Internal Contact | 1908 June 28 at 15:41:23.7 UTC | |
| Greatest Eclipse | 1908 June 28 at 16:29:51.0 UTC | |
| Equatorial Conjunction | 1908 June 28 at 16:30:40.3 UTC | |
| Ecliptic Conjunction | 1908 June 28 at 16:31:28.2 UTC | |
| Greatest Duration | 1908 June 28 at 16:37:12.6 UTC | |
| Last Penumbral Internal Contact | 1908 June 28 at 17:18:16.1 UTC | |
| Last Umbral Internal Contact | 1908 June 28 at 18:23:16.9 UTC | |
| Last Central Line | 1908 June 28 at 18:24:58.5 UTC | |
| Last Umbral External Contact | 1908 June 28 at 18:26:40.0 UTC | |
| Last Penumbral External Contact | 1908 June 28 at 19:30:35.4 UTC |
| Eclipse Magnitude | 0.96548 | |
| Eclipse Obscuration | 0.93215 | |
| Gamma | 0.13895 | |
| Sun Right Ascension | 06h28m25.7s | |
| Sun Declination | +23°17'24.0" | |
| Sun Semi-Diameter | 15'43.8" | |
| Sun Equatorial Horizontal Parallax | 08.6" | |
| Moon Right Ascension | 06h28m24.0s | |
| Moon Declination | +23°24'59.9" | |
| Moon Semi-Diameter | 14'57.6" | |
| Moon Equatorial Horizontal Parallax | 0°54'54.1" | |
| ΔT | 8.4 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. The first and last eclipse in this sequence is separated by one synodic month.