A total solar eclipse will occur at the Moon's ascending node of orbit on Saturday, May 11, 2097,[1] with a magnitude of 1.0538. 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 about 1.3 days before perigee (on May 13, 2097, at 1:30 UTC), the Moon's apparent diameter will be larger.[2]
The path of totality will be visible from parts of Alaska, Svalbard, eastern Norway, and northwestern Russia. A partial solar eclipse will also be visible for parts of Hawaii, northern Russia, Canada, the northwestern United States, Greenland, and Northern 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.[3]
| First Penumbral External Contact | 2097 May 11 at 16:21:50.6 UTC | |
| First Umbral External Contact | 2097 May 11 at 17:38:00.1 UTC | |
| First Central Line | 2097 May 11 at 17:40:15.9 UTC | |
| First Umbral Internal Contact | 2097 May 11 at 17:42:36.0 UTC | |
| Greatest Eclipse | 2097 May 11 at 18:34:31.4 UTC | |
| Greatest Duration | 2097 May 11 at 18:35:50.5 UTC | |
| Ecliptic Conjunction | 2097 May 11 at 18:43:07.3 UTC | |
| Equatorial Conjunction | 2097 May 11 at 19:07:38.5 UTC | |
| Last Umbral Internal Contact | 2097 May 11 at 19:26:03.9 UTC | |
| Last Central Line | 2097 May 11 at 19:28:25.7 UTC | |
| Last Umbral External Contact | 2097 May 11 at 19:30:43.3 UTC | |
| Last Penumbral External Contact | 2097 May 11 at 20:46:55.7 UTC |
| Eclipse Magnitude | 1.05381 | |
| Eclipse Obscuration | 1.11052 | |
| Gamma | 0.85156 | |
| Sun Right Ascension | 03h17m49.7s | |
| Sun Declination | +18°13'35.1" | |
| Sun Semi-Diameter | 15'50.2" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 03h16m33.2s | |
| Moon Declination | +19°01'53.1" | |
| Moon Semi-Diameter | 16'32.8" | |
| Moon Equatorial Horizontal Parallax | 1°00'43.7" | |
| ΔT | 121.0 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.