A partial solar eclipse will occur at the Moon's descending node of orbit between Monday, April 10 and Tuesday, April 11, 2051,[1] with a magnitude of 0.9849. 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 partial solar eclipse occurs in the polar regions of the Earth when the center of the Moon's shadow misses the Earth.
The umbral shadow of the Moon will pass just above the North Pole. It will be the largest partial solar eclipse in 21st century.[2]
The maximal phase of the partial eclipse (0.98) will be recorded in the Barents Sea. The partial solar eclipse will be visible for parts of Asia, Alaska, and western Canada.
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 | 2051 April 11 at 00:12:31.3 UTC | |
| Ecliptic Conjunction | 2051 April 11 at 02:00:30.3 UTC | |
| Greatest Eclipse | 2051 April 11 at 02:10:38.6 UTC | |
| Equatorial Conjunction | 2051 April 11 at 02:41:35.1 UTC | |
| Last Penumbral External Contact | 2051 April 11 at 04:08:32.1 UTC |
| Eclipse Magnitude | 0.98490 | |
| Eclipse Obscuration | 0.98811 | |
| Gamma | 1.01694 | |
| Sun Right Ascension | 01h18m13.3s | |
| Sun Declination | +08°15'12.8" | |
| Sun Semi-Diameter | 15'57.8" | |
| Sun Equatorial Horizontal Parallax | 08.8" | |
| Moon Right Ascension | 01h17m01.7s | |
| Moon Declination | +09°14'52.8" | |
| Moon Semi-Diameter | 16'42.8" | |
| Moon Equatorial Horizontal Parallax | 1°01'20.2" | |
| ΔT | 84.9 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.