A partial solar eclipse will occur at the Moon's ascending node of orbit between Tuesday, September 1 and Wednesday, September 2, 2054,[1] with a magnitude of 0.9793. 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 partial solar eclipse will be visible for parts of Northeast Asia, Alaska, western Canada, and the western United States. This is the last of the first set of partial eclipses in Solar Saros 155.
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.[2]
| First Penumbral External Contact | 2054 September 01 at 23:12:21.2 UTC | |
| Equatorial Conjunction | 2054 September 02 at 00:38:15.2 UTC | |
| Greatest Eclipse | 2054 September 02 at 01:09:33.7 UTC | |
| Ecliptic Conjunction | 2054 September 02 at 01:19:46.2 UTC | |
| Last Penumbral External Contact | 2054 September 02 at 03:07:02.1 UTC |
| Eclipse Magnitude | 0.97932 | |
| Eclipse Obscuration | 0.98275 | |
| Gamma | 1.02148 | |
| Sun Right Ascension | 10h45m28.2s | |
| Sun Declination | +07°52'58.6" | |
| Sun Semi-Diameter | 15'50.9" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 10h46m40.4s | |
| Moon Declination | +08°52'49.8" | |
| Moon Semi-Diameter | 16'42.0" | |
| Moon Equatorial Horizontal Parallax | 1°01'17.5" | |
| ΔT | 86.9 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. The first and last eclipse in this sequence is separated by one synodic month.
