A partial solar eclipse occurred at the Moon’s ascending node of orbit on Friday, November 25, 2011,[1] [2] [3] with a magnitude of 0.9047. 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.
This was the last of four partial solar eclipses in 2011, with the others occurring on January 4, June 1, and July 1.
This eclipse was visible across Antarctica in its summer 24-hour day sunlight, and New Zealand at sunset with less than 20% of the Sun obscured. Parts of the western Antarctic Peninsula experienced nearly 90% obscuration of the Sun, while South Africa and Tasmania experienced a very small partial eclipse.
Animated path
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 | 2011 November 25 at 04:24:22.8 UTC | |
| Ecliptic Conjunction | 2011 November 25 at 06:10:47.5 UTC | |
| Greatest Eclipse | 2011 November 25 at 06:21:24.5 UTC | |
| Equatorial Conjunction | 2011 November 25 at 06:32:28.3 UTC | |
| Last Penumbral External Contact | 2011 November 25 at 08:18:24.1 UTC |
| Eclipse Magnitude | 0.90468 | |
| Eclipse Obscuration | 0.88451 | |
| Gamma | −1.05359 | |
| Sun Right Ascension | 16h02m13.7s | |
| Sun Declination | -20°40'56.2" | |
| Sun Semi-Diameter | 16'12.1" | |
| Sun Equatorial Horizontal Parallax | 08.9" | |
| Moon Right Ascension | 16h01m46.2s | |
| Moon Declination | -21°44'25.4" | |
| Moon Semi-Diameter | 16'32.6" | |
| Moon Equatorial Horizontal Parallax | 1°00'42.7" | |
| ΔT | 66.5 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.
