A total solar eclipse will occur at the Moon's ascending node of orbit on Thursday, November 25, 2049,[1] with a magnitude of 1.0057. It is a hybrid event, with only a fraction of its path as total, and longer sections at the start and end as an annular eclipse. 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 3.2 days before perigee (on November 28, 2049, at 11:05 UTC), the Moon's apparent diameter will be larger.[2]
The path of the eclipse will be visible as an annular eclipse from parts of Saudi Arabia and Yemen before transitioning to a total eclipse. Totality will be visible from parts of Indonesia before the eclipse transforms back to an annular eclipse, then passing over Micronesia. A partial solar eclipse will also be visible for parts of East Africa, the Middle East, Central Asia, South Asia, Southeast Asia, and Australia.
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.[3]
| First Penumbral External Contact | 2049 November 25 at 02:49:44.1 UTC | |
| First Umbral External Contact | 2049 November 25 at 03:50:24.6 UTC | |
| First Central Line | 2049 November 25 at 03:50:45.7 UTC | |
| Greatest Duration | 2049 November 25 at 03:50:45.7 UTC | |
| First Umbral Internal Contact | 2049 November 25 at 03:51:06.8 UTC | |
| First Penumbral Internal Contact | 2049 November 25 at 04:57:11.0 UTC | |
| Equatorial Conjunction | 2049 November 25 at 05:30:50.7 UTC | |
| Greatest Eclipse | 2049 November 25 at 05:33:47.9 UTC | |
| Ecliptic Conjunction | 2049 November 25 at 05:36:57.1 UTC | |
| Last Penumbral Internal Contact | 2049 November 25 at 06:10:30.6 UTC | |
| Last Umbral Internal Contact | 2049 November 25 at 07:16:33.1 UTC | |
| Last Central Line | 2049 November 25 at 07:16:51.6 UTC | |
| Last Umbral External Contact | 2049 November 25 at 07:17:10.1 UTC | |
| Last Penumbral External Contact | 2049 November 25 at 08:17:47.4 UTC |
| Eclipse Magnitude | 1.00570 | |
| Eclipse Obscuration | 1.01144 | |
| Gamma | 0.29427 | |
| Sun Right Ascension | 16h05m24.9s | |
| Sun Declination | -20°49'25.8" | |
| Sun Semi-Diameter | 16'12.0" | |
| Sun Equatorial Horizontal Parallax | 08.9" | |
| Moon Right Ascension | 16h05m31.7s | |
| Moon Declination | -20°32'13.6" | |
| Moon Semi-Diameter | 16'02.3" | |
| Moon Equatorial Horizontal Parallax | 0°58'51.9" | |
| ΔT | 84.0 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.