A partial solar eclipse will occur at the Moon's descending node of orbit on Friday, July 3, 2065,[1] with a magnitude of 0.1638. 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 will be the second of four partial solar eclipses in 2065, with the others occurring on February 5, August 2, and December 27.
The partial solar eclipse will be visible for parts of Northern Europe and northern Russia.
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 | 2065 July 03 at 16:32:44.5 UTC | |
| Equatorial Conjunction | 2065 July 03 at 17:01:37.1 UTC | |
| Ecliptic Conjunction | 2065 July 03 at 17:17:29.5 UTC | |
| Greatest Eclipse | 2065 July 03 at 17:33:52.5 UTC | |
| Last Penumbral External Contact | 2065 July 03 at 18:35:10.0 UTC |
| Eclipse Magnitude | 0.16388 | |
| Eclipse Obscuration | 0.07678 | |
| Gamma | 1.46186 | |
| Sun Right Ascension | 06h53m43.9s | |
| Sun Declination | +22°51'26.7" | |
| Sun Semi-Diameter | 15'43.9" | |
| Sun Equatorial Horizontal Parallax | 08.6" | |
| Moon Right Ascension | 06h54m50.6s | |
| Moon Declination | +24°10'43.8" | |
| Moon Semi-Diameter | 15'05.3" | |
| Moon Equatorial Horizontal Parallax | 0°55'22.6" | |
| ΔT | 94.2 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.
The partial solar eclipses on January 1, 1805 (part of Saros 109) and November 21, 1862 (part of Saros 111) are also a part of this series but are not included in the table below.