| Type: | partial |
| Date: | April 25, 2013 |
| Gamma: | -1.0121 |
| Magnitude: | 0.0160 |
| Saros Ser: | 112 |
| Saros No: | 65 of 72 |
| Partiality: | 27 minutes, 0 seconds |
| Penumbral: | 247 minutes, 42 seconds |
| P1: | 18:03:41 |
| U1: | 19:54:04 |
| Greatest: | 20:07:29 |
| U4: | 20:21:04 |
| P4: | 22:11:23 |
| Previous: | November 2012 |
| Next: | May 2013 |
A partial lunar eclipse occurred at the Moon’s ascending node of orbit on Thursday, April 25, 2013,[1] with an umbral magnitude of 0.0160. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A partial lunar eclipse occurs when one part of the Moon is in the Earth's umbra, while the other part is in the Earth's penumbra. Unlike a solar eclipse, which can only be viewed from a relatively small area of the world, a lunar eclipse may be viewed from anywhere on the night side of Earth. Occurring about 1.8 days before perigee (on April 27, 2013, at 15:50 UTC), the Moon's apparent diameter was larger.[2]
Only a tiny sliver (1.48%) of the Moon was covered by the Earth's umbral shadow at maximum eclipse, but the entire northern half of the Moon was darkened from being inside the penumbral shadow. This was one of the shortest partial eclipses of the Moon in the 21st century, lasting 27 minutes. This was also the last of 58 umbral lunar eclipses in Lunar Saros 112.
The eclipse was completely visible over Africa, Europe, and Asia, seen rising over eastern South America and setting over Australia.[3]
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Penumbral Magnitude | 0.98783 | |
| Umbral Magnitude | 0.01596 | |
| Gamma | −1.01214 | |
| Sun Right Ascension | 02h13m51.3s | |
| Sun Declination | +13°26'35.0" | |
| Sun Semi-Diameter | 15'53.7" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 14h12m51.4s | |
| Moon Declination | -14°25'34.1" | |
| Moon Semi-Diameter | 16'21.4" | |
| Moon Equatorial Horizontal Parallax | 1°00'01.6" | |
| ΔT | 67.1 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 lunar year series repeats after 12 lunations or 354 days, shifting back by about 10 days in consecutive years. Because of the date shift, the Earth's shadow will be about 11 degrees west in sequential events.
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros).[5] This lunar eclipse is related to two partial solar eclipses of Solar Saros 119.