| Type: | total |
| Date: | June 15, 2011 |
| Gamma: | 0.0897 |
| Magnitude: | 1.7014 |
| Saros Ser: | 130 |
| Saros No: | 34 of 72 |
| Totality: | 100 minutes, 13 seconds |
| Partiality: | 219 minutes, 17 seconds |
| Penumbral: | 336 minutes, 4 seconds |
| P1: | 17:24:37 |
| U1: | 18:22:57 |
| U2: | 19:22:29 |
| Greatest: | 20:12:36 |
| U3: | 21:02:42 |
| U4: | 22:02:14 |
| P4: | 23:00:41 |
| Previous: | December 2010 |
| Next: | December 2011 |
A total lunar eclipse occurred at the Moon’s ascending node of orbit on Wednesday, June 15, 2011,[1] with an umbral magnitude of 1.7014. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A total lunar eclipse occurs when the Moon's near side entirely passes into the Earth's umbral shadow. 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. A total lunar eclipse can last up to nearly two hours, while a total solar eclipse lasts only a few minutes at any given place, because the Moon's shadow is smaller. Occurring about 4.1 days after perigee (on June 11, 2011, at 21:40 UTC), the Moon's apparent diameter was larger.[2]
This was a relatively rare central lunar eclipse, where the Moon crossed the center of the Earth's shadow. The last time a lunar eclipse was closer to the center of the Earth's shadow was on July 16, 2000. The next central total lunar eclipse occurred on July 27, 2018.
The eclipse was completely visible over east Africa, Antarctica, and west, central, and south Asia, seen rising over Europe, west Africa, and South America and setting over east Asia and Australia.[3]
In western Asia, Australia, and the Philippines, the lunar eclipse was visible just before sunrise.[4] It was very visible in the clear and cloudless night sky throughout eastern and southeast Asia. Africa, far eastern Russia and Europe witnessed the whole event even in the late stages (as in partial lunar eclipse). The Americas (including North and northwestern South America) missed the eclipse completely (except in most areas) because it occurred at moonset.
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[5]
| Penumbral Magnitude | 2.68833 | |
| Umbral Magnitude | 1.70136 | |
| Gamma | 0.08968 | |
| Sun Right Ascension | 05h35m33.6s | |
| Sun Declination | +23°19'06.1" | |
| Sun Semi-Diameter | 15'44.7" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 17h35m32.3s | |
| Moon Declination | -23°13'51.6" | |
| Moon Semi-Diameter | 15'57.2" | |
| Moon Equatorial Horizontal Parallax | 0°58'33.0" | |
| 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. The first and last eclipse in this sequence is separated by one synodic month.
This eclipse is the center of nine lunar eclipses in a short-lived series. Each eclipse in the series repeats after one semester (6 lunations or 177 days) occurring at alternating nodes.
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros).[6] This lunar eclipse is related to two annular solar eclipses of Solar Saros 137.