| Type: | partial |
| Date: | September 7, 2006 |
| Gamma: | −0.9262 |
| Magnitude: | 0.1837 |
| Saros Ser: | 118 |
| Saros No: | 51 of 74 |
| Partiality: | 91 minutes, 6 seconds |
| Penumbral: | 254 minutes, 23 seconds |
| P1: | 16:44:07 |
| U1: | 18:05:47 |
| Greatest: | 18:51:19 |
| U4: | 19:36:53 |
| P4: | 20:58:30 |
| Previous: | March 2006 |
| Next: | March 2007 |
A partial lunar eclipse occurred at the Moon’s ascending node of orbit on Thursday, September 7, 2006,[1] with an umbral magnitude of 0.1837. 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 only about 4 hours before perigee (on September 7, 2006, at 23:00 UTC), the Moon's apparent diameter was larger.[2]
The eclipse was completely visible over Asia, east Africa, eastern Europe and western Australia, seen rising over west Africa and western Europe and setting over eastern Australia and the western Pacific Ocean.[3]
Degania A, Israel
Shown below is a table displaying details about this particular solar eclipse. It describes various parameters pertaining to this eclipse.[4]
| Penumbral Magnitude | 1.13488 | |
| Umbral Magnitude | 0.18568 | |
| Gamma | −0.92619 | |
| Sun Right Ascension | 11h04m47.1s | |
| Sun Declination | +05°54'23.1" | |
| Sun Semi-Diameter | 15'52.4" | |
| Sun Equatorial Horizontal Parallax | 08.7" | |
| Moon Right Ascension | 23h06m35.6s | |
| Moon Declination | -06°44'25.6" | |
| Moon Semi-Diameter | 16'43.3" | |
| Moon Equatorial Horizontal Parallax | 1°01'22.3" | |
| ΔT | 65.1 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.
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 125.
