Top Qs
Timeline
Chat
Perspective
March 2006 lunar eclipse
Penumbral lunar eclipse 14 March 2006 From Wikipedia, the free encyclopedia
Remove ads
A penumbral lunar eclipse occurred at the Moon’s descending node of orbit on Tuesday, March 14, 2006,[1] with an umbral magnitude of −0.0584. It was a relatively rare total penumbral lunar eclipse, with the Moon passing entirely within the penumbral shadow without entering the darker umbral shadow. A lunar eclipse occurs when the Moon moves into the Earth's shadow, causing the Moon to be darkened. A penumbral lunar eclipse occurs when part or all of the Moon's near side passes into 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 2.2 days after apogee (on March 12, 2006, at 20:45 UTC), the Moon's apparent diameter was smaller.[2]
.jpg)
Remove ads
Remove ads
Visibility
The eclipse was completely visible much of Africa, eastern South America, Europe, and west Asia, seen rising over North and South America and setting over much of Asia and western Australia.[3]
 |
 Hourly motion shown right to left |
 The Moon's hourly motion across the Earth's shadow in the constellation of Virgo. |
 Visibility map | ||
Images
Eclipse details
Shown below is a table displaying details about this particular lunar eclipse. It describes various parameters pertaining to this eclipse.[4]
Eclipse season
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.
Remove ads
Related eclipses
Summarize
Perspective
Eclipses in 2006
- A penumbral lunar eclipse on March 14.
- A total solar eclipse on March 29.
- A partial lunar eclipse on September 7.
- An annular solar eclipse on September 22.
Metonic
- Preceded by: Lunar eclipse of May 26, 2002
- Followed by: Lunar eclipse of December 31, 2009
Tzolkinex
- Preceded by: Lunar eclipse of January 31, 1999
- Followed by: Lunar eclipse of April 25, 2013
Half-Saros
- Preceded by: Solar eclipse of March 9, 1997
- Followed by: Solar eclipse of March 20, 2015
Tritos
- Preceded by: Lunar eclipse of April 15, 1995
- Followed by: Lunar eclipse of February 11, 2017
Lunar Saros 113
- Preceded by: Lunar eclipse of March 3, 1988
- Followed by: Lunar eclipse of March 25, 2024
Inex
- Preceded by: Lunar eclipse of April 4, 1977
- Followed by: Lunar eclipse of February 22, 2035
Triad
- Preceded by: Lunar eclipse of May 15, 1919
- Followed by: Lunar eclipse of January 12, 2093
Lunar eclipses of 2006–2009
This eclipse is a member of a semester series. An eclipse in a semester series of lunar eclipses repeats approximately every 177 days and 4 hours (a semester) at alternating nodes of the Moon's orbit.[5]
The lunar eclipses on July 7, 2009 (penumbral) and December 31, 2009 (partial) occur in the next lunar year eclipse set.
Metonic series
The Metonic cycle repeats nearly exactly every 19 years and represents a Saros cycle plus one lunar year. Because it occurs on the same calendar date, the Earth's shadow will in nearly the same location relative to the background stars.
|
|
 |
Saros 113
This eclipse is a part of Saros series 113, repeating every 18 years, 11 days, and containing 71 events. The series started with a penumbral lunar eclipse on April 29, 888 AD. It contains partial eclipses from July 14, 1014 through March 10, 1411; total eclipses from March 20, 1429 through August 7, 1645; and a second set of partial eclipses from August 18, 1663 through February 21, 1970. The series ends at member 71 as a penumbral eclipse on June 10, 2150.
The longest duration of totality was produced by member 38 at 103 minutes, 6 seconds on June 5, 1555. All eclipses in this series occur at the Moon’s descending node of orbit.[6]
Eclipses are tabulated in three columns; every third eclipse in the same column is one exeligmos apart, so they all cast shadows over approximately the same parts of the Earth.
Tritos series
This eclipse is a part of a tritos cycle, repeating at alternating nodes every 135 synodic months (≈ 3986.63 days, or 11 years minus 1 month). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee), but groupings of 3 tritos cycles (≈ 33 years minus 3 months) come close (≈ 434.044 anomalistic months), so eclipses are similar in these groupings.
Inex series
This eclipse is a part of the long period inex cycle, repeating at alternating nodes, every 358 synodic months (≈ 10,571.95 days, or 29 years minus 20 days). Their appearance and longitude are irregular due to a lack of synchronization with the anomalistic month (period of perigee). However, groupings of 3 inex cycles (≈ 87 years minus 2 months) comes close (≈ 1,151.02 anomalistic months), so eclipses are similar in these groupings.
Half-Saros cycle
A lunar eclipse will be preceded and followed by solar eclipses by 9 years and 5.5 days (a half saros).[8] This lunar eclipse is related to two total solar eclipses of Solar Saros 120.
| March 9, 1997 | March 20, 2015 |
|---|---|
 |
 |
Remove ads
See also
Notes
External links
Wikiwand - on
Seamless Wikipedia browsing. On steroids.
Remove ads