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October 2005 lunar eclipse
Partial lunar eclipse 17 October 2005 From Wikipedia, the free encyclopedia
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A partial lunar eclipse occurred at the Moon’s ascending node of orbit on Monday, October 17, 2005,[1] with an umbral magnitude of 0.0645. 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 3.1 days before perigee (on October 14, 2005, at 10:00 UTC), the Moon's apparent diameter was larger.[2]
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Visibility
The eclipse was completely visible much of Australia, east Asia, and western North America, seen rising over much of Asia and setting over much of North America and western South America.[3]
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 Hourly motion shown right to left |
 The Moon's hourly motion across the Earth's shadow in the constellation of Pisces. |
 Visibility map | ||
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Akita City, Japan, 12:21 UTC
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Eclipse details
Shown below is a table displaying details about this particular lunar eclipse. It describes various parameters pertaining to this eclipse.[4]
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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.
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Related eclipses
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Eclipses in 2005
- A hybrid solar eclipse on April 8.
- A penumbral lunar eclipse on April 24.
- An annular solar eclipse on October 3.
- A partial lunar eclipse on October 17.
Metonic
- Preceded by: Lunar eclipse of December 30, 2001
- Followed by: Lunar eclipse of August 6, 2009
Tzolkinex
- Preceded by: Lunar eclipse of September 6, 1998
- Followed by: Lunar eclipse of November 28, 2012
Half-Saros
- Preceded by: Solar eclipse of October 12, 1996
- Followed by: Solar eclipse of October 23, 2014
Tritos
- Preceded by: Lunar eclipse of November 18, 1994
- Followed by: Lunar eclipse of September 16, 2016
Lunar Saros 146
- Preceded by: Lunar eclipse of October 7, 1987
- Followed by: Lunar eclipse of October 28, 2023
Inex
- Preceded by: Lunar eclipse of November 6, 1976
- Followed by: Lunar eclipse of September 28, 2034
Triad
- Preceded by: Lunar eclipse of December 17, 1918
- Followed by: Lunar eclipse of August 17, 2092
Lunar eclipses of 2002–2005
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 penumbral lunar eclipse on June 24, 2002 occurs in the previous 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 146
This eclipse is a part of Saros series 146, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on July 11, 1843. It contains partial eclipses from October 17, 2005 through May 14, 2348; total eclipses from May 25, 2366 through November 16, 2654; and a second set of partial eclipses from November 27, 2672 through June 12, 2997. The series ends at member 72 as a penumbral eclipse on August 29, 3123.
The longest duration of totality will be produced by member 37 at 99 minutes, 22 seconds on August 8, 2492. All eclipses in this series occur at the Moon’s ascending 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 partial solar eclipses of Solar Saros 153.
| October 12, 1996 | October 23, 2014 |
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References
External links
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