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January 2001 lunar eclipse
Total lunar eclipse 9 January 2001 From Wikipedia, the free encyclopedia
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A total lunar eclipse occurred at the Moon’s ascending node of orbit on Tuesday, January 9, 2001,[1] with an umbral magnitude of 1.1902. 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 only about 8 hours before perigee (on January 10, 2001, at 4:00 UTC), the Moon's apparent diameter was larger.[2]
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Visibility
The eclipse was completely visible over Africa, Europe, and Asia, seen rising over eastern and northern North America and eastern South America and setting over Australia and the western Pacific Ocean.[3]
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 Hourly motion shown right to left |
 The Moon passed straight through the center of the Earth's shadow at the descending node in Gemini. | |
Eclipse details
Shown below is a table displaying details about this particular solar 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.
Related eclipses
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Eclipses in 2001
- A total lunar eclipse on January 9.
- A total solar eclipse on June 21.
- A partial lunar eclipse on July 5.
- An annular solar eclipse on December 14.
- A penumbral lunar eclipse on December 30.
Metonic
- Preceded by: Lunar eclipse of March 24, 1997
- Followed by: Lunar eclipse of October 28, 2004
Tzolkinex
- Preceded by: Lunar eclipse of November 29, 1993
- Followed by: Lunar eclipse of February 21, 2008
Half-Saros
- Preceded by: Solar eclipse of January 4, 1992
- Followed by: Solar eclipse of January 15, 2010
Tritos
- Preceded by: Lunar eclipse of February 9, 1990
- Followed by: Lunar eclipse of December 10, 2011
Lunar Saros 134
- Preceded by: Lunar eclipse of December 30, 1982
- Followed by: Lunar eclipse of January 21, 2019
Inex
- Preceded by: Lunar eclipse of January 30, 1972
- Followed by: Lunar eclipse of December 20, 2029
Triad
- Preceded by: Lunar eclipse of March 12, 1914
- Followed by: Lunar eclipse of November 10, 2087
Lunar eclipses of 1998–2002
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 eclipses on March 13, 1998 and September 6, 1998 occur in the previous lunar year eclipse set, and the penumbral lunar eclipses on May 26, 2002 and November 20, 2002 occur in the next lunar year eclipse set.
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Saros 134
This eclipse is a part of Saros series 134, repeating every 18 years, 11 days, and containing 72 events. The series started with a penumbral lunar eclipse on April 1, 1550. It contains partial eclipses from July 7, 1694 through October 13, 1856; total eclipses from October 25, 1874 through July 26, 2325; and a second set of partial eclipses from August 7, 2343 through November 12, 2505. The series ends at member 72 as a penumbral eclipse on May 28, 2830.
The longest duration of totality will be produced by member 38 at 100 minutes, 23 seconds on May 22, 2217. 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 annular solar eclipses of Solar Saros 141.
| January 4, 1992 | January 15, 2010 |
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External links
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