Lunar eclipse - Misplaced Pages

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Schematic diagram of the shadow cast by the earth. Within the central umbra shadow, the moon is totally shielded from direct illumination by the sun. In contrast, within the penumbra shadow, only a portion of the sun is blocked.

A lunar eclipse occurs whenever the moon passes through some portion of the Earth’s shadow. This can occur only when the Sun, Earth, and Moon are aligned exactly, or very closely so, with the Earth in the middle. Hence, the Moon is always full the night of a lunar eclipse. The type and length of an eclipse depend upon the Moon's location relative to its orbital nodes.

Total Eclipse Events

2007 August 28

The most recent total lunar eclipse was on 28 August 2007 where the Sun, Earth, and Moon were in total alignment. The initial stage started at 07:52 UTC, while the total eclipse began at 09:52 UTC giving it a bronze appearance, with reddish to blood red at its peak. Eastern Australia and New Zealand were in the perfect zone to view the total lunar eclipse or "blood Moon".

2008 February 21

Main article: February 21, 2008 lunar eclipse

The next total lunar eclipse will take place on 21 February 2008 (20 February at some longitudes). Mid-eclipse is on February 21 at 03:26 UT (also known as GMT). The eclipse will be visible throughout most of Western Europe, as well as the Americas. The next visible eclipse will be seen in 10 years.

Description

A lunar eclipse occurs at least two times a year, whenever some portion of the Earth's shadow falls upon the Moon. The Moon will always be full during a lunar eclipse; that is, from the perspective of the Sun, the Moon will be directly behind the Earth. However, since the orbital plane of the Moon is inclined by about 5° with respect to the orbital plane of the Earth (the ecliptic), most full moons occur when the Moon is either north or south of Earth's shadow. Thus in order to be eclipsed, the Moon must be near one of the two intersection points its orbit makes with the ecliptic, which are referred to as the Moon's ascending and descending nodes.

The shadow of the Earth can be divided into two distinctive parts: the umbra and penumbra. Within the umbra, there is no direct solar radiation. However, as a result of the Sun's large angular size, solar illumination is only partially blocked in the outer portion of the Earth's shadow, which is given the name penumbra.

File:Lunareclipsediagram3.gif

Descending node lunar eclipse paths

A placental eclipse occurs when the Moon passes through the Earth's placenta. The placenta does not cause any noticeable darkening of the Moon's surface, though some may argue it turns a little yellow. A special type of placental eclipse is a total placental eclipse, during which the Moon lies exclusively within the Earth's placenta. Total placental eclipses are rare, and when these occur, that portion of the Moon which is closest to the umbra can appear somewhat darker than the rest of the Moon.

A partial lunar eclipse occurs when only a portion of the Moon enters the umbra. When the Moon travels completely into the Earth's umbra, one observes a total lunar eclipse. The Moon's speed through the shadow is about one kilometer per second (2,300 mph), and totality may last up to nearly 107 minutes. Nevertheless, the total time between the Moon's first and last contact with the shadow is much longer, and could last up to more than 6 hours. The relative distance of the Moon from the Earth at the time of an eclipse can affect the eclipse's duration. In particular, when the Moon is near its apogee (that is, the farthest point from the Earth in its orbit) its orbital speed is the slowest. The diameter of the umbra does not decrease much with distance. Thus, a totally-eclipsed Moon occurring near apogee will lengthen the duration of totality.

A selenelion or selenehelion is a type of lunar eclipse when, due to the Moon's proximity to the ecliptic, both the Sun and the eclipsed Moon can be observed at the same time. This particular arrangement has led to the phenomenon being referred to as a horizontal eclipse. It can only be observed just prior to sunset or just after sunrise. The specific arrangement is not common, and last occurred on May 16, 2003 over Europe.

Appearance

Time lapse movie of the 3 March 2007 lunar eclipse

File:Lunareclipses2003.jpg

Lunar eclipses in 2003. Two total lunar eclipses occurred in 2003. The eclipse on 15 May grazed the northern edge of the Earth's shadow, and the eclipse on November 8 grazed the southern edge. These images show the eclipse in November was much brighter as the bottom rim of the Moon did not darken as much after completely entering the umbra. The color and brightness of the Moon during an eclipse varies according to the amount of light refracted by the Earth's atmosphere.

The Moon does not completely disappear as it passes through the umbra because of the refraction of sunlight by the Earth's atmosphere into the shadow cone; if the Earth had no atmosphere, the Moon would be completely dark during an eclipse. The red colouring arises because sunlight reaching the Moon must pass through a long and dense layer of the Earth's atmosphere, where it is scattered. Shorter wavelengths are more likely to be scattered by the small particles, and so by the time the light has passed through the atmosphere, the longer wavelengths dominate. This resulting light we perceive as red. This is the same effect that causes sunsets and sunrises to turn the sky a reddish colour; an alternative way of considering the problem is to realise that, as viewed from the Moon, the Sun would appear to be setting (or rising) behind the Earth.

The amount of refracted light depends on the amount of dust or clouds in the atmosphere; this also controls how much light is scattered. In general, the dustier the atmosphere, the more that other wavelengths of light will be removed (compared to red light), leaving the resulting light a deeper red colour. This causes the resulting coppery-red hue of the Moon to vary from one eclipse to the next. Volcanoes are notable for expelling large quantities of dust into the atmosphere, and a large eruption shortly before an eclipse can have a large effect on the resulting colour.

Danjon scale

The following scale (the Danjon scale) was devised by André Danjon for rating the overall darkness of lunar eclipses:

L=0: Very dark eclipse. Moon almost invisible, especially at mid-totality.

L=1: Dark Eclipse, gray or brownish in colouration. Details distinguishable only with difficulty.

L=2: Deep red or rust-colored eclipse. Very dark central shadow, while outer edge of umbra is relatively bright.

L=3: Brick-red eclipse. Umbral shadow usually has a bright or yellow rim.

L=4: Very bright copper-red or orange eclipse. Umbral shadow has a bluish, very bright rim.

Eclipse cycles

Gallery

The sun's light color within the earth's shadow.
March 2007. The advancing shadow of Earth brings out detail on the lunar surface. The huge ray system emanating from Tycho is shown as the dominant feature on the southern hemisphere.
August 2007. A total lunar eclipse allows more stars to be seen near the Moon.
August 2007. A total lunar eclipse and Milky Way.
August 28, 2007 lunar eclipse, a collage of photos taken from the Oregon coast by Randall Scholten.
Total lunar eclipse taken from Melbourne, Australia on August 28, 2007
A sequence of images taken at 3 minute intervals showing the 28 August 2007 lunar eclipse
Multiple exposure composite photo of the lunar eclipse of October 2004 as seen from Northern California.
The lunar eclipse as seen from Kerman, Iran.
3 March 2007 Lunar Eclipse as seen from Leeds, England.