Royal Greenwich Observatory
Information Leaflet No. 12: 'Eclipses'.
We generally talk of eclipses of the Sun and Moon,
but other bodies inside and outside the Solar System exhibit eclipses that are very important in astronomy.
Eclipses of the moons of Jupiter were used in one of the first measures of the speed of light, and eclipsing binary stars give us fundamental data on the masses of those stars.
An eclipse occurs when a body cuts off the light from a light source so that we can no longer see it shining. An eclipse can be due either to a dark body coming between us and a light emitter, so that we can no longer see the source, or it can be a body coming between a light source and the body that the light is illuminating, so that we no longer see the illuminated body.
Let us first consider eclipses of the Sun and Moon.
Eclipses of the Sun and Moon:
An eclipse of the Sun occurs when the Moon comes directly between the Sun and the Earth so that the Earth lies in the shadow of the Moon.
An eclipse of the Moon occurs when the Earth lies directly between the Sun and the Moon, and the Moon lies in the shadow of the Earth.
If the orbit of the Moon about the Earth lay in the same plane as the orbit of the Earth about the Sun then there would be eclipses of the Sun and Moon at every New and Full Moon respectively. The orbits are inclined, however, and eclipses can only occur when the Moon is close to the nodes of its orbit (when it is near to the places where the orbital planes cross).
The amount of the Moon's disk that is eclipsed depends on how close the Moon is to the node of its orbit at Full Moon.
Like all shadows of light from an extended source, the shadow produced by the Earth has an umbra,
where all the light from the Sun is shadowed, and a penumbra, where only some of it is.
Penumbral eclipses of the Moon occur when the Moon passes only through the Earth's penumbral shadow. Although these are catalogued they are inconspicuous events and are not noteworthy.
When the Moon passes through the Earth's umbral shadow, we can either see a Partial Eclipse, when only part of the Moon is obscured,
or a Total Eclipse.
The Earth's shadow is much larger than the Moon, and so eclipses can last up to 3 hrs 40 mins., with totality lasting up to 1 hr 40 mins. They can be seen from anywhere on the side of the Earth that faces the Moon.
During a Total Eclipse, the Moon does not, as might be expected, disappear entirely, but turns a deep, dark red. The brightness and colour depend on the state of the Earth's atmosphere; for the Moon, during eclipse, is illuminated by light that has passed through the Earth's atmosphere and has been bent towards the Moon by refraction.
As an illustration, see
Andrés Valencia: Total Lunar Eclipse - April 3 '96 and
Andrés Valencia: Total Lunar Eclipse - Sept. 26 '96 in ARVAL's Gallery.
Note that during a Total Eclipse of the Moon, not all of the Moon's disc is equally obscured; the umbra is less dense towards its border with the penumbra.
These, like Lunar Eclipses, can only occur when the Moon is near the nodes
of its orbit, but in this case, at New Moon. The shadow of the Moon can
then pass over the surface of the Earth.
Because the Moon is much smaller than the Earth, its shadow only covers a small part of the Earth's surface, and a solar eclipse can only be seen from a restricted area.
Like the Earth's shadow, the Moon's has an umbra and a penumbra. Viewed from the Earth, a person in the umbra sees the whole of the Sun eclipsed while someone in the penumbra sees only part of the Sun obscured. These are called a Total and a Partial Eclipse respectively.
Quite by chance, the apparent sizes of the Sun and the Moon are very nearly
The apparent angular size of the Sun does not change very much due to the Earth's non-circular orbit, but the Moon's apparent size varies quite a lot. For most solar eclipses the Moon's apparent diameter is less than the Sun's, and so the whole solar disk is nowhere totally obscured. It is only when the Moon is close to the Earth that, at some places, the whole disk is obscured and a Total Eclipse is seen.
The track of the small area on the Earth's surface where a total eclipse can be seen is several thousand miles long but only up to 160 miles wide. Outside this track and outside the short time of totality, maximum about 7 minutes, a Partial Eclipse is seen.
When the Moon is not at its closest to the Earth its apparent diameter is less than that of the Sun and even where the Moon's disk obscures the Sun centrally the outer ring of the Sun's disk is still visible. This is called an Annular Eclipse.
Total eclipses of the Sun are much more spectacular than Partial eclipses, as virtually all the light from the Sun is blocked out by the Moon and it becomes as dark as night, and stars can be seen. The solar chromosphere and corona can be seen. The former as a reddish rim around the eclipsing Moon, and the latter as a whitish glow surrounding the eclipsed Sun.
The length of totality depends on how close the Moon is to the Earth. The 1991 total eclipse was the longest for 140 years. The next total solar eclipse to be visible in Britain will be in August 1999. It will only be visible from parts of Cornwall and Devon.
The next total solar eclipse to be visible in Venezuela, will be in February 1998. It will only be visible from parts of Zulia and Falcon. Northeast of Paraguaná, the islands of Aruba and Curaçao will also experience totality. See Paraguaná: Total Eclipse of the Sun, February 26 '98
WARNING! Never look at the Sun with any kind of telescope or binoculars. You could easily blind yourself. It is even dangerous to look at the fully bright Sun with the naked eye.
The eclipse of an apparently small object by one that appears much larger is generally called an occultation. Thus the Moon occults many stars as it moves across the sky. Observations of occultations by the Moon were used for a long time to get the most accurate positions for the Moon and have been used to determine the position and size of such strange objects as radio stars.
Eclipses of the satellites of Jupiter by the planet, and also by one another, were used in one of the first determinations of the speed of light. And occultations of stars by the planets have allowed analyses of the planetary atmospheres.
Eclipsing binary stars, in which two stars are in orbit about each other, and each passes in front of the other as seen from the Earth, have given us most of our knowledge of the masses of different kinds of stars.
See also; 'The Sun', 'Photometry', 'What is a Star?', and 'The Metonic Cycle and the Saros.
Produced by the Information Services Department of the Royal Greenwich Observatory.
PJA Tue Apr 16 10:58:04 GMT 1996
Updated: October 14 '97, June 27 '14
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