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DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

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length range, normally associated with optical<br />

<strong>and</strong>/or X-ray flares. Microwave bursts provide<br />

a powerful diagnostic of energetic electrons in<br />

the solar atmosphere.<br />

mid-ocean ridge A location of seafloor<br />

spreading (divergence zone). The more or less<br />

continuous line centered in the oceans where<br />

new material reaches the surface of the Earth,<br />

driven by convection in the Earth’s mantle. The<br />

Mid-Atlantic ridge begins in the North polar region,<br />

w<strong>and</strong>ers south between W15 ◦ <strong>and</strong> W45 ◦ ,<br />

essentially staying in the middle of the Atlantic<br />

Ocean. It connects to the Southwest Indian<br />

Ridge at about latitude S50 ◦ , longitude 0 ◦ . The<br />

Southwest Indian Ridge connects with the Indian<br />

Ridge at about S30 ◦ , E70 ◦ . From this<br />

junction, the Indian Ridge extends north as the<br />

Central Indian Ridge through the Red Sea; it<br />

extends South <strong>and</strong> East as the Southeast Indian<br />

Ridge along about S45 ◦ , becoming the Pacific<br />

Antarctic Ridge at S60 ◦ , E150 ◦ . This becomes<br />

the East Pacific Rise at about S60 ◦ , W120 ◦ . The<br />

East Pacific Rise runs north along approximately<br />

W100 ◦ , up the west coast of North America,<br />

ending around N50 ◦ as the Juan de Fuca ridge.<br />

Mie scattering Scattering of light by a spherical<br />

particle. Given the complex index of refraction<br />

of the particle, <strong>and</strong> the ratio of its radius to<br />

the wavelength of the light, it is possible to exactly<br />

solve Maxwell’s equations to find the fraction<br />

of light absorbed, <strong>and</strong> the fraction scattered,<br />

as well as the phase function of the scattered<br />

light <strong>and</strong> its polarization. The detailed solution<br />

of this problem is called Mie scattering.<br />

Mie size parameter For scattering by<br />

spheres, the ratio of a sphere’s circumference<br />

to the wavelength.<br />

migration (seismic) This is a technique<br />

which, when implemented on data from seismic<br />

reflection surveys, can help to elucidate the<br />

structure of the underlying rock. In a reflection<br />

survey, seismic waves are generated at one<br />

point on the Earth’s surface <strong>and</strong> recorded at geophones<br />

(i.e., seismic wave detectors) distributed<br />

nearby (for example, in a linear fashion behind<br />

a ship). Each time the seismic signal encounters<br />

a “reflector”, i.e., a rock layer that causes part<br />

© 2001 by CRC Press LLC<br />

Milankovich cycle<br />

of the seismic energy to be reflected back to the<br />

surface, a seismic pulse is returned to the geophones.<br />

The time delay between the generation<br />

of the seismic signal <strong>and</strong> its detection at a geophone<br />

depends on the speed of seismic waves<br />

in the rock, the depth of the reflector, <strong>and</strong> the<br />

horizontal distance between seismic source <strong>and</strong><br />

geophone, but also on the geometry of the reflector.<br />

For example, if the reflector is inclined<br />

upwards toward the geophone from the direction<br />

of the source, then the part of the reflection that<br />

is recorded at the geophone will have been reflected<br />

closer to the geophone, rather than midway<br />

between the geophone <strong>and</strong> the source if the<br />

reflector had been horizontal. Migration corrects<br />

this effect, <strong>and</strong> also removes other geometrical<br />

artifacts such as diffractions associated<br />

with scattering centers in the rock.<br />

Milankovich cycle Cyclic variations in climate<br />

driven by periodic changes in orbital <strong>and</strong><br />

Earth orientation parameters. Climate in a particular<br />

area depends on the solar flux, <strong>and</strong> therefore<br />

on both the distance from the Earth to the<br />

sun <strong>and</strong> the angle between the surface of the area<br />

in question <strong>and</strong> the sun’s rays over the course<br />

of a day (overhead sunlight leading to a greater<br />

flux than tangential sunlight). These both cause<br />

the seasonal variations in weather. The importance<br />

of the former depends on the eccentricity<br />

of the Earth’s orbit, which varies on a 96,000year<br />

cycle, while the importance of the latter<br />

depends on the obliquity, i.e., the angle between<br />

the planes defined by the Earth’s equator <strong>and</strong><br />

by the Earth’s orbit around the sun (the ecliptic<br />

plane), which varies between 21 ◦ <strong>and</strong> 24 ◦<br />

(it is currently at 23.5 ◦ ) <strong>and</strong> which varies on a<br />

41,000-year cycle. The effect of the eccentricity<br />

may be either to augment the seasonal variations<br />

in either the northern or southern hemisphere<br />

while reducing the variations in the other hemisphere<br />

(if the closest approach of the Earth to<br />

the sun occurs near a solstice, i.e., northern or<br />

southern winter), or to have a relatively neutral<br />

effect (if it occurs near an equinox, i.e., northern<br />

or southern spring). The orientation of the<br />

orbit is also cyclic, so that these effects vary on<br />

a 22,000-year timescale. As long, hard winters<br />

are thought to be important for growing ice<br />

sheets, these cycles may therefore have significant<br />

impact on global climate, although they<br />

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