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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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emissivity<br />

cence of aromatic hydrocarbons pumped by UV<br />

photons. Similarly, emission from both atoms<br />

(i.e., sodium D lines) <strong>and</strong> fluorescence from<br />

molecules (i.e., 3.4 µm, methanol) <strong>and</strong> fragments<br />

(i.e., Swan b<strong>and</strong>s ofC2 ∗) excited by sunlight<br />

have been observed from cometary comae.<br />

emissivity An indirect measure of reflectivity,<br />

where emissivity = 1 − reflectivity <strong>and</strong> reflectivity<br />

is the reflected energy measured from<br />

a surface by a single energy bounce. Mirrored<br />

surfaces reflect large amounts of energy (around<br />

98%) but absorb very little (around 2%). A<br />

blackbody surface, on the other h<strong>and</strong>, reverses<br />

the ratio, absorbing 98% of the energy <strong>and</strong> reflecting<br />

only 2%. Emissivity is affected by<br />

the geometric shape of the object, the electrical<br />

properties of the radiating surface, <strong>and</strong> the<br />

measuring wavelength.<br />

A Magellan radiometer experiment observed<br />

the 12.6-cm-wavelength radiothermal emissivity<br />

on Venus. The nominal pattern of radiothermal<br />

emissivity shows high mountain summits<br />

display abnormally low emissivity <strong>and</strong> plains regions<br />

high emissivity. One explanation for the<br />

low emissivity of mountaintops is the presence<br />

of electrically conductive minerals, produced by<br />

weathering, embedded in the surface rocks.<br />

empirical model of the magnetosphere A<br />

mathematical representation of the global magnetic<br />

field of the magnetosphere, whose coefficients<br />

are fitted to data. It is a convenient tool<br />

for predicting the magnetic field vector or field<br />

line linkage to the ionosphere which a satellite<br />

at some point P in space is most likely to find.<br />

The construction of empirical fields is also the<br />

best way of extracting global information from<br />

magnetic field data.<br />

The parameters of modern empirical models<br />

are generally derived from flexible representations<br />

of the fields of the different magnetospheric<br />

current systems, e.g., those of the magnetopause,<br />

tail, ring current, <strong>and</strong> the Birkel<strong>and</strong><br />

current circuit. The field predicted at P depends<br />

not only on the location but also on the tilt angle<br />

ψ, on the dynamic pressure of the solar wind,<br />

on the interplanetary magnetic field <strong>and</strong> on geomagnetic<br />

activity indices such as Dst <strong>and</strong> AE.<br />

© 2001 by CRC Press LLC<br />

152<br />

Enceladus Moon of Saturn, also designated<br />

SII. Discovered by Herschel in 1789 its surface<br />

has the highest albedo of any solar system body.<br />

It also displays evidence of resurfacing, possibly<br />

as a result of water volcanism. Since it is<br />

too small to retain radioactive heat, tidal heating<br />

aided by a 1:2 resonance with Dione may<br />

provide the required energy. Its orbit has an eccentricity<br />

of 0.0045, an inclination of 0.00 ◦ ,a<br />

precession of 156.2 ◦ yr −1 , <strong>and</strong> a semimajor axis<br />

of 2.38 ×10 5 km. Its radius is 250 km, its mass,<br />

8.40 × 10 19 kg, <strong>and</strong> its density 1.28 g cm −3 .It<br />

has a geometric albedo of 1.0, <strong>and</strong> orbits Saturn<br />

once every 1.370 Earth days.<br />

Encke’s comet Comet with the shortest<br />

known orbital period: 3.30 years. Its orbit has<br />

semimajor axis 2.21 AU <strong>and</strong> perihelion distance<br />

0,338 AU.<br />

endothermic A process that absorbs heat as<br />

it proceeds. Opposite of exothermic.<br />

energetic particles Supra-thermal particles;<br />

that is all particles with speeds large compared<br />

to the thermal plasma speed.<br />

energetic particles in interplanetary space<br />

Energetic particles in interplanetary space can<br />

be observed with energies ranging from the<br />

supra-thermal up to 10 20 eV. The main constituents<br />

are protons,α-particles, <strong>and</strong> electrons;<br />

heavier particles up to iron can be found in substantially<br />

smaller numbers. The particle populations<br />

originate in different sources, all having<br />

their typical spectrum, temporal development,<br />

<strong>and</strong> spatial extent.<br />

1. Galactic cosmic rays (GCR) are the highenergy<br />

background with energies extending up<br />

to 10 20 eV. They are incident upon the heliosphere<br />

uniformly <strong>and</strong> isotropically. In the inner<br />

heliosphere, the galactic cosmic radiation<br />

is modulated by solar activity: the intensity of<br />

GCRs is highest during solar minimum <strong>and</strong> reduced<br />

during solar maximum conditions. See<br />

modulation of galactic cosmic rays.<br />

2. Anomalous galactic cosmic rays (AGCR),<br />

also called anomalous component, energetically<br />

connect to the lower end of the galactic cosmic<br />

rays but differ from them with respect to composition,<br />

charge states, spectrum, <strong>and</strong> variation

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