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DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

DICTIONARY OF GEOPHYSICS, ASTROPHYSICS, and ASTRONOMY

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detritus<br />

detritus The particulate decomposition or<br />

disintegration products of plankton, including<br />

dead cells, cell fragments, fecal pellets, shells,<br />

<strong>and</strong> skeletons, <strong>and</strong> sometimes mineral particles<br />

in coastal waters.<br />

deuterium 2H; the isotope of hydrogen<br />

whose nucleus consists of 1 proton <strong>and</strong> 1 neutron.<br />

The nucleus is called a deuteron.<br />

deuterium burning The capture of a proton<br />

by a deuteron to produce 3 He (which then<br />

easily burns through to 4 He; see proton-proton<br />

chain). Deuterium burning occurs at the lowest<br />

temperature of any important nuclear reaction,<br />

about 10 6 K. Thus, its onset marks the end of the<br />

protostellar collapse stage of star formation (see<br />

proto-star). It is the only reaction that occurs in<br />

thelowestmassstars, near0.08solarmasses(see<br />

brown dwarf), <strong>and</strong> it has long ago destroyed all<br />

the deuterium in the sun <strong>and</strong> other normal stars.<br />

Thus, the presence of deuterium in the Earth <strong>and</strong><br />

other planets means they are made of material<br />

that was never inside the sun. Deuterium is produced<br />

only in the early universe (see Big Bang<br />

nucleosynthesis).<br />

de Vaucouleurs’ classification scheme A<br />

classification scheme that refines <strong>and</strong> extends<br />

the Hubble scheme of classification for galaxies,<br />

introduced by G. de Vaucouleurs in 1959.<br />

de Vaucouleurs’ scheme attempts to account for<br />

the variety of morphologies observed for each<br />

Hubble type. His scheme employs three main<br />

parameters: (1) a refined Hubble type, where<br />

severalintermediatestagesareaddedtotheHubble<br />

sequence, notably E + ,S0 − ,S0 + , which<br />

account for some lenticular features in ellipticals<br />

or weak arms in S0 galaxies, <strong>and</strong> Sd, Sm,<br />

<strong>and</strong> Im, which more closely detail the transition<br />

from Sc to Magellanic irregulars; (2) a parameterdescribingthespiraldesign,<br />

asringshaped(r)<br />

or s-shaped (s), or intermediate (rs); <strong>and</strong> (3) a parameter<br />

designating barred galaxies (SB), nonbarred<br />

(SA), <strong>and</strong> intermediate (SAB), for galaxies<br />

where the bar is less developed than in classical<br />

Hubble’s barred galaxies. In addition, the<br />

presence of an outer ring or of a ring-like feature<br />

formed by joining spiral arms is indicated with<br />

an uppercase R preceding all other labels. The<br />

de Vaucouleurs classification scheme has been<br />

© 2001 by CRC Press LLC<br />

extensively used in the three editions of the Reference<br />

Catalogue of Galaxies, where de Vaucouleurs’<br />

types are given for several thous<strong>and</strong><br />

galaxies. For example, Messier 31, the spiral<br />

galaxy nearest to the Galaxy, <strong>and</strong> the nearby<br />

spiral Messier 101 are classified as Sb <strong>and</strong> as<br />

Sc according to Hubble, <strong>and</strong> as SA(s)b <strong>and</strong> as<br />

SAB(rs)cd according to de Vaucouleurs.<br />

de Vaucouleurs’ law Empirical law describing<br />

the brightness profile of an elliptical galaxy.<br />

The surface brightness of typical giant elliptical<br />

galaxies, apart from constants, decreases<br />

with radius as<br />

log(r)∝(r/re) −1/4 ,<br />

where re denotes a scaling parameter, the effective<br />

radius, within which half the light of<br />

the galaxy is emitted. de Vaucouleurs’ law applies<br />

more frequently to giant elliptical galaxies;<br />

dwarf elliptical galaxies are often better fitted by<br />

other laws. See elliptical galaxies.<br />

deviative absorption Deviative absorption<br />

ofaradiowaveoccursnearthepointofreflection<br />

in the ionosphere. See critical frequency.<br />

deviatoric strain A state of strain defined<br />

by subtracting one-third of the volumetric strain<br />

from the total strain. If εij is the total strain<br />

tensor, the deviatoric strain tensor is ε ′ ij = εij −<br />

θδij /3, where θ = εii = ε11 + ε22 + ε33, <strong>and</strong><br />

δij is the Kronecker delta.<br />

deviatoric stress A state of stress with pressure<br />

subtracted. If σij is the total stress tensor,<br />

the deviatoric stress tensor is σ ′ ij = σij − pδij ,<br />

where p = σii/3 = (σ11 + σ22 + σ33)/3, <strong>and</strong><br />

δij is the Kronecker delta.<br />

dew During night or early morning, due to<br />

radiational cooling, water condensed onto objects<br />

near the ground whose temperature has<br />

fallen below the dew point of adjacent air but<br />

still above freezing. Dew often appears in warm<br />

seasons with clear weather <strong>and</strong> light winds. Although<br />

the amount of water is small, in dry season<br />

<strong>and</strong> regions it amounts to a significant contribution<br />

to plant growth requirements.

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