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[A]
Accretion disk A rotating disk of gas orbiting a star, formed by
material falling toward the star (Kuhn, 1998).
Accretionary heating Thermal energy resulting from bolide impacts
upon the surface of an object (Planetary Geology for Teachers,
1999).
Achondrites A rare stony meteorite without spherical granules
(chondrites). Achondrites represent meteorites that are most like
terrestrial rocks (Bates and Jackson, 1984).
Albedo The ratio of the amount of solar radiation reflected from
an object to the total amount incident upon it (Welcome to the Planets,
1995).
Albite A white or colorless, lower relative temperature,
triclinic mineral of the feldspar group:
(NaAlSi3O8). It is a variety of plagioclase that
commonly occurs in igneous and metamorphic rocks (Bates and Jackson,
1984).
Alluvial fan An outspread, gently sloping mass of alluvium
deposited by a stream, esp. in an arid or semiarid region where a stream
issues from a narrow canyon onto a plain or valley floor (Bates and
Jackson, 1984).
Alpine glaciers A glacier or body of compacted snow and ice, in
mountainous terrain. It generally originates in a cirque and may flow
down a valley previously made by a stream (Bates and Jackson,
1984).
Amphibole A mineral group with the general formula
A2B2(Si,Al)8O22(OH)2
where A is mainly Mg,Fe,Ca, or Na, and B is mainly Mg, Fe+2,
Al, or Fe+3. The most common amphibole minerals are
hornblende, tremolite-actinolite and cummingtonite-grunerite (Bates and
Jackson, 1984).
Anion A negatively charged atom or molecule resulting from the
atom’s gain of an electron (Beatty and Chaikin, 1990).
Anorthite A white or gray, high temperature, triclinic mineral of
the feldspar group: (CaAl2Si2O8). It is
the most calcic member of the plagioclase series, and occurs esp. in
basic and ultrabasic igneous rocks (Bates and Jackson, 1984).
Anorthosite A plutonic rock composed almost wholly of plagioclase
(Bates and Jackson, 1984).
Antipodes Two points on the surface of a celestial body that are
diametrically opposed to each other. The term may be extended to include
a whole region at the opposite end of a body’s diameter, as on Earth,
Australia and New Zealand are roughly opposite the British Isles (Bates
and Jackson, 1984).
Antipodes/ hills of Mercury "Weird terrain" best describes
this hilly, lineated region of Mercury. This area is at the antipodal
point from the large Caloris basin. The shock wave produced by the
Caloris impact was reflected and focused to this antipodal point, thus
jumbling the crust and breaking it into a series of complex blocks. The
area covered is about 100 kilometers (62 miles) on a side (Planetary
Geology for Teachers, 1999).
Aphelion The point in the orbit of a planet, asteroid, comet, or
other body that is farthest from the sun (Kuhn, 1998).
Aphrodite Terra (Venus) Approximately the size of Africa,
Aphrodite terra straddles the equator, is over 10,000 kilometers (6,214
miles) long, and is made up of four smaller highlands: Ovda, Thetis,
Atla, and Ulfrun Regiones. Western Aphrodite Terra is believed to be the
site of crustal spreading on Venus, with an estimated separation rate of
several centimeters per year (Beatty and Chaikin, 1990).
Apogee The point in the orbit of an Earth satellite where it is
farthest from the Earth (Kuhn, 1998).
Apollo asteroids Asteroids that cross the Earth’s orbit (Beatty
and Chaikin, 1990).
Arachnoids A coronae with less than a 170 kilometer (106-mile)
diameter. It is a circular-to-elongate Venusian feature surrounded by
multiple concentric ridges and complex lineations, thought to be formed
by hot spots (Planetary Geology for Teachers, 1999).
Archean The earlier part of Precambrian time form about 2500mya
to 570 mya (Bates and Jackson, 1984).
Arete A rocky, sharp-edged ridge or spur, commonly present above
the snowline in rugged mountains sculptured by glaciers, and resulting
from the continued backward growth of the walls of adjoining cirques
(Bates and Jackson, 1984).
Asteroid belt Asteroids that orbit the Sun at distances from 2.2
AU to 3.6 AU. This orbital zone between Mars and Jupiter is the location
of most of the known asteroids (Kuhn, 1998).
Asteroids Any of the 1000’s of small rocky/metallic bodies that
orbit the sun mostly between Mars and Jupiter; also referred to as minor
planets (Welcome to the Planets, 1995).
Asthenophere The layer or shell of the Earth below the
lithosphere, which is weak and in which isostatic adjustments take
place, magmas may be generated, and seismic waves are strongly
attenuated. The asthenosphere begins about 100 km below the surface and
extends to a depth of about 350 km (Bates and Jackson, 1984).
Atmosphere (Earth) The gaseous envelope surrounding the
Earth. 78% nitrogen, 21% oxygen, 0.9% argon, 0.3% carbon dioxide and
other trace elements (Bates and Jackson, 1984).
Atom The smallest unit of material which retains its chemical
identity (Beatty and Chaikin, 1990).
Atomic mass The total number of protons and neutrons in the
nucleus of an atom (Beatty and Chaikin, 1990).
Atomic number The total number of protons in the nucleus of an
atom (Beatty and Chaikin, 1990).
Augite A dark mineral of the pyroxene group, (Ca,Na)( Mg,
Fe+2, Al)(Si,Al) 2O6. It is an
essential constituent of many basic igneous rocks (Bates and Jackson,
1984).
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Baryons A fundamental atomic particle. The known baryons include
protons, neutrons and hyperons which are said to have a baryon number of
1 (Beatty and Chaikin, 1990).
Basalt A fine-grained, dark rock made of plagioclase and pyroxene
(often with olivine and Fe-oxides), it usually occurs as lava flows or
tephra (fragmented lava that makes up cinder cones, spatter cones, etc).
Basaltic magma is generated by partial melting of mantle rock, and rises
through the crust to the surface (Planetary Geology for Teachers,
1999).
Basin A depressed area with no surface outlet (Welcome to the
Planets, 1995).
Batholith A large, generally discordant plutonic mass that has
> 40 square miles (100 km2) of surface area and no known
floor (Bates and Jackson, 1984).
Belts Thick, rotating clouds that swirl around the planet,
blowing in opposite directions in adjacent bands. The darker colored
bands are called belts (Beatty and Chaikin, 1990).
Beta Regio (Venus) Best example of an upland dome is Beta Regio
located around 280° E. longitude and 30° N. Latitude (Planetary Geology
for Teachers, 1999).
Big Bang One theory of the origin of the universe that proposes a
tremendous release of energy (i.e.an explosion) called the "big bang"
which initiated the formation of matter approximately 15 billion years
ago. This is partly suggested by the astronomical observation that the
universe is expanding; the expansion is projected backwards in time to
some initial state (singularity) (Planetary Geology for Teachers,
1999).
Biosphere All the areas of the Earth occupied by living
organisms, including the lithosphere, hydrosphere and atmosphere (Bates
and Jackson, 1984).
Biotite A common rock forming mineral of the mica group,
K(Mg,Fe+2)3(Al,Fe+3)
Si3O10(OH)2. It is black in hand
specimen, brown or green thin section, and has perfect basal (001)
cleavage (Bates and Jackson, 1984).
Black hole A celestial object of infinite density whose escape
velocity exceeds the speed of light (Kuhn, 1998).
Blowouts A general term for various saucer- or through-shaped
hollows formed by wind erosion on a dune or other sand deposit: the
adjoining accumulation of sediment derived from the depression where
readily recognizable, is commonly included (Bates and Jackson,
1984).
Breccia A coarse-grained, clastic rock, composed of angular,
broken rock fragments held together by a mineral cement or a
fine-grained matrix (Bates and Jackson, 1984).
Bright highlands (Venus) Magellan images of highland regions
above 2.5 kilometers (1.5 miles) are unusually bright, characteristic of
moist soil. However, liquid water does not exist on the surface and
cannot account for the bright highlands. One theory suggests that the
bright material might be composed of metallic compounds (Planetary
Geology for Teachers, 1999).
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Canali (Venus, Mars) Long sinuous forms, Canali are best
preserved in regions of subdued relief. They have a high width-to-depth
ratio and maintain a remarkably constant width over very long distances.
Images reveal the presence of meanders, point bars, cut banks, and
abandoned channel segments (Planetary Geology for Teachers,
1999).
Caldera A large, basin-shaped volcanic depression that is more or
less circular in form. Most calderas are produced by collapse of the
roof of a magma chamber due to removal of magma by voluminous eruptions
or subterranean withdrawal of the magma, although some calderas may be
formed by explosive removal of the upper part of a volcano (Bates and
Jackson, 1984).
Caloris Basin (Mercury) Caloris is Latin for heat and the basin
is named this because it is near the subsolar point (the point closest
to the sun) when Mercury is at aphelion. Caloris basin is 1,300
kilometers (800 miles) in diameter and is the largest known structure on
Mercury. It was formed from an impact of a projectile with asteroid
dimensions. The interior floor of the basin contains smooth plains but
is highly ridged and fractured. The large impactor is believed to be
buried below the floor of the crater and contributes to the uneven mass
of the planet (Planetary Geology for Teachers, 1999).
Carbonaceous chondrites Asteroids made of undifferentiated
silicates with carbon compounds and water (densities ~2.3gm/cc). They
represent the primordial material of the Solar System from which planets
accreted. Besides an aggregate of carbonaceous dust and hydrated
silicates, they also contain chondrules, spherical blobs ranging in size
from less than 1 mm to nearly 2 cm that have higher temperatures of
melting than the surrounding material. Chemical analyses indicate that,
except for volatile elements (H, He, Ne, Ar, N, etc.), the relative
chemical proportions of rock-forming elements (e.g. Si, O, Mg, Fe, Ca,
Al, etc.) in carbonaceous chondrites closely correspond to the relative
proportions in the Sun (Planetary Geology for Teachers, 1999).
Carbonates A mineral compound characterized by a fundamental
anion structure of CO3-2. Calcite and aragonite,
CaCO3 are examples (Bates and Jackson, 1984).
Cassini Gian Domenico Cassini, (1625-1712). An astronomer born in
Italy, Cassini later became a naturalized French citizen. He discovered
four of Saturn's satellites and observed a dark division in Saturn's
ring (the Cassini Division) (Welcome to the Planets, 1995).
Cassini Division A space observed between the A and B segments of
Saturn’s rings. The gap is believed to have been created by the
gravitational pull from Mimas, one of Saturn’s moons (Planetary Geology
for Teachers, 1999).
Cataclasis A special type of metamorphism in which "weathering"
involving mechanical processes along fault zones pulverizes mineral
grains into smaller grains and dust. This type of metamorphism depends
on forces related to tectonics (faulting). Another form of cataclasis is
impacting, which involves planetesimal bodies such as asteroids striking
the planet with enough energy to pulverize, or even melt, rock
(Planetary Geology for Teachers, 1999).
Cation A positively charged atom or molecule resulting from the
atom’s loss of an electron (Beatty and Chaikin, 1990).
Cenozoic The latest of the four eras into which geologic time is
divided; it extends from the close of the Mesozoic Era, about 65 mya, to
the present. The Cenozoic Era is subdivided into the Tertiary and the
Quaternary Periods (Bates and Jackson, 1984).
Channels (Venus) Lava channels extending from hundreds to
thousands of kilometers in length are conspicuous on the Venusian
plains. Simple channels typically show little or no branching. They
include long sinuous forms, termed "canali", and sinuous rilles. Canali
are best preserved in regions of subdued relief. They have a high
width-to-depth ratio and maintain a remarkably constant width over very
long distances. Images reveal the presence of meanders, point bars, cut
banks, and abandoned channel segments (Planetary Geology for Teachers,
1999).
Chaotic terrain (Mars) Regions of fractured, jumbled rocks that
apparently collapsed when groundwater suddenly surged outward (Planetary
Geology for Teachers, 1999).
Chemical potential energy Stored energy contained in matter that
can be released by chemical reactions (Beatty and Chaikin, 1990).
Chemical weathering The process whereby minerals in rocks are
dissolved or changed to other minerals, such as feldspar weathers to a
clay mineral (both are alumino-silicates). This type of weathering is
enabled by processes such as hydration, oxidation, and ion exchange
(Planetary Geology for Teachers, 1999).
Chlorite A group of platy, monoclinic, usually greenish minerals
of the general formula: (Mg, Fe+2,
Fe+3)6AlSi3O10(OH)8.
Chlorites are associated with and resemble micas, they may also be
considered as clay minerals. They are widely distributed, esp. in
low-grade metamorphic rocks, or as alteration products in ferromagnesian
minerals (Bates and Jackson, 1984)..
Chondrites A stony meteorite containing spherical granules,
usually about one mm in diameter, consisting chiefly of olivine and/or
enstatite or bronzite embedded in a fine matrix of pyroxene, olivine,
and nickel-iron with or without glass. They constitute more than 80% of
meteorite falls (Bates and Jackson, 1984).
Chromosphere The region of the solar atmosphere between the
photosphere and the corona notable for its ruby red light. Temperatures
of the chromosphere vary from 4500 K at its base to 8500 K at its top
(Kuhn, 1998).
Cirque A deep steep-walled recess or hollow, horseshoe-shaped or
semicircular in plan view, situated high on the side of a mountain and
produced by the erosive activity of a mountain glacier. It often
contains a small round lake (Bates and Jackson, 1984).
Coma A roughly spherical region of diffuse gas which surrounds
the nucleus of a comet. Together, the coma and the nucleus form the
comet's head (Welcome to the Planets, 1995).
Comet Shoemaker-Levy 9 On July 7, 1992, Comet Shoemaker-Levy 9
made a close approach to Jupiter and broke apart into 21 pieces due to
tidal forces inside Jupiter’s Roche limit. On the subsequent pass, each
of the pieces of the comet impacted Jupiter (Planetary Geology for
Teachers, 1999).
Comets Small, icy bodies that revolve around the sun, usually
with long periods, that are made up of a nucleus, coma and two tails-
one composed of ions and the other composed of dust. Also, a small
celestial body composed at least partially of ices. Comets either orbit
the Sun or pass through the Solar System on hyperbolic orbital paths
(Welcome to the Planets, 1995).
Composite volcano A volcano that is constructed of alternating
layers of lava and pyroclastic deposits, along with abundant dikes and
sills. Also, a composite cone (Bates and Jackson, 1984).
Compound A distinct substance formed by the union of two or more
ingredients in definite proportions by weight; for example,
H2O (Beatty and Chaikin, 1990).
Compression wave Kinetic energy is transferred by a shock wave
that spreads outward from the point of impact (Planetary Geology for
Teachers, 1999).
Conduction The transfer of heat in a solid by collisions between
atoms and/or molecules (Kuhn, 1998).
Conglomerate A cemented mixture of rounded pebbles transported
from various places. Rounding is evidence of stream transport that
causes the sharp edges and corners to become worn down as the particle
is bounced along with other particles in a stream (Planetary Geology for
Teachers, 1999).
Continental crust The rocks of the continental crust underlie the
continents; they are equivalent to sial, and range in thickness from
about 35 km to as much as 60 km under mountain ranges. The density of
the upper layer of the continental crust is ~ 2.7 g/cm3, and
the velocity of compressional seismic waves through it are less than ~
7.0 km/sec (Bates and Jackson, 1984).
Continental glaciers A glacier or body of compacted snow and ice,
of considerable thickness and more than 50,000 square kilometers in
extent, forming a continuous cover of ice and snow, spreading outward in
all directions, and not confined to the underlying topography (Bates and
Jackson, 1984).
Continental rift A long, narrow continental through bounded by
normal faults, a graben of regional extent, often associated with
volcanism (Bates and Jackson, 1984).
Convection Fluid circulation driven by temperature gradients; the
transfer of heat by this automatic circulation within gaseous or liquid
materials (Kuhn, 1998).
Convection Zone (Sun) The outer 30% of the Sun’s radius where
heat is transferred via convection currents. Temperatures continue to
drop in this zone from 1.5 x 106 K at the base to 5800 K at
the surface or photosphere (Kuhn, 1998).
Convergent Boundary A boundary between two crustal plates that
are moving together, with the more dense plate descending beneath the
less dense, usually continental, overriding plate (Bates and Jackson,
1984).
Copernicus Polish astronomer who advanced the heliocentric theory
that the Earth and other planets revolve around the Sun. This was highly
controversial at the time as the Ptolemaic view of the universe
(geocentric theory), which was the prevailing theory for over 1000
years, was deeply ingrained in the prevailing philosophy and religion.
(It should be noted, however, that the heliocentic idea was first put
forth by Aristarcus of Samos in the 3rd century BC, a fact known to
Copernicus but long ignored.) (Kuhn, 1998).
Core (Earth) The central part of the Earth, beginning at a
depth of about 2900 km, probably consisting of iron-nickel alloy; it is
divisible into a solid inner and liquid outer core (Bates and Jackson,
1984).
Core (of the Sun) Site of nuclear fusion where hydrogen is fused
into helium and thermonuclear energy is released. The core temperature
of the Sun is approximately 1.5 x 107 K (Kuhn, 1998).
Core formation The heat driven process whereby materials of
higher density sink through less dense material and form the center of a
planet. Also, planetary differentiation (Planetary Geology for Teachers,
1999).
Corona (Geology) A circular to elongate feature which is
surrounded by multiple concentric ridges. Coronae are thought to be
formed by hot spots (Welcome to the Planets, 1995).
Corona (Venus) A 170- to 1,000-kilometer- (106- to
621-mile-) diameter circular-to-elongate Venusian feature surrounded by
multiple concentric ridges, thought to be formed by hot spots (Planetary
Geology for Teachers, 1999).
Corona: (Sun) The outermost portion of the Sun’s
atmosphere. During eclipse it is observed as a white, glowing light
extending far into interplanetary space. Corona temperatures are about
1.0 x 106 K near the transition zone where the chromosphere
gives way to the corona (Kuhn, 1998).
Covalent bond A chemical bond formed by the sharing of a pair of
electrons between atoms (Beatty and Chaikin, 1990).
Crater An approximately circular depression, sometimes surrounded
by a raised rim. Craters are typically formed by explosion during
meteorite impact (Welcome to the Planets, 1995).
Crater degradation Once a crater has been formed, it will degrade
over time as gravity and isostatic rebound modify the crater walls and
floor. The central portion of a large crater will rise by isostatic
uplift that results from removal of overburden. Walls may collapse by
slumping to produce terraced crater walls that form the rings in
multi-ring basins. Continued bombardment causes the crater to become
less and less distinct from its surroundings. Degradation also can be
attributed to lava flows, atmospheric processes such as weathering and
erosion, groundwater processes (sapping), and tectonism. Thus old
craters may exhibit only remnants of the original crater walls
(Planetary Geology for Teachers, 1999).
Crater Mead (Venus) Mead crater, with a diameter of 280
kilometers (174 miles), is the largest impact crater on Venus. The inner
ring is thought to represent the original rim of the crater cavity,
while the outer scarp is thought to be the expression of a ring fault
that has down-dropped the flank terrace (Planetary Geology for Teachers,
1999).
Cratered southern highlands (Mars) The often densely cratered
southern hemisphere of Mars which stands 1 to 3 km above topographic sea
level, and is composed of a very ancient crust which is nearly saturated
with craters, and younger intercrater plains which appear ancient but
have been modified less (Planetary Geology for Teachers, 1999).
Cratered terrain (Mercury) Mercury's major landforms include
impact craters which dominate the landscape, cratered terranes,
widespread intercrater plains, multiring basins, and some smooth plains
that may have been formed by flood basalts. Though an absolute age is
not available now, scientists assume Mercury's heavily cratered regions
probably formed during the same period of intense bombardment that
formed the lunar highlands (Planetary Geology for Teachers,
1999).
Craters with streaks Ray craters with a distinctive radial
pattern of fresh ejecta (Planetary Geology for Teachers, 1999).
Crust The outermost layer of the Earth; that part of the Earth
above the Moho. It represents less than 0.1% of the Earth’s total volume
(Bates and Jackson, 1984).
Crustal upwarps (Mars) Large areas of the Martian surface which
stand high in topographic relief due to the expansion of the crust
resulting from the presence of an underlying mantle plume or hot spot
(Planetary Geology for Teachers, 1999).
Crystal A homogeneous, solid body of a chemical element, compound
or isomorphous mixture, having a regularly repeating atomic arrangement
that may by outwardly expressed by plane faces (Bates and Jackson,
1984).
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Danu Mountains (Venus) A mountain range situated south of Lakshmi
Planum, which shows intense deformation (faulting and folding) of the
planet's crust, similar to deformed rocks seen in mountain belts on
Earth (Planetary Geology for Teachers, 1999).
Dactyl A small asteroid which measures 1.6 x 1.4 x 1.2 km and
orbits a larger asteroid, Ida. Dactyl is the first evidence that
asteroids may have tiny moons (Beatty and Chaikin, 1990).
Deflation basins A topographic basin resulting from the removal
of material from a beach, desert or other land surface by wind action
(Bates and Jackson, 1984).
Deimos The irregularly shaped, dark colored moon of Mars. Deimos
is smaller than its companion moon, Phobos. Both orbit very close to
Mars, have short periods of revolution (1.3 days for Deimos) and are
believed to be captured asteroids (Kuhn, 1998).
Dendritic river systems Networks of interconnecting dry river
beds that exhibited dendritic (from the Greek, meaning "treelike")
drainage patterns characteristic of water-carved channels (Bates and
Jackson, 1984).
Deposit Material of any kind that has accumulated through the
activities of water, wind ice or other agents (Bates and Jackson,
1984).
Desert pavement A residual accumulation of coarse rock fragments
on a surface after the finer material has been blown away by winds.
Also, lag deposits (Bates and Jackson, 1984).
Devana Chasma (Venus) A north-south trough located in the Beta
Regiones highland regions in the equatorial zone (Planetary Geology for
Teachers, 1999).
Differentiated Refers to meteorites that are differentiated,
i.e., they have igneous textures because they were once molten. All
other meteorite types (achondrites, stony-irons and irons) are
undifferentiated (Planetary Geology for Teachers, 1999).
Divergent Boundry A boundary between two crustal plates that are
moving apart, with new oceanic type lithosphere being created in the
seam. Also, accreting plate boundary (Bates and Jackson, 1984).
Domes An uplift or anticlinal structure, circular or elliptical
in outline, in which rocks dip gently away in all directions. Doming
results in extension of the crust above, and leads to predominantly
extensional tectonic features, such as fracture belts, troughs, grabens,
and rifts (an area of extension) (Bates and Jackson, 1984).
Dominant ices (Solar System) Water (H2O) ice,
CO2 ice and NH4 ice (Planetary Geology for
Teachers, 1999).
Double chain A class or structural type of silicate characterized
by the linkage of the SiO4 tetrahedra into linear chains by
the sharing of oxygens. In a double chain or band, e.g. amphiboles, half
the SiO4 tetrahedra share three oxygens and the other half
share two (Bates and Jackson, 1984).
Drumlins A low, smoothly rounded, elongate hill of compact
glacial till, or rarely other kinds of drift, built under the margin of
the ice and shaped by its flow or carved out of an older moraine by
re-advancing ice; its longer axis is parallel to the direction of
movement of the ice (Bates and Jackson, 1984).
Dunes (longitudinal, star, transverse, and barchan) A mound,
ridge, or hill of wind-blown sand, either bare or covered with
vegetation (Bates and Jackson, 1984).
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Eistla Regio (Venus) A region centered at 12.3 degrees north
latitude, 8.3 degrees east longitude, with an area 160 kilometers (96
miles) by 250 kilometers (150 miles). Its prominent circular features
are volcanic domes, 65 kilometers (39 miles) in diameter with broad,
flat tops less than one kilometer (0.6 mile) in height. Sometimes
referred to as "pancake" domes, they represent a unique category of
volcanic extrusions on Venus formed from viscous (sticky) lava. The
cracks and pits commonly found in these features result from cooling and
the withdrawal of lava (Planetary Geology for Teachers, 1999).
Ejecta Material thrown out from and deposited around an impact
crater (Welcome to the Planets, 1995).
Electron The negatively charged, almost mass-less particle that
orbits the nucleus of an atom (Kuhn, 1998).
Element A substance that consists of atoms, each with the same
atomic number (Bates and Jackson, 1984).
Elysium uplift (Mars) A region at the center of a huge
bulge in the Martian surface formed by a series of fluid lava flow
eruptions that carpeted its flanks and slowly built up the high features
we see today, and is evidence for tectonism on Mars. The Elysium uplift
was likely caused by upwelling mantle material (Planetary Geology for
Teachers, 1999).
Enstatite A common rock forming mineral of the orthhopyroxene
group, (Mg,Fe)SiO3. It is isomorphous with hypersthene. It is
an essential constituent of many igneous rocks (Bates and Jackson,
1984).
Eolian features Related to wind deposits and associated effects.
Including wind streaks, sand dunes, ripples, deposits of loess, and
yardangs (Bates and Jackson, 1984).
Eolian systems Pertaining to the wind, esp. said of such deposits
as loess and dune sand, of sedimentary structures such as wind formed
ripple marks, or erosion and deposition accomplished by the wind (Bates
and Jackson, 1984).
Erratic A rock fragment carried by glacial ice, deposited at some
distance from the outcrop from which it was derived, and generally
resting on bedrock of different lithology. Size ranges from pebbles to
house-sized blocks. Also, glacial erratic (Bates and Jackson,
1984).
Escarpment A long, more or less continuous cliff or relatively
steep slope facing in one general direction, produced by erosion or
faulting (Welcome to the Planets, 1995).
Esker A serpentine ridge of roughly stratified gravel and sand
that was deposited by a stream flowing in or beneath the ice of a
stagnant or retreating glacier and was left behind when the ice melted
(Bates and Jackson, 1984).
Extrusive rocks (volcanic) Magma that erupts onto the surface is
called lava. It cools very quickly because the temperature at the
surface is relatively low, and crystals will probably cease growth
because the liquid is quenched. Volcanic glass is a type of quenched
lava, and typical volcanic rocks are rhyolite, basalt, and andesite
(Planetary Geology for Teachers, 1999).
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Fault-bounded troughs A long linear depression defined and
bordered by a crack or break in the crust of a planet along which
slippage or movement can take place (Welcome to the Planets,
1995).
Fault A crack or break in the crust of a planet along which
slippage or movement can take place (Welcome to the Planets,
1995).
Feldspars A group of abundant rock forming minerals of the
general formula: MAl(Al,Si)3O8, where M can be
K,Na,Ca,Ba,Rb,Sr, or Fe. Feldspars are the most widespread of any
mineral group and constitute 60% of the Earth’s crust, they occur in all
types of rock (Bates and Jackson, 1984).
Ferromagnesian Containing iron and magnesium, applied to mafic
minerals, esp. amphibole, pyroxene, biotite and olivine (Bates and
Jackson, 1984).
Flood basalts A term applied to those basaltic lavas that occur
as vast composite accumulations of horizontal or sub-horizontal flows,
which, erupted in rapid succession over great areas, have at times
flooded sectors of a body’s surface on a regional scale; and are
generally thought to be the product of fissure eruptions (Bates and
Jackson, 1984).
Fluvial channels Channels associated with rivers and streams that
are produced by the action of flowing water, e.g. erosion (Bates and
Jackson, 1984).
Fluvial processes Processes pertaining to rivers and streams that
are produced by the action of flowing water, e.g. erosion (Bates and
Jackson, 1984).
Foliation An important texture in metamorphic rocks, caused by
alignment of platy minerals such as mica, or compositional layering. It
is the manifestation of directed stresses that occur within the crust
(Planetary Geology for Teachers, 1999).
Framework silicates A class or structural type of silicate
characterized by the sharing of all four oxygens of the SiO4
tetrahedra with neighboring tetrahedra, and with a Si:O ratio of 1:2.
Quartz, SiO2 is an example (Bates and Jackson,
1984).
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Galileo Galileo Galilei, (1564-1642). Italian mathematician,
astronomer, and physicist. First astronomer to use a telescope to
observe the skies and discoverer of the major (Galilean) moons of
Jupiter, craters on the Moon, the phases of Venus and sunspots. (Kuhn,
1998) (Welcome to the Planets, 1995).
Galileo Spacecraft The Galileo mission consists of two
spacecraft: an orbiter and an atmospheric probe. The probe descended
through the cloud layers of Jupiter and relayed information about the
pressures, chemical compositions, cloud densities, and other data before
it was eventually destroyed by the high temperatures and pressures
(Planetary Geology for Teachers, 1999).
Gaspra An "S-type", main belt asteroid of silicaceous chemical
composition. 951 Gaspra, photographed by the Galileo spacecraft in 1991,
is a generally gray, irregular object measuring 18 x 11 x 19 km. The
surface is heavily cratered and fractured with a dusty regolith similar
to Deimos. Sharp-edged craters and ridges appear bluish while low-lying
areas are reddish (Beatty and Chaikin, 1990).
Geologic history of Mars The early geologic history of Mars is
believed to be similar to that of Mercury and the Moon, however
volcanism persisted well into the last half of solar system history and
may continue today (Planetary Geology for Teachers, 1999).
Geologic history of Mercury (5 stage) 1. Initial planetary
material coalesced form the solar nebula. 2. Heating from
accretion of planetesimals and other space debris. 3. Planetary
differentiation into layers of increasingly denser material from the
surface to the core. 4. Catastrophic impact and stripping away of
much of the surface and the upper part of the mantle. 5. Additional
accretion and formation of a rigid crust through heat loss to
surrounding space (Beatty and Chaikin, 1990).
Geomorphology The study of the external structure, form, and
arrangement of rocks in relation to the development of landforms (Bates
and Jackson, 1984).
Glacial systems The formation, movement and recession of glaciers
or ice sheets (Bates and Jackson, 1984).
Glass beads Small, rounded pieces of silicate glass, thought to
have become airborne during terrestrial impact events, also, tektites
(Bates and Jackson, 1984).
Global escarpment A long, more or less continuous cliff or
relatively steep slope of global proportions, facing in one general
direction, separating two level or gently sloping surfaces, and produced
by erosion and/or faulting (Beatty and Chaikin, 1990).
Globular cluster A spherical group of up to hundreds of thousands
of stars, found in the halo at the margin of galaxies (Kuhn,
1998).
Gneiss A high-grade, metamorphic rock that has experienced
intense recrystallization and segregation of compositional layers
(Planetary Geology for Teachers, 1999).
Golubkina (Venus) A 30.1 kilometer (19 mile) diameter
crater characterized by terraced inner walls and a central peak, typical
of large impact craters on the Earth, the Moon and Mars. The terraced
inner walls take shape late in the formation of an impact crater, due to
the collapse of the initial cavity created by the meteorite impact. The
central peak forms due to the rebound of the inner crater floor. This
crater is named after the Russian sculptor Anna Golubkina (Planetary
Geology for Teachers, 1999).
Graben An elongated, relatively depressed crustal unit or block
that is bounded by faults on its sides (Welcome to the Planets,
1995).
Gravitational potential energy Stored energy in a system
resulting from the force of gravity (Beatty and Chaikin, 1990).
Great Red Spot (Jupiter) A complex storm moving in a
counter-clockwise direction. At the outer edge, material appears to
rotate in four to six days; near the center, motions are small and
nearly random in direction (Beatty and Chaikin, 1990).
Ground ice Wedge-shaped, foliated ice produced in permafrost,
occurring as a vertical or inclined sheet, dike or vein tapering
downward, and measuring form a few mm to as much as 6 meters wide and
from 1 meter to > 30 meters high. It originates by the growth of hoar
frost or by the freezing of water in a narrow crack or fissure produced
by the thermal contraction of permafrost (Bates and Jackson,
1984).
Ground water That part of the subsurface water that is in the
zone of saturation, including underground streams. Loosely, all
subsurface water as distinct from surface water (Bates and Jackson,
1984).
Gula Mons (Venus) A 3 kilometer (1.86 mile) high volcano,
located at approximately 22 degrees north latitude, 359 degrees east
longitude (Planetary Geology for Teachers, 1999).
[H]
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Halides A mineral compound characterized by a halogen such as
fluorine, chlorine, iodine, or bromine as the anion. Example, Halite,
NaCl (Bates and Jackson, 1984).
Halley, Edmond (1656-1742) English astronomer. In 1758, he
accurately predicted the return of a comet previously observed in 1531,
1607, and 1682. The body was subsequently named Halley's Comet (Welcome
to the Planets, 1995).
Herschel, Sir William (1738-1822) British astronomer. He built a
reflecting telescope of superior quality and with it discovered planet
Uranus. He also discovered some of the satellites of Uranus and of
Saturn (Welcome to the Planets, 1995).
Horn A high pyramidal peak with steep sides formed by the
intersecting walls of three or more cirques formed by alpine glaciation
(Bates and Jackson, 1984).
Hornblende The most common mineral of the amphibole group
(Ca,Na)2-3
(Mg,Fe+2,Fe+3,Al)5(Al,
Si)8O22(OH)2. It has a variable
composition, and may contain potassium and appreciable fluorine. It is
commonly black and occurs in distinct monoclinic crystals or in
columnar, fibrous, or granular forms (Bates and Jackson, 1984).
Hubble Space Telescope (HST) A 98 inch, Earth orbiting reflecting
space telescope which is equipped with infrared, x-ray and other
electromagnetic sensors. Named after famous American astronomer, Edwin
Hubble (Kuhn, 1998).
Hummocky Uneven; describing a terrain abounding in irregular
knolls, mounds, or other small elevations (Welcome to the Planets,
1995).
Hydrologic system (Mars) Water cycling during past wet
episodes on Mars would have had many components. A thick atmosphere most
likely carried a substantial amount of water evaporated from lakes and
seas. That water vapor would, in turn, condense into clouds and
eventually precipitate. Rain formed in this way would have created
surface runoff, and much of this water would have percolated into the
ground. Snowfalls might have accumulated to form glaciers, which in turn
would have discharged their meltwaters into glacial lakes. Hydrothermal
circulation, associated perhaps with sites of volcanism, could also have
brought water to the surface from reservoirs deep underground (Planetary
Geology for Teachers, 1999).
Hydrosphere The waters of the Earth, including surface and
subsurface water. All the oceans, snow, ice and glaciers (Bates and
Jackson, 1984).
Hypersthene A common rock forming mineral of the orthopyroxene
group, (Mg,Fe)SiO3. It is isomorphous with enstatite. It is
an essential constituent of many igneous rocks (Bates and Jackson,
1984).
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Ice (dominant Solar System) Water (H2O) ice,
CO2 ice and NH4 ice (Planetary Geology for
Teachers, 1999).
Ice age A loosely used synonym for glacial epoch, or time of
extensive glacial activity (Bates and Jackson, 1984).
Ice shelves A sheet of very thick ice with a level or gently
undulating surface, which is attached to the land along one side but
most of which is afloat and bounded on the seaward side by a steep cliff
(ice front) rising 2 to 50 meters or more above sea level (Bates and
Jackson, 1984).
Iceberg A large, massive piece of floating or stranded glacier
ice of any shape, broken from the front of a glacier into a body of
water. An iceberg has the greater part of its mass (4/5 to 8/9) below
sea level (Bates and Jackson, 1984).
Ida An "S-type", main belt asteroid of silicaceous chemical
composition. 251 Ida exhibits an irregular, heavily cratered surface and
measures 55 x 24 x 20 km making it the largest member of a
compositionally similar group called the Koronis Family. Ida rotates
every 4.6 hours on its axis and was first photographed by the Galileo
spacecraft in 1993. At about 100 km from its center, Ida is orbited by
the small satellite, Dactyl, which measures 1.6 x 1.4 x 1.2 km. Dactyl
is the first evidence that asteroids may have tiny moons. Crater density
on Ida is 5 times that of Gaspra from which it is inferred that Ida is
the older of the two (Beatty and Chaikin, 1990).
Igneous Said of a rock or mineral that solidified from molten or
partly molten material, e.g. from a magma; also applied to processes
related to the formation of such rocks (Bates and Jackson, 1984).
Impact basin A depression formed by the impact of a meteorite,
and also a depression around the orifice of a volcano (Bates and
Jackson, 1984).
Impact craters A depression formed by the impact of an
unspecified projectile, esp. a crater formed on the Earth, planet or
moon surface where the nature of the impacting body is unknown (Bates
and Jackson, 1984).
Impact events An individual bolide (comet, meteorite, or
asteroid) impact and the associated geological, biological and climatic
changes that result (Beatty and Chaikin, 1990).
Impact glass Glassy material produced by a complete or partial
fusion of target rock by the heat generated from the impact of a large
meteorite and occurring in and around the resulting crater (Bates and
Jackson, 1984).
Impact melts During an impact event, a compression wave spreads
outward from the point of impact. Engulfed by the shock wave, the
colliding meteoroid and the surface rocks are melted and partially
vaporized (Beatty and Chaikin, 1990).
Inner core (Earth) The central, solid part of the Earth’s core,
extending from a depth of about 5100 km to the center (6371) of the
Earth; its radius is about 1/3 that of the whole core and is effectively
de-coupled from the mantle due to the molten nature of the surrounding
outer core. Its density is about 12 g/cm3 (Bates and Jackson,
1984).
Intercrater plains (Mercury) Mercury was larger and closer to the
Sun, therefore its surface cooled more slowly. For a long time after the
crust started forming, meteoric debris was able to break through the
soft crust and allow lava to erupt and obliterate older craters. This
resulted in the plains seen today between the craters (Planetary Geology
for Teachers, 1999).
Interferometry A procedure that allows a number of telescopes to
be used as a single, large telescope by taking into account the time
differences at which individual waves from an object strike the
individual telescopes (Kuhn, 1998).
Internal structure (Jupiter) Jupiter is thought to have very
rare, liquid metal hydrogen surrounding its core, which could give the
planet its magnetic field. Gaseous clouds may become dense enough at
Jupiter’s center to support a solid rocky core (Beatty and Chaikin,
1990).
Internal structure (Saturn) The internal structure of Saturn
consists of a gas outer layer with traces of ice, a middle layer of
liquid metal hydrogen, and, possibly a rocky core (Beatty and Chaikin,
1990).
Intrusive rocks (plutonic) Rocks formed beneath the surface where
magma tends to cool slowly and develop large crystals. Mineral growth is
often enhanced by aqueous fluids that can help carry the chemical
components necessary for rapid crystal growth. Common examples of
plutonic rock are granite, diorite, gabbro, anorthosite, and syenite,
with rock names depending on the relative proportions of constituent
minerals and their bulk chemistry (Planetary Geology for Teachers,
1999).
Ion A charged atom or molecule resulting from the atom’s loss or
gain of an electron (Kuhn, 1998).
Ionic bond A chemical bond formed by the electrostatic attraction
between positive and negative ions; for example, NaCl (Beatty and
Chaikin, 1990).
Iron A meteorite consisting essentially of iron with up to 30% of
nickel in solid solution (Bates and Jackson, 1984).
Iron core, Large (Mercury) Mercury's large metallic core,
three-fourths the size of the planet, makes it much denser than the Moon
and the most iron-rich planet in the solar system. Surrounding the
metallic core is a rigid outer shell, or lithospheric mantle, that is
about 500-600km thick (The New Solar System, 1990)
Ishtar Terra (Venus) A highland area in the northern
hemisphere (about the size of Australia) which stands several kilometers
above the average planetary radius. It is separated from the surrounding
rolling uplands by relatively steep flanks, and the western portion is a
vast plateau, Lakshmi Planum, some 2000 kilometers across. Eastern
Isthar contains Maxwell Montes, the highest topographic feature on Venus
(Planetary Geology for Teachers, 1999).
Island arc A curved chain of islands, e.g. the Aleutians, rising
from a deep sea floor and near the continents. Its curve is generally
convex toward the open ocean (Bates and Jackson, 1984).
Isostacy The condition of equilibrium, comparable to floating, of
the units of the lithosphere above the asthenosphere. Also, isostatic
compensation (Bates and Jackson, 1984).
Isotope Atoms of the same element with different numbers of
neutrons in their nuclei. Also, the same atomic number but a different
atomic mass (Beatty and Chaikin, 1990).
[J]
Jovian Of or relating to the planet Jupiter. Also designating the
outer, Jupiter-like gas giants which in addition to Jupiter, include
Saturn, Uranus and Neptune (Kuhn, 1998).
[K]
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Karst A type of topography that is formed over limestone,
dolomite or gypsum by dissolution, and that is characterized by
sinkholes, caves, and underground drainage (Bates and Jackson,
1984).
Kettle lake A body of water occupying a depression in glacial
drift, esp. in outwash and a kame field, formed by the melting of a
detached block of stagnant ice that was buried in the drift. Walden’s
Pond is and example (Bates and Jackson, 1984).
Kinetic energy The energy of motion. Kinetic energy is
transferred by a shock wave that spreads outward from the point of
impact (Beatty and Chaikin, 1990).
Kreep basalts An acronyum for a type of basaltic lunar rock first
found by Apollo 12. The fines and breccia of this lunar basalt are
characterized by an unusually high content of potassium (K), rare earth
elements (REE), phosphorus (P) and other trace elements. The KREEP
basalts are compositionally different form the iron-rich mare
basalts (Bates and Jackson, 1984).
Kuiper Belt A region beyond the orbit of Neptune from which the
short period comets (>200 years) are theorized to originate (Kuhn,
1998).
Kuiper, Gerard Peter (1905-1973) An American astronomer born in
the Netherlands. He studied the origin of the solar system, planetary
atmospheres and proposed the Kuiper Belt as the source of short period
comets (Welcome to the Planets, 1995).
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Lag deposits A residual accumulation of coarse rock fragments on
a surface after the finer material has been blown away by winds. Also,
desert pavement (Bates and Jackson, 1984).
Lakshmi Planum (Venus) A high volcanic plateau situated
nearly 5 kilometers (3 miles) above the mean radius of Venus and
surrounded by mountain belts (ranges), Akna Montes (west), Freyja Montes
(north), Maxwell Montes (east), and Danu Montes (south). Two large
volcanic calderas, Colette and Sacajawea, are located in the center of
Lakshmi Planum and are surrounded by long volcanic flows (Planetary
Geology for Teachers, 1999).
Large Magellanic Cloud Hazy, cloud-like patches in the sky of the
Earth’s southern hemisphere which are gigantic groups of stars forming
separate galaxies (Kuhn, 1998).
Lava Magma that erupts onto the surface (Planetary Geology for
Teachers, 1999).
Lava Channels (Venus) Lava channels extending from hundreds to
thousands of kilometers in length are conspicuous on the Venusian
plains. Simple channels typically show little or no branching. They
include long sinuous forms, termed "canali", and sinuous rilles. Canali
are best preserved in regions of subdued relief. They have a high
width-to-depth ratio and maintain a remarkably constant width over very
long distances. Images reveal the presence of meanders, point bars, cut
banks, and abandoned channel segments (Planetary Geology for Teachers,
1999).
Lava flows A lateral, surficial outpouring of molten lava from a
vent or fissure; also, the solidified body of rock that is so formed
(Bates and Jackson, 1984).
Lavinia Planitia (Venus) A topographic basin consisting of
extensive, probably basaltic, lava flows and could be compared to the
Earth’s ocean basins in respect to extent and composition. Features seen
within the lowlands include broad bowl-like depressions, flood lavas
(similar to the Columbia River Basalts on Earth), lava channels that can
extend for hundreds of kilometers, and compressional ridges (Planetary
Geology for Teachers, 1999).
Limb The apparent outer edge of a lunar or planetary disk
(Welcome to the Planets, 1995).
Lineations Linear topographic features that may depict crustal
structure (Welcome to the Planets, 1995).
Liquid metal hydrogen A liquid metal form of hydorgen which
exists only at high pressures (over 4 million bars) and is theorized to
exist near the core of Jupiter (Planetary Geology for Teachers,
1999).
Lithosphere The solid portion of the Earth, as compared with the
atmosphere and the hydrosphere. In place tectonics, a layer of strength
relative to the underlying asthenosphere. It includes the crust and part
of the upper mantle and is of the order of 100 km in thickness (Bates
and Jackson, 1984).
Loess A blanket deposit of buff-colored calcareous silt,
homogeneous, nonstratified, weakly coherent, porous, and friable. It is
considered to be windblown dust of Pleistocene age (Bates and Jackson,
1984).
Lower mantle (Earth) That part of the mantle that lies
below a depth of about 1000 km and has a density of 4.7
g/cm3, in which the seismic velocity increases slowly with
depth (Bates and Jackson, 1984).
Lowlands (Venus) These large plains consist of extensive,
probably basaltic, lava flows and could be compared to the Earth’s ocean
basins in respect to extent and composition. Features seen within the
lowlands include broad bowl-like depressions, flood lavas (similar to
the Columbia River Basalts on Earth), lava channels that can extend for
hundreds of kilometers, and compressional ridges. The largest lowland
feature is Atalanta Planitia, which is located east of Ishtar Terra
(~165° E Long., 65° N Lat.) and is about the size of the Gulf of Mexico
(Planetary Geology for Teachers, 1999).
Lunar Magma Ocean The outer several hundred kilometers of the
lunar mantle became molten yielding a Lunar Magma Ocean (LMO) that began
to cool and differentiate like a thick intrusion of mafic magma. Dense
ferromagnesian minerals, such as olivine and pyroxene, crystallized and
sank to the deeper mantle. Less dense calcium plagioclase feldspar
minerals accumulated into anorthosite masses (along with minor amounts
of ferromagnesian minerals) that rose and concentrated near the surface.
These masses formed the early lunar crust of which the highland regions
are made (Planetary Geology for Teachers,
1999).
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Magma A 3-phase system of silicate liquid, solid minerals, and
perhaps a vapor phase. It takes on various forms including pods, lenses,
diapirs, veins, or dikes depending on viscosity, density, and the forces
applied to it by surrounding rock (Planetary Geology for Teachers,
1999).
Magnetosphere (Earth) The confines of the Earth’s magnetic
field, modified by the influence of the solar wind. On the sunlit side,
the magnetosphere is nearly hemispherical with a radius ~10 Earth radii
under quiet conditions and ~6 Earth radii during solar storms. Opposite
the sunlit side, the magnetosphere extends in a ‘tail’ of several
hundred Earth radii (Kuhn, 1998).
Main Belt asteroids Asteroids that orbit the Sun at distances
from 2.2 AU to 3.6 AU. This orbital zone between Mars and Jupiter is the
location of most of the known asteroids. Also, asteroid belt (Beatty and
Chaikin, 1990).
Manicougan impact stucture A 70 km diameter impact crater in
Quebec, Canada. The 210 million year old structure has a central peak of
shock-metamorphosed rock, surrounded by a thick layer of frozen impact
melt that pooled on the original crater floor (Beatty and Chaikin,
1990).
Mantle (Earth) The zone of the Earth below the crust and above
the core, it is divided into the upper mantle and the lower mantle, with
a transition zone between (Bates and Jackson, 1984).
Mantle plume A buoyant mass of hot, partially molten mantle
material that rises to the base of the lithosphere. A persistent
pipelike body of hot material moving upward from the planetary mantle
into the crust. Its surface expression may be a hot spot (Welcome to the
Planets, 1995).
Mare A dark, low-lying lunar plain, filled to some depth with
volcanic rocks (Welcome to the Planets, 1995).
Mariner 10 Only one spacecraft, Mariner 10, has ever visited
Mercury. It made three passes near the planet in 1974 and '75. It
snapped pictures of half of the planet's surface, measured temperatures,
and discovered a weak magnetic field. American and European space
agencies are drafting plans for future missions to Mercury, but none
will take place before the next century (Planetary Geology for Teachers,
1999).
Mass extinction The total disappearance of many species or higher
taxon, such that they no longer exist anywhere (Bates and Jackson,
1984).
Mass movement Unit downslope movement of a portion of the land
surface, as in creep, landslide or slip (Bates and Jackson,
1984).
Maxwell Montes (Venus) Maxwell Montes in Ishtar Terra is
the highest peak on Venus. It towers more than 11 kilometers (7 miles)
above the lowland plains
(Planetary Geology for Teachers, 1999).
Mead crater (Venus) Crater Mead, with a diameter of 280
kilometers (174 miles), is the largest impact crater on Venus. The inner
ring is thought to represent the original rim of the crater cavity,
while the outer scarp is thought to be the expression of a ring fault
that has downdropped the flank terrace (Planetary Geology for Teachers,
1999).
Mercury’s landforms Mercury's major landforms include impact
craters which dominate the landscape, cratered terranes, widespread
intercrater plains, multiring basins, and some smooth plains that may
have been formed by flood basalts. Though an absolute age is not
available now, scientists assume Mercury's heavily cratered regions
probably formed during the same period of intense bombardment that
formed the lunar highlands (Planetary Geology for Teachers,
1999).
Mesas A broad, flattop, erosional hill or mountain, commonly
bounded by steep slopes (Bates and Jackson, 1984).
Mesozoic An era of geologic time, from the end of the Paleozoic
to the beginning of the Cenozoic Era, or from about 225 mya to about 65
mya. It includes the Triassic Period (230 mya to 190 mya), the Jurassic
Period (190 mya to 140 mya) and the Cretaceous (140 mya to 65 mya)
(Bates and Jackson, 1984).
Metallic bond A chemically bonded solid that consists of positive
cores of atoms held together by a "sea" of electrons (Beatty and
Chaikin, 1990).
Metamorphic Any rock derived from pre-existing rocks by
mineralogic, chemical and/or structural changes, essentially in the
solid state, in response to marked changes in tempeature, pressure,
shearing stress and chemical environment, generally at depth in the
Earth’s crust (Bates and Jackson, 1984).
Metasomatism Metamorphic rocks formed by the addition or
subtraction of chemical components. Hot, aqueous fluids can be generated
by magma that heats groundwater or gives off primary water. Such
hydrothermal fluids can alter rocks that surround intrusive bodies. This
is how some economic mineral deposits are formed (Planetary Geology for
Teachers, 1999).
Meteorite Any solid object from interplanetary space that has
fallen to the Earth’s surface without being vaporized by frictional
heating during its passage through the atmosphere; a stony or metallic
object large enough to reach the ground. Most meteorites are believed to
be fragments of asteroids and to consist of primitive solid matter
similar to that from which the Earth was originally formed (Bates and
Jackson, 1984).
Meteorite crater An impact crater formed by the falling of
a large meteorite onto a surface (Bates and Jackson, 1984).
Meteoroid Any relatively small fragment of solid material
associated with a meteor and made luminous as a result of friction
during its passage through the Earth’s atmosphere (Bates and Jackson,
1984).
Mica A group of monoclinc minerals of the general formula
(K,Na,C,)(Mg,Fe,Li,Al)2-3(Al,Si)4O10(OH,F)2.
It consists of complex phyllosilicates with perfect basal cleavage,
which split into thin elastic laminae and range from colorless to black
(Bates and Jackson, 1984).
Microcline A white, gray, brick-red or green mineral of the
alkali feldspar group: (KAlSi3O8). It is the fully
ordered, triclinic modification of potassium feldspar and is dimorphous
with orthoclase, being stable at lower temperatures, it usually contains
sodium in minor amounts. Microcline is a common rock forming mineral of
granitic rocks and pegmatites, and is often secondary in orthoclase
(Bates and Jackson, 1984).
Mineral A naturally occurring inorganic element or compound
having an orderly internal structure and characteristic chemical
composition, crystal form, and physical properties (Bates and Jackson,
1984).
Moons Any of the 63 (so far known) smaller objects that revolve
around the planets (Kuhn, 1998).
Moraines A mound or ridge of unstratified glacial drift, chiefly
till, deposited by direct action of glacial ice (Bates and Jackson,
1984).
Morphology The study of structure or form (Welcome to the
Planets, 1995).
Mountain belts A group of mountain ranges exhibiting certain
unifying features, such as similarity in form, structure, and alignment,
and presumably originating from the same general causes. Cf: orogenic
belt, mountain chain (Bates and Jackson, 1984).
Multiring basins Multiring basins have diameters over 300
kilometers and often contain mare lava flows that filled the crater
floor after the crater formation. These craters look like a bulls-eye,
with low ridges radial around the crater (Beatty and Chaikin,
1990).
Muscovite A mineral of the mica group:
KAl2(AlSi3)O10(OH)2. It is
colorless to pale brown, and is a common mineral in gneisses and
schists, in granites and pegmatites, and in may sedimentary rocks, esp.
sandstones (Bates and Jackson, 1984).
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Neutrino An elementary particle that has little or no rest mass
and no charge which carries energy from a nuclear reaction (Kuhn,
1998).
Neutron The
massive nuclear particle with no charge (Kuhn, 1998).
Northern plains (Mars) The northern hemisphere where
volcanic flows surround the largest volcanoes, but elsewhere the plains
are featureless except for craters and mare-like ridges (Planetary
Geology for Teachers, 1999).
Nucleosynthesis The creation of new elements in nuclear reactions
(Kuhn, 1998).
Nucleus (atomic) The central, massive part of an atom consisting
of protons and neutrons (Kuhn, 1998).
Nucleus (comet) The frozen core of a comet which contains almost
the entire cometary mass and is located in the comet's head (Welcome to
the Planets, 1995).
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Oceanic crust The oceanic crust underlies the ocean basins and is
equivalent to the sima. The oceanic crust is about 5 to 10 km thick, has
a density of 3.0 g/cm3, and compressional seismic wave
velocities exceeding 6.2 km/sec (Bates and Jackson, 1984).
Olivine A green or brown orthorhombic mineral,
(Mg,Fe)2SiO4. It consists of the isomorphous
solid-solution series forsterite-fayalite (Bates and Jackson,
1984).
Olivine phenocrysts The relatively large and ordinarily
conspicuous crystal of the mineral olivine generated early in
prophyritic igneous rocks (Bates and Jackson, 1984).
Orthoclase A white, pink or gray mineral of the alkali feldspar
group: (KAlSi3O8). It is the partly ordered,
monoclinic modification of potassium feldspar and is dimorphous with
microcline, being stable at higher temperatures; it usually contains
sodium in minor amounts. Orthoclase is a common rock forming mineral; it
occurs esp. in granites, acid igneous rocks and crystalline schists, and
is usually perthitic (Bates and Jackson, 1984).
Outer core (Earth) The upper zone of the Earth’s core,
extending from a depth of 2900 km to 5100 km, and including the
transition zone. It is presumed to be liquid because it sharply reduces
compressional wave velocities and does not transmit shear waves. Its
density ranges from 9 to 11 g/cm3 (Bates and Jackson,
1984).
Outflow channels (Mars) Structures are more than 200
kilometers wide and can stretch for 2,000 kilometers or more. These
channels emanate from what is called chaotic terrain, regions of
fractured, jumbled rocks that apparently collapsed when groundwater
suddenly surged outward (Planetary Geology for Teachers, 1999).
Outwash Sand and gravel deposited by meltwater streams in front
of the end moraine to the margin of an active glacier (Bates and
Jackson, 1984).
Ovda Regio (Venus) The tectonic fabric of this region trends
predominantly east-west. The large radar-dark areas are probably
tectonically formed basins that have been filled in by fluid lava flows,
thus presenting a smooth surface to the Magellan radar system (Planetary
Geology for Teachers, 1999)
Oxides A mineral compound characterized by the linking of oxygen
with one or more metallic elements, such as Cuprite, Cu2O
(Bates and Jackson, 1984).
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Paleozoic An era of geologic time, from the end of the
Precambrian to the beginning of the Mesozoic Era, or from about 570 mya
to about 225 mya (Bates and Jackson, 1984).
Patera A shallow crater with a scalloped, complex edge (Welcome
to the Planets, 1995).
Patterned ground A group term for the more or less symmetrical
forms such as circles, polygons, nets, steps, and stripes that are
characteristic of, but not necessarily confined to, surficial material
subject to intensive frost action (Bates and Jackson, 1984).
Peak-ring craters A central uplift characterized by a ring of
peaks rather than a single peak; peak rings are typical of larger
terrestrial craters above about 50 kilometers (30 miles) in diameter
(Planetary Geology for Teachers, 1999).
Perigee The point in the orbit of an Earth satellite where it is
closest to the Earth (Kuhn, 1998).
Perihelion The point in the path of a planet, asteroid, comet, or
other body that is closest to the sun (Welcome to the Planets,
1995).
Permafrost Permanently frozen soil or subsoil, occurring in
arctic, sub-arctic, and alpine regions. Its thickness ranges from 30 cm
to > 1000 meters, and it underlies about 1/5 of the Earth’s land area
(Bates and Jackson, 1984).
Phanerozoic That part of geologic time represented by rocks in
which the evidence of life is abundant, and includes the Cambrian and
later time (Bates and Jackson, 1984).
Phlogopite A magnesium rich mineral of the mica group:
K(Mg,Fe)3AlSi3O10(OH,F)2. It
is yellowish brown to brownish red and usually occurs in crystalline
limestones as a result of dedolomization (Bates and Jackson,
1984).
Phobos The irregularly shaped, dark colored moon of Mars. Phobos
is larger than its companion moon Deimos. Both orbit very close to Mars,
have short periods of revolution (0.3 days for Phobos) and are believed
to be captured asteroids (Kuhn, 1998).
Photon The smallest possible amount of electromagnetic energy of
a particular wavelength. This bundle or quanta of energy is called a
photon (Kuhn, 1998).
Photosphere The visible "surface" of the Sun with temperatures of
about 5800 K and an average thickness of 400 km. The part of the solar
atmosphere that radiates light into space (Kuhn, 1998).
Physical weathering The breaking down of rocks by mechanical
processes into pieces that get smaller and smaller until they may
eventually become sand, silt, or dust-sized particles (Planetary Geology
for Teachers, 1999).
Plagioclase A group of triclinic feldspars of general formula:
(Na,Ca)Al(Si,Al)Si2O8. At high temperatures it
forms a complete solid-solution series from Albite
(NaAlSi3O8) to Anorthite
(CaAl2Si2O8). The series is subdivided
and named according to the mole fraction of the Anorhtite component.
Plagioclase minerals are among the most common rock forming minerals
(Bates and Jackson, 1984).
Planet Any of the nine (?) so far known, large objects that
revolve around the Sun. The designation of Pluto as a planet is in
dispute among astronomers (Kuhn, 1998).
Planetary differentiation The heat driven process whereby planets
develop concentric layers of differing composition based on the density
of the materials involved, with heavier elements sinking toward the core
and lighter elements remaining near the surface (Planetary Geology for
Teachers, 1999).
Plate tectonics A theory of global crustal displacement in which
the lithosphere is divided into a number of plates whose pattern of
horizontal movement is that of torsionally rigid bodies that interact
with one anther at their boundaries, causing seismic and volcanic
activity along the boundaries (Bates and Jackson, 1984).
Plateau Any comparatively flat area of great extent or elevation
(Welcome to the Planets, 1995).
Plutonic rocks (intrusive) Rocks formed beneath the surface where
magma tends to cool slowly and develop large crystals. Mineral growth is
often enhanced by aqueous fluids that can help carry the chemical
components necessary for rapid crystal growth. Common examples of
plutonic rock are granite, diorite, gabbro, anorthosite, and syenite;
the rock names depend on the relative proportions of constituent
minerals and the bulk chemistry (Planetary Geology for Teachers,
1999).
Polar dune fields (Mars) A vast "sea" of sand dunes
surrounds the north polar cap. The dunes are classic forms known as
barchan dunes, small, crescent-shaped hills, and transverse dunes, with
ridges that resemble coalesced barchans. These dunes are similar in size
and shape to familiar sand dunes found in desert regions on Earth. These
two varieties form from winds that persistently come from a single
direction (in this case, from the southwest) (Planetary Geology for
Teachers, 1999).
Polar ice caps (Mars) Stacks of layered sediments and ice
which are at least 4-6km thick in the north and 1-2km thick in the
south. Cratered plains surround the ice caps and seem to extend beneath
them, indicating that the ice covers the older craters and is,
therefore, one of the youngest features on the planet. During the
Martian winter, the ice caps grow in extent and are covered with
CO2 frost and ice. The summertime brings with it receding ice
caps and sublimation of the CO2 ice (Planetary Geology for
Teachers, 1999).
Polymorph The characteristic of a chemical substance to
crystallize in more than one form, e.g. rhombic and monoclinic sulfur
(Bates and Jackson, 1984).
Proterozoic The entire Precambrian ranging from about 4500 mya to
570 mya and includes the Hadean and the Archean (Bates and Jackson,
1984).
Proton The massive, positively charged particle in the nucleus of
an atom (Kuhn, 1998).
Pulsar A celestial object of small angular size that emits pulses
of radio waves with a regular period between about 0.03 and 5 seconds
(Kuhn, 1998).
Pyroxene A group of the common rock forming minerals with the
general formula, ABSi2O6, where A is chiefly Mg,
Fe+2, Ca or Na, and B is Mg, Fe+2 or Al (Bates and
Jackson, 1984).
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Quartz Crystalline silica, an important rock forming mineral,
SiO2. It is, next to feldspar, the most common mineral,
occurring either in transparent hexagonal crystals or in crystalline or
cryptocrystalline masses (Bates and Jackson, 1984).
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Radiative Zone The inner 70% of the Sun’s radius where heat from
the fusion reaction is radiated toward the surface at temperatures of
1.5 x 107 K at the base of the zone to temperatures of 1.5 x
106 K at the top of the zone (Kuhn, 1998).
Radiation The
transfer of heat by electromagnetic waves (Kuhn, 1998).
Radiogenic heating Thermal energy resulting from the decay of
radioactive isotopes. Long-lived nuclides are still present in the Earth
and other planetary bodies, although in lower abundance than when the
Solar System formed. This allows for sustained long-term heating during
planetary evolution (Planetary Geology for Teachers, 1999).
Rampart craters (Mars) Impact features characterized by a
mud-like flow of overlapping lobes out and away from the crater caused
when the heat and pressure of an impact fluidized the local ground water
or ground ice that was trapped within the Martian surface (Planetary
Geology for Teachers, 1999).
Refractory minerals Minerals that can resist high temperatures,
also minerals which exhibit high melting points (Bates and Jackson,
1984).
Regolith The fragmented and unconsolidated rock material, whether
residual or transported, that nearly everywhere forms the surface of the
land and overlies the bedrock. It includes rock debris of all kinds
(Bates and Jackson, 1984).
Relief The maximum regional difference in elevation (Bates and
Jackson, 1984).
Rhea Mons (Venus) A large shield volcano (similar to
Hawaii or Olympus Mons) (Planetary Geology for Teachers, 1999).
Rift valley An elongated valley formed by the depression of a
block of the planet's crust between two faults or groups of faults of
approximately parallel strike (Bates and Jackson, 1984).
Rille (Moon) One of several trench-, or crack-like valleys up to
several hundred km long and 1-2 km wide commonly occurring on the Moon's
surface (Welcome to the Planets, 1995).
Rings A thin, disk-like accumulation of very small grains of
rock, ice and ice covered rock which probably originated with the tidal
force induced breakup of nearby moons. The rings lie within the Roch
limit of the planet and rotate according to Kepler’s laws (Planetary
Geology for Teachers, 1999).
Ripples Formations in fine-grained sediment caused by the
movement of water or wind over a depositional surface. They can be
asymmetrical indicating flow direction, or they can be fairly
symmetrical indicating an oscillating current (Planetary Geology for
Teachers, 1999).
Rock forming minerals Said of those minerals than enter into the
composition of rocks, and determine their classification. The more
important rock forming minerals include quartz, feldspars, micas,
amphiboles, pyroxenes, olivine, calcite and dolomite (Bates and Jackson,
1984).
Roche limit The Roche limit was first described by Edouard Roche
in 1848. The Roche limit is the closest distance an object can come to
another object without being pulled apart by tidal forces. If a planet
and a moon have identical densities, then the Roche limit is 2.446 times
the radius of the planet. A large moon orbiting inside the Roche limit
will be destroyed. The Earth's Roche limit is 18,470 km (11,470 miles).
If our Moon ever ventured within this Roche limit, it would be pulled
apart by tidal forces and the Earth would have rings. The four gaseous
outer planets have their ring systems inside of their respective Roche
limit (Planetary Geology for Teachers, 1999).
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Sand sea A very large sand mass; an erg. From a Hamitic
word areg or ergh for such a sand mass in the Sahara
(Bates and Jackson, 1984).
Sapping Spring fed channels that are created when soft sediment
layers are removed by underlying water erosion (Planetary Geology for
Teachers, 1999).
Scarp A cliff or steep slope of some extent that may form a
marked topographic boundary (Welcome to the Planets, 1995).
Schiaparelli Giovanni Virginio Schiaparelli (1835-1910). Italian
astronomer at the Milan Observatory who reported markings on Mars which
he called "canali" (Welcome to the Planets, 1995).
Schist A foliated, metamorphic rock that usually contains micas
oriented sub-parallel to one another (Planetary Geology for Teachers,
1999).
Sea ice Any form of ice originating from the freezing of sea
water, thus excluding icebergs (Bates and Jackson, 1984).
Sediment Generally, solid, fragmented material transposrted and
deposited by wind, water, or ice, chemically precipitated from solution,
or secreted by organisms, and that forms layers of loose, unconsolidated
form, e.g. sand mud and till. Solid material that has settled down from
a state of suspension in a liquid (Bates and Jackson, 1984).
Sedimentary A layered rock resulting from the consolidation of
sediment, e.g. a clastic rock such as sandstone, a chemical rock such a
salt, or an organic rock such as coal. Usually includes pyroclastic
rocks, such as tuff (Bates and Jackson, 1984).
Shearing The motion resulting from stresses that cause or tend to
cause contiguous parts of a body to slide relatively to each other
(Welcome to the Planets, 1995).
Shepherd satellites (moons) A shepherd moon is a satellite that
constrains the extent of a planetary ring through gravitational forces
(Planetary Geology for Teachers, 1999).
Shield A large region of exposed basement rocks, commonly with a
very gently convex surface, surrounded by sediment covered platforms;
e.g. Canadian Shield. Shield rocks are usually Precambrian in age (Bates
and Jackson, 1984).
Shield volcano A broad volcanic cone with gentle slopes
constructed of successive nonviscous, mostly basaltic, lava flows
(Welcome to the Planets, 1995).
Sif Mons (Venus) A large shield volcano (similar to Hawaii
or Olympus Mons). Its dark central caldera, which may contain pools of
lava, is surrounded by extensive flow features that seem to cascade down
its flanks. The volcano has a diameter of 300 kilometers (180 miles) and
a height of 2 kilometers (1.2 miles) (Planetary Geology for Teachers,
1999).
Silicates A compound whose crystal structure contains
SiO4 tetrahedra, either isolated or joined through one or
more of the oxygen atoms to form groups, chains, sheets, or three
dimensional structures with metallic elements (Bates and Jackson,
1984).
Silicic volcanism Said of silica rich igneous rocks or magma,
with silica contents > 65% (Bates and
Jackson, 1984).
Single chains A class or structural type of silicate
characterized by the linkage of the SiO4 tetrahedra into
linear chains by the sharing of oxygens. In a simple chain, e.g.
pyroxenes, two oxygens are shared (Bates and Jackson, 1984).
Single element minerals A mineral composed of a single substance
that cannot be decomposed into other substances except by radioactive
decay (Bates and Jackson, 1984).
Sinkholes A circular depression in a karst area. Its drainage is
subterranean, its size is measured in meters to tens of meters, and it
is commonly funnel shaped (Bates and Jackson, 1984).
Slumping A landslide that results from the downward sliding of
rock debris as a single mass, usually with a backward rotation relative
to the slope along which the movement takes place (Welcome to the
Planets, 1995).
Smooth plains (Mercury) (Volcanic or ejecta?) The smooth plains
seen on Mercury resemble lunar maria and are likewise, sparsely
cratered, but may have formed from different processes than those on the
Moon. Mercury's smooth plains might have been caused by large amounts of
ejecta from the impacts that cratered the surface and formed the Caloris
Basin. On the other hand, a volcanic origin is possible and would liken
Mercury's plains to the Moon's maria (Planetary Geology for Teachers,
1999).
SNC meteorites Rare achondrites about 1.3 billion years old
believed to be pieces of Mars. They are classified according to the
original group of specimens used to chemically and lithologically
suggest a Martian origin (Beatty and Chaikin, 1990).
SNC meteorites General name for three groups of meteorites with
relatively young ages (slightly over 1 billion years old) that probably
came from Mars. The groups are the Shergottites, Nakhlites, and
Chassigny (Bates and Jackson, 1984).
Solar energy Thermal energy generated by the fusion reaction of
the Sun (Kuhn, 1998).
Solar Prominences The eruption of solar material beyond the disk
of the Sun (Kuhn, 1998).
Solid solution A single crystalline phase that may be varied in
composition within finite limits without the appearance of an additional
phase (Bates and Jackson, 1984).
Spectroscopy The use of an instrument that produces an array of
visible light ordered according to its constituent wavelengths or colors
(Kuhn, 1998).
Spicules A narrow jet of gas that is part of the chromosphere of
the Sun and extends upward into the corona (Kuhn, 1998).
Spin-orbit coupling/ orbital resonance For many decades,
scientists thought the same side of Mercury always faced the Sun. But in
1965, astronomers discovered that Mercury completes three full turns on
its axis for every two orbits around the Sun. Because of this motion, we
see the same side of Mercury each time the planet comes closest to
Earth. It is the only planet in our solar system with an
orbital:rotational resonance ratio of 2:3. This resonance ratio is
caused by Mercury’s mass not being evenly distributed throughout the
planet. One side is more massive than the other. Because of this, the
Sun exerts a torque (a turning force) on the planet, especially at
perihelion. After countless revolutions this has resulted in the
rotational period of the planet being coupled with its revolution period
(Planetary Geology for Teachers, 1999).
Spokes (Saturn) Faint, dark areas perpendicular to the rings that
seem to grow and shrink. Little is known about the spokes, but they may
be charged particles that float above the actual ring plain (Planetary
Geology for Teachers, 1999).
Stable platform The part of a continent that is covered by
flat-lying or gently tilted sedimentary rocks, underlain by a complex of
rocks that were consolidated during earlier deformations. The platform
is part of the craton (Bates and Jackson, 1984).
Stony A general name for meteorites consisting largely or
entirely of silicate minerals (chiefly olivine, pyroxene and
plagioclase). Stony meteorites resemble ultramafic rocks in composition,
and they constitute more than 90% of meteorites seen to fall (Bates and
Jackson, 1984).
Stony-irons As their name implies, the stony-irons are comprised
of differentiated igneous silicates plus iron and nickel metal. They are
fairly rare (~1% of falls and ~5% of finds) and thus are valuable to
scientists as well as collectors. The stony-irons provide a glimpse of
the region within a planetary body near the core-mantle boundary where
metallic core components have not entirely separated from the silicate
mantle (Bates and Jackson, 1984).
Structurally bonded water Water molecules held within the
geometric pattern of crystal lattices. Amphibole is an example. The
water held between the layers of atoms in sheet silicates such as
smectite is termed interstitial water (Bates and Jackson,
1984).
Subduction zone A long, narrow belt in which one lithospheric
plate descends beneath another usually of lower density, e.g. along the
Peru-Chile trench (Bates and Jackson, 1984).
Sulfates A mineral compound characterized by the sulfate radical,
SO4 (Bates and Jackson, 1984).
Sulfides A mineral compound characterized by the linking of
sulfur with a metal, such as Galena, PbS (Bates and Jackson,
1984).
Sunspots A magnetically induced feature of the photosphere that
is temporarily cool and dark compared to surrounding regions (Kuhn,
1998).
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Tarns A small, deep, commonly circular glacial lake occupying a
cirque; it is fed by runoff from the surrounding slopes and dammed by a
lip of bedrock or by a small moraine (Bates and Jackson, 1984).
Tectonic Relating to the deformation of the crust of a moon or
planet, the forces involved in or producing such deformation, and the
resulting forms (Welcome to the Planets, 1995).
Tektites Small, rounded pieces of silicate glass, thought to have
become airborne during terrestrial impact events (Bates and Jackson,
1984).
Terminator The line separating the illuminated and unilluminated
parts of a celestial body; the dividing line between day and night as
observed from a distance (Beatty and Chaikin, 1990).
Terrestrial Belonging to the class of planets that are similar to
the Earth in density and composition (i.e. Mercury, Venus, and Mars)
(Welcome to the Planets, 1995).
Tesserae (Venus) Tesserae terrain, which was first detected by
the Soviet Venera 15 and 16 spacecraft in the early 1980s, is
characterized by complex intersecting ridges and grooves. This terrain
may have been formed by large blocks of material sliding and collapsing
down slopes, pulled by the force of gravity. In the extremely
high-temperature Venus environment, rock can behave more like a fluid,
unlike the rigid behavior of rocks found on Earth (Planetary Geology for
Teachers, 1999).
Tetrahedral A crystal form in the isometric system, having four
faces each with equal intercepts on all three axes (Bates and Jackson,
1984).
Tharsis uplift (Mars) The Tharsis region is at the center of a
huge bulge in the surface that is over 4000 km across and 10 km high.
Huge shield volcanoes dominate the Tharsis region, including Olympus
Mons on the northwest flank, the largest shield volcano in the solar
system. The Tharsis uplift was likely caused by upwelling mantle
material and is evidence for tectonism on Mars (Planetary Geology for
Teachers, 1999).
Theia Mons (Venus) A large shield volcano which lies in
the southern part of the Dvana Chasam rift valley (Planetary Geology for
Teachers, 1999).
Thermal energy Energy associated with or pertaining to the heat
derived from planetary processes such as gravitational collapse, solar
radiant energy, radioactive decay and impactor accretion (Beatty and
Chaikin, 1990).
Thermokarst An irregular land surface containing cave-in lakes,
bogs, caverns, pits and other small depressions formed in a permafrost
region by the melting of ground ice, in exterior appearance, it
resembles uneven karst topography formed by the solution of limestone
(Bates and Jackson, 1984).
Thrust faults A fault with a dip of 45°
or less over much of its extent, on which the hanging wall appears to
have moved upward relative to the footwall. Horizontal compression
rather than vertical displacement is its characteristic feature. (Bates
and Jackson, 1984).
Tick (Venus) A type of volcano. About 65.6 kilometers (41
miles) across at the base, this volcano has a flat, concave summit 34.8
kilometers (22 miles) in diameter. The sides of the volcano are
characterized by radiating ridges and valleys. The rim of the volcano to
the west appears to have been breached by dark lava flows that emanated
from a shallow summit pit 5.4 kilometers (3.4 miles) in diameter and
traveled west along a channel. A series of coalescing, collapsed pits 2
to 10 kilometers (1.2 to 6.2 miles) in diameter is 10 kilometers (6.2
miles) west of the summit rim (Planetary Geology for Teachers,
1999).
Tidal heat The frictional heating of a satellite’s interior
caused by repeated flexure induced by the gravitational field of its
parent planet or other nearby more massive object (Planetary Geology for
Teachers, 1999).
Transform (strike-slip) A special variety of strike/slip fault,
along which the displacement suddenly stops or changes form. Many
transform faults are associated with mid-oceanic ridges, where the
actual slip is opposite from the apparent displacement across the fault.
Also, a plate boundary that ideally shows pure strike/slip displacement
(Bates and Jackson, 1984).
Transition zone (Earth) A region with in the upper mantle
bordering the lower mantle at a depth of 410 to 1000 km, characterized
by a rapid increase in density of about 20% and an increase in seismic
wave velocities (Bates and Jackson, 1984).
Transport The movement of sediment by natural agents (such as
flowing water, ice, wind or gravity) either as solid particles or in
solution, from one place to another (Bates and Jackson, 1984).
Tritium An isotope of hydrogen with 2 neutrons and 1 proton in
the nucleus, designated by the symbol 3H (Beatty and Chaikin,
1990).
Trough A long linear depression (Welcome to the Planets,
1995).
T-tauri stage The pre-main sequence stage in the development of
certain stars characterized by rapid and erratic changes in brightness.
Planetesimals and planets form during the T-tauri stage (Kuhn,
1998).
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Undifferentiated (meteorites) Resembling Earth rocks, the stones
are primitive, i.e., they are made up of primordial Solar System
material. Primitive stones are chondrites, the class that makes up most
of the meteorites that fall to Earth (~87% of falls and ~52% of finds).
Chondrites are so-called because of the presence of small round
chondrules, which are typically ~ 1 mm diameter and appear to be
material condensed from the primordial solar nebula (Beatty and Chaikin,
1990).
Uplands and highlands (Venus) Uplands represent a
transition of terrain from the lowland plains to the highlands. Doming
of the lithosphere implies large upwelling thermal plumes from the
mantle that are possibly responsible for creating these uplands. Doming
resulted in extension of the crust above, and led to predominantly
extensional tectonic features, such as fracture belts, troughs, grabens,
and rifts. The best example of an upland dome is Beta Regio, located
around 280° E. longitude and 30° N. latitude. This region is 2500
kilometers across and contains a huge shield volcano, numerous
crisscrossing faults, and several circular coronae (Planetary Geology
for Teachers, 1999).
Upper mantle (Earth) The part of the mantle which lies
above a depth of about 1000 km and has a density of 3.40
g/cm3, in which P-wave velocity increases from about 8 to 11
km/sec with depth and S-wave velocity increases from about 4.5 to 6
km/sec with depth. It is presumed to be peridotitic in composition and
is sometimes referred to as the asthenosphere (Bates and Jackson,
1984).
U-shaped valley A deep, steep-sided through leading down from a
cirque, and excavated by an alpine glacier that has widened, deepened,
and straightened a preglacial river valley; e.g. Yosemite Valley,
California (Bates and Jackson, 1984).
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Vent An opening or fissure in a planet's surface through which
volcanic material erupts (Welcome to the Planets, 1995).
Viscosity A measure of resistance to flow (Welcome to the
Planets, 1995).
Volatile elements A chemical element that exists in a gaseous
state at relatively low tempertures (Bates and Jackson, 1984).
Volcanic glass Natural glass produced by the cooling of molten
lava, or some liquid fraction of it, too rapidly to permit
crystallization. Examples are obsidian, pitchstone, tachylyte, and the
glassy groundmass of many extrusive rocks (Bates and Jackson,
1984).
Volcanic plains (Mars) Basaltic lava plains are the most
widespread and voluminous features on Mars, covering over 60 percent of
its surface. The plains have been compared to the huge flood basalts on
the Earth and the lunar Maria, but are much more extensive (Planetary
Geology for Teachers, 1999).
Volcanic plains (Venus) Basaltic lava plains are the most
widespread and voluminous features on Venus. The plains have been
compared to the huge flood basalts on the Earth and the lunar Maria, but
are much more extensive (Planetary Geology for Teachers, 1999).
Volcanic rocks (extrusive) Magma that erupts onto the surface is
called lava. It cools very quickly because the temperature at the
surface is relatively low, and crystals will probably cease growth
because the liquid is quenched. Volcanic glass is a type of quenched
lava, and typical volcanic rocks are rhyolite, basalt, and andesite
(Planetary Geology for Teachers, 1999).
Volcanic shields A volcano in the shape of a flattened dome,
broad and low, built by flows of very fluid lava (Bates and Jackson,
1984).
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Weathering The destructive processes by which rocks are changed
in response to exposure to atmospheric agents at or near the Earth’s
surface, with little or no transport of the loosened or altered
materials (Bates and Jackson, 1984).
Wind streaks Dark and light streaks thought to be caused by the
removal of a thin veneer of dust, revealing a darker surface beneath
(Planetary Geology for Teachers, 1999).
Wrinkle ridges (Moon) A sinuous, irregular, segmented,
apparently smooth elevation occurring within the borders of a mare
region of the Moon’s surface characterized by dike-like outcrops,
crest-top craters and longitudinal rifts. Wrinkle ridges are up to 35 km
wide and 100 m high, and may extend for hundreds of kilometers. The
likely originate in fissure eruptions or from volcanic activity along
fractures (Planetary Geology for Teachers, 1999).
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Yardangs A long, irregular, sharp-crested, undercut ridge between
two round-bottomed troughs, carved on a plateau or sheltered plain in a
desert region by wind erosion, and consisting of soft but coherent
deposits in the direction of the dominant wind, and may be up to 6
meters high and 40 meters wide (Gray et al., 1974).
[Z]
Zones (Jupiter) Thick rotating clouds swirl around the
planet, blowing in opposite directions in adjacent bands. The lighter
colored bands are called zones (Planetary Geology for Teachers,
1999).
References
Bates, R.L. and Jackson, J.A., editors, 1984, Dictionary of
geologic terms, (third edition), American Geologic Institute: New
York, Anchor Books, 571 p.
Beatty, J.K. and Chaikin, A., editors, 1990, The new solar system,
(third edition): Massachusetts, Sky Publishing Corp., 326 p.
Gray, M., McAfee Jr., R. And Wolf, C.L., editors, 1974, Glossary of
geology: Virginia, American Geologic Institute, 805 p.
Kuhn, K.F., 1998, In quest of the universe (second edition):
Massachusetts, Jones and Bartlett, 568 p.
Planetary Geology for Teachers, 1999, Idaho State University:
http://wapi.isu.edu/Geo_Pgt/index.htm
Welcome to the Planets, 1995, California Institute of Technology:
http://pds.jpl.nasa.gov/planets/welcome.htm. |