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| Rocks From Outer Space! |
Stony meteorites
Chondrites (85.7%)
Carbonaceous
Enstatite
Achondrites (7.1%)
HED group
SNC group
Aubrites
Ureilites
Stony iron meteorites (1.5%)
Pallasites
Mesosiderites
Iron meteorites (5.7%)
Stony-iron meteorites are composed of approximately 50% nickel-iron and 50% silicate material. They make up only
1 to 2% of all meteorites. There two large subgroups:
Pallasites are composed of olivine crystals set in a nickel-iron matrix. They are believed to form at the core-mantle
boundary of a large asteroid. When cut and polished, they are among the most beautiful of meteorites.
Mesosiderites are a mixture of metal grains, pyroxene, olivine, and plagioclas. It is believed that mesosiderites are
formed when two asteroids, one metal-rich and the other silicate-rich, collide in a violent impact.
Iron meteorites are composed almost entirely of nickel-iron. They often have mineral inclusions and are believed to
originate from the core of large asteroids. Iron meteorites are often grouped into three large categories, based upon
the chemical composition and structure:
Octahedrite iron meteorites contain about 7 to 10% nickel. When sliced and etched with acid, they display bands
call "widmanstatten" bands. A further subdivision of octahedrites is made based upon the width of the bands: fine,
medium, coarse, and coarsest. The bands narrows with increasing nickel content.
Hexahedrite iron meteorites contain a relatively low amount of nickel (approximately 6% or less) and when etched
with acid, show very thin lines called "Neumann lines" which have a hexahedral structure.
Ataxite iron meteorites are the highest in nickel content (approximately 16% or more) and show no structure when
etched with acid.
A "fall" means the meteorite was witnessed by someone as it fell from the sky. A "find" means the meteorite was not
witnessed and the meteorite was found after the fact. About 33% of the meteorites are witnessed falls.
A very large number of meteoroids enter the Earth's atmosphere each day amounting to more than a hundred tons of
material. But they are almost all very small, just a few milligrams each. Only the largest ones ever reach the surface to
become meteorites. The largest found meteorite,Hoba, in Namibia, weighs 60 tons.
The average meteoroid enters the atmosphere at between 10 and 70 km/sec. All but the very largest are quickly
decelerated to a few hundred km/hour by atmospheric friction and hit the Earth's surface with very little fanfare.
However meteoroids larger than a few hundred tons are slowed very little; only these large (and fortunately rare) ones
make craters.
A good example of what happens when a small asteroid hits the Earth is Barringer Crater (a.k.a. Meteor Crater) near
Winslow, Arizona. It was formed about 50,000 years ago by an iron meteor about 30-50 meters in diameter. The crater
is 1200 meters in diameter and 200 meters deep. About 120 impact craters have been identified on the Earth, so far...
Meteorites have proven difficult to classify, but the three broadest groupings
are stony, stony iron, and iron. The most common meteorites are chondrites,
which are stony meteorites. Radiometric dating of chondrites has placed them
at the age of 4.55 billion years, which is the approximate age of the solar
system. They are considered pristine samples of early solar system matter,
although in many cases their properties have been modified by thermal
metamorphism or icy alteration.
Some scientists have suggested that the different properties found in various
chondrites suggest the location in which they were formed. Enstatite
chondrites contain the most refractory elements and are believed to have
formed in the inner solar system. Ordinary chondrites, being the most
common type containing both volatile and oxidized elements, are thought to
have formed in the inner asteroid belt.
Carbonaceous chondrites, which have the highest proportions of volatile
elements and are the most oxidized, are thought to have originated in even
greater solar distances.
Achondrites are also stony meteorites, but they are considered reprocessed
matter. They are formed by melting and recrystallization on or within meteorite
parent bodies; as a result, achondrites have distinct textures and
mineralogies indicative of igneous processes.
are stony, stony iron, and iron. The most common meteorites are chondrites,
which are stony meteorites. Radiometric dating of chondrites has placed them
at the age of 4.55 billion years, which is the approximate age of the solar
system. They are considered pristine samples of early solar system matter,
although in many cases their properties have been modified by thermal
metamorphism or icy alteration.
Some scientists have suggested that the different properties found in various
chondrites suggest the location in which they were formed. Enstatite
chondrites contain the most refractory elements and are believed to have
formed in the inner solar system. Ordinary chondrites, being the most
common type containing both volatile and oxidized elements, are thought to
have formed in the inner asteroid belt.
Carbonaceous chondrites, which have the highest proportions of volatile
elements and are the most oxidized, are thought to have originated in even
greater solar distances.
Achondrites are also stony meteorites, but they are considered reprocessed
matter. They are formed by melting and recrystallization on or within meteorite
parent bodies; as a result, achondrites have distinct textures and
mineralogies indicative of igneous processes.
| Meteorites for Sale Pages Click on name for link to page |
Nantan Iron Meteorite Octahedrite |
| Sikhote-Alin Octahedrite |
| Vaca Muerta Stony Iron Mesosiderite |
| Campo del Cielo Iron Meteorite Octahedrite |
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