Meteorites have proven difficult to classify, but the three broadest groupings are stony, stony iron, and iron.

meteor

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.

Animated moving meteor in sky

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 for Sale Pages

Sikhote-Alin
Sikhote-Alin
Sikhote-Alin Sikhote-Alin

Sikhote-Alin

Octahedrite

Russia

Campo del Cielo
Campo del Cielo
Campo del Cielo Campo del Cielo

Campo del Cielo

Iron Meteorite Octahedrite

Argentina

Nantan
Nantan
Nantan Nantan

Nantan

Iron Meteorite Octahedrite

China

Vaca Muerta

Vaca Muerta

Stony Iron Mesosiderite

Chile

Mundrabilla

Mundrabilla

Iron Meteorite Octahedral Coarse

Australia

Henbury

Henbury

Iron Meteorite Octahedrite

Australia

Canyon Diablo
Canyon Diablo
Canyon Diablo Canyon Diablo

Canyon Diablo

Iron Meteorite Coarse Octahedrite

Cochino City, Arizona, USA

Muonionalusta

Muonionalusta

Iron Meteorite Octahedrite

Sweden

Brenham

Brenham

Stony Iron Meteorite Siderite/Pallasite

Haviland, Kansas, USA

Glorieta Mountain

Glorieta Mountain

Stony Iron Meteorite Siderite/Pallasite

Sante Fe County, New Mexico

Seymchan Pallasite

Seymchan Pallasite

Pallasite Pallasite Iron Meteorite

Magadan District, Russia

Seymchan Pallasite

Shirokovsky Pallasite

Pseudo-Meteorite aka "Meteor Wrong"

Shirokovsky Reservoir , Russia

Muonionalusta
Salvage Sale

Muonionalusta

Iron Meteorite Octahedrite

Sweden

Splash Tektites

Splash Tektites

Libyan Desert Glass

Libyan Desert Glass

Tektites

Egypt

Meteorites