Barringer Crater, Arizona
As you stare up into the star-filled sky on almost any moonless night, you will probably see a few meteors every hour. During meteor showers (such as the Leonid shower which occurs each fall) you may see as many as one hundred meteors every hour. Meteor showers can be very impressive. A meteor is a bright streak of light in the sky created when a small meteoroid enters the Earth's atmosphere. Meteors are sometimes called shooting stars or falling stars. Very bright meteors are called fireballs.
Meteorites are bits of the solar system that have fallen to Earth. Most meteorites come from asteroids which have strayed from the asteroid belt located between Earth and Mars. Some have been found that are believed to have come specifically from the 4 Vesta asteroid. Some probably came from comets. A few have been found which came from our Moon and a few are believed to have come from Mars. One famous meteorite, called ALH84001, is believed to show evidence of early life on Mars. Meteorites are very important in scientific research, because they are our only material link to the universe beyond Earth.
 Iron: primarily iron and nickel; similar to type M asteroids
 Stony iron: mixtures of iron and stony material like type S asteroids
 Chondrite: by far the largest number of meteorites fall into this class; similar in composition to the mantles and crusts of the terrestrial planets
 Carbonaceous Chondrite: very similar in composition to the Sun less volatiles; similar to type C asteroids
 Achondrite: similar to terrestrial basalts; the meteorites believed to have originated on the Moon and Mars are achondrites
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 all meteorites are witnessed falls. More than one hundred tons of meteoroid material enters the Earth's atmosphere every day. Most of this material is very small, weighing only a few milligrams each. They are called micro-meteorites. Only the largest bits of meteoroid material ever reach the surface of the Earth to become meteorites. Weighing in at 60 tons, the Hoba Meteorite, found in Namibia, is the largest on record.
The average meteoroid enters the atmosphere at between 10 and 70 km/sec. But 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 Earth, so far.
A more recent impact occurred in 1908 in a remote uninhabited region of western Siberia known as Tunguska. The impactor was about 60 meters in diameter and probably consisting of many loosely bound pieces. In contrast to the Barringer Crater event, the Tunguska object completely disintegrated before hitting the ground and so no crater was formed. Nevertheless, all the trees were flattened in an area 50 kilometers across. The sound of the explosion was heard half-way around the world in London.
There are probably at least 1000 asteroids larger than 1 km in diameter that cross the orbit of Earth. One of these hits the Earth about once in a million years or so on the average. Larger ones are less numerous and impacts are less frequent, but they do sometimes happen and with disastrous consequences.
The impact of a comet or asteroid hitting the Earth was probably responsible for the extinction of the dinosaurs 65 million years ago. It left a 180 km crater now buried below the jungle near Chicxulub in the Yucatan Peninsula.
Freshly fallen meteorites and what to do if you find one:
Calculations based on the observed number of asteroids suggest that we should expect about 3 craters 10 km or more across to be formed on the Earth every million years. This is in good agreement with the geologic record. It is more difficult to compute the frequency of larger impacts like Chicxulub but once per 100 million years seems like a reasonable guess.
The most important primitive meteorites are generally those that were observed falling and collected soon after hitting the ground. These samples are particularly useful because they have not been altered by chemical and physical processes (such as rain) that are typical of the Earth's surface.
Freshly-fallen meteorites are usually the easiest to identify, because they are surrounded by a fusion crust produced when the surface of the meteoroid was melted by friction with the Earth's atmosphere. (You may recall that when space capsules or shuttles return to Earth, they are protected by heat shields to prevent the spacecraft from being consumed.). Fusion crusts are usually black or brown. Sometimes they contain flow lines radiating from one end of the meteorite towards the other, indicating the thin skin of melt was being blown backwards. These samples are called oriented meteorites, because we can tell how they were oriented when they fell through the atmosphere.
If a sample is unbroken and has a complete fusion crust, handle the sample gently to preserve the fusion crust. To see the interior of the object, only chip away or grind off a very small portion of the sample. If the interior resembles one of the meteorites described above, bring the sample to a credible laboratory where a complete examination can be properly documented and precautions can be taken to preserve the integrity of the sample.
If you believe you have found a freshly-fallen meteorite, try to photograph the area before removing any specimens. If a meteorite has produced a crater, measure its diameter and depth (some may only be a few centimeters deep). You should also look for multiple meteorite fragments scattered around the area. If you find more than one, try to estimate the distance between the samples.
Hunting for meteorites:
Scientists recently discovered that meteorites have been preserved and concentrated in certain regions of Antarctica. Consequently, within the last 20 years, Japanese and American teams of scientists have collected over 15,000 meteorite specimens from Antarctica, increasing the number of samples in our collections dramatically.
Until the work in Antarctica began, the total number of known meteorites was about 2,600. Of these, only about one-third were observed to fall. Most meteorites are classified as finds and were discovered by farmers, shepherds, ranchers, hikers, and so on. In some cases, however, they were found by diligent meteorite hunters. A few meteorites have also been found in fossiliferous limestones and two were found in rocks collected from the Moon by Apollo astronauts.
Although 93% of the meteorites observed to fall are chondrites and achondrites, only 56% of the meteorites that are found accidentally are of these same types. Iron meteorites are much more common among the meteorite finds, because they are so unlike most terrestrial rocks and because stony meteorites are highly susceptible to weathering on the surface of the Earth. While hunting for meteorites (in the case of iron meteorites), look for dense rocks with brown fusion crusts which are also magnetic and have a metallic silver interior.
If you find a possible meteorite, try to avoid handling the stone. In contrast to some myths, you will not be harmed by touching a meteorite, but you may inadvertently contaminate the sample with salts and oils from your hands. If possible, place the stone in a clean (and dry) plastic bag. Bring the sample to a credible laboratory as soon as possible.
 David A. Kring. Meteorites and their properties. Lunar and
Planetary Laboratory. Department of Planetary Sciences. The University
of Arizona. http://meteorites.lpl.arizona.edu/index.html. 27 Feb 2007.
 Bill Arnett. Meteors, Meteorites and Impacts. The Nine (8)
27 Feb 2007.