Meteoroid - wikipedia Meteoroid Not to be confused with Meteorite. A meteoroid shown entering the atmosphere, becoming visible as a meteor and hitting the Earth 's surface as a meteorite. A meteoroid ( / ˈmiːtiərɔɪd / ) is a small rocky or metallic body in outer space. Meteoroids are significantly smaller than asteroids, and range in size from small grains to one - meter - wide objects. Objects smaller than this are classified as micrometeoroids or space dust. Most are fragments from comets or asteroids, whereas others are collision impact debris ejected from bodies such as the Moon or Mars. When a meteoroid, comet, or asteroid enters Earth 's atmosphere at a speed typically in excess of 20 km / s ( 72,000 km / h ; 45,000 mph ), aerodynamic heating of that object produces a streak of light, both from the glowing object and the trail of glowing particles that it leaves in its wake. This phenomenon is called a meteor or `` shooting star ''. A series of many meteors appearing seconds or minutes apart and appearing to originate from the same fixed point in the sky is called a meteor shower. If that object withstands ablation from its passage through the atmosphere as a meteor and impacts with the ground, it is then called a meteorite. An estimated 15,000 tonnes of meteoroids, micrometeoroids and different forms of space dust enter Earth 's atmosphere each year. Contents 1 Meteoroids 1.1 Composition 1.2 In the Solar System 1.3 Collision with Earth 's atmosphere 2 Meteors 2.1 History 2.2 Fireball 2.3 Effect on atmosphere 2.3. 1 Colours 2.3. 2 Acoustic manifestations 2.4 Meteor shower 2.5 Notable meteors 2.6 Gallery of meteors 3 Meteorites 3.1 Frequency of impacts 3.2 Impact craters 3.3 Gallery of meteorites 4 See also 4.1 Relating to meteoroids 4.2 Relating to meteors 4.3 Relating to meteorites 5 References 6 External links Meteoroids See also : Micrometeoroid Meteoroid embedded in aerogel ; the meteoroid is 10 μm in diameter and its track is 1.5 mm long 2008 TC 3 meteorite fragments found on February 28, 2009, in the Nubian Desert, Sudan In 1961, the International Astronomical Union ( IAU ) defined a meteoroid as `` a solid object moving in interplanetary space, of a size considerably smaller than an asteroid and considerably larger than an atom ''. In 1995, Beech and Steel, writing in the Quarterly Journal of the Royal Astronomical Society, proposed a new definition where a meteoroid would be between 100 μm and 10 meters across. In 2010, following the discovery of asteroids below 10 m in size, Rubin and Grossman proposed a revision of the previous definition of meteoroid to objects between 10 μm and 1 m in diameter in order to maintain the distinction. According to Rubin and Grossman, the minimum size of an asteroid is given by what can be discovered from Earth - bound telescopes, so the distinction between meteoroid and asteroid is fuzzy. Some of the smallest asteroids discovered ( based on absolute magnitude H ) are 2008 TS with H = 33.2 and 2011 CQ 1 with H = 32.1 both with an estimated size of 1 meter. In April 2017, the IAU adopted an official revision of its definition, limiting size to between 30 μm and 1 m in diameter, but allowing for a deviation for any object causing a meteor. Objects smaller than meteoroids are classified as micrometeoroids and interplanetary dust. The Minor Planet Center does not use the term `` meteoroid ''. Composition Almost all meteoroids contain extraterrestrial nickel and iron. They have three main classifications : iron, stone, and stony - iron. Some stone meteoroids contain grain - like inclusions known as chondrules and are called chondrites. Stony meteoroids without these features are called `` achondrites '', which are typically formed from extraterrestrial igneous activity ; they contain little or no extraterrestrial iron. The composition of meteoroids can be inferred as they pass through Earth 's atmosphere from their trajectories and the light spectra of the resulting meteor. Their effects on radio signals also give information, especially useful for daytime meteors, which are otherwise very difficult to observe. From these trajectory measurements, meteoroids have been found to have many different orbits, some clustering in streams ( see meteor showers ) often associated with a parent comet, others apparently sporadic. Debris from meteoroid streams may eventually be scattered into other orbits. The light spectra, combined with trajectory and light curve measurements, have yielded various compositions and densities, ranging from fragile snowball - like objects with density about a quarter that of ice, to nickel - iron rich dense rocks. The study of meteorites also gives insights into the composition of non-ephemeral meteoroids. In the solar system Most meteoroids come from the asteroid belt, having been perturbed by the gravitational influences of planets, but others are particles from comets, giving rise to meteor showers. Some meteoroids are fragments from bodies such as Mars or our moon, that have been thrown into space by an impact. Meteoroids travel around the Sun in a variety of orbits and at various velocities. The fastest move at about 42 kilometers per second through space in the vicinity of Earth 's orbit. This is escape velocity from the sun, equal to the square root of 2 times Earth 's speed, and is the upper speed limit of objects in the vicinity of Earth, unless they come from interstellar space. Earth travels at about 29.6 kilometers per second, so when meteoroids meet the atmosphere head - on ( which only occurs when meteors are in a retrograde orbit such as the Eta Aquarids, which are associated with the retrograde Halley 's Comet ) the combined speed may reach about 71 kilometers per second ( see Specific energy # Astrodynamics ). Meteoroids moving through Earth 's orbital space average about 20 km / s. On January 17, 2013 at 05 : 21 PST, a 1 meter - sized comet from the Oort cloud entered Earth atmosphere over California and Nevada. The object had a retrograde orbit with perihelion at 0.98 ± 0.03 AU. It approached from the direction of the constellation Virgo ( which was in the south about 50 ° above the horizon at the time ), and collided head - on with Earth 's atmosphere at 72 ± 6 km / s vapourising more than 100 km above ground over a period of several seconds. Collision with Earth 's atmosphere When meteoroids intersect with Earth 's atmosphere at night, they are likely to become visible as meteors. If meteoroids survive the entry through the atmosphere and reach Earth 's surface, they are called meteorites. Meteorites are transformed in structure and chemistry by the heat of entry and force of impact. A noted 4 - meter asteroid, 2008 TC 3, was observed in space on a collision course with Earth on 6 October 2008 and entered Earth 's atmosphere the next day, striking a remote area of northern Sudan. It was the first time that a meteoroid had been observed in space and tracked prior to impacting Earth. NASA has produced a map showing the most notable asteroid collisions with Earth and its atmosphere from 1994 to 2013 from data gathered by U.S. government sensors ( see below ). Meteors `` Meteor '' redirects here. For other uses, see Meteor ( disambiguation ). Meteor seen from the site of the Atacama Large Millimeter Array ( ALMA ) World map of large meteoric events ( also see Fireball below ) A meteor, known colloquially as a shooting star or falling star, is the visible passage of a glowing meteoroid, micrometeoroid, comet or asteroid through Earth 's atmosphere, after being heated to incandescence by collisions with air molecules in the upper atmosphere, creating a streak of light via its rapid motion and sometimes also by shedding glowing material in its wake. Although a meteor may seem to be a few thousand feet from the Earth, meteors typically occur in the mesosphere at altitudes from 76 to 100 km ( 45 to 60 mi ). The root word meteor comes from the Greek meteōros, meaning `` high in the air ''. Millions of meteors occur in Earth 's atmosphere daily. Most meteoroids that cause meteors are about the size of a grain of sand, i.e. they are usually millimeter - sized or smaller. Meteoroid sizes can be calculated from their mass and density which, in turn, can be estimated from the observed meteor trajectory in the upper atmosphere. Meteors may occur in showers, which arise when Earth passes through a stream of debris left by a comet, or as `` random '' or `` sporadic '' meteors, not associated with a specific stream of space debris. A number of specific meteors have been observed, largely by members of the public and largely by accident, but with enough detail that orbits of the meteoroids producing the meteors have been calculated. All of the orbits passed through the asteroid belt. The atmospheric velocities of meteors result from the movement of Earth around the Sun at about 30 km / s ( 18 miles / second ), the orbital speeds of meteoroids, and the gravity well of Earth. Meteors become visible between about 75 to 120 km ( 45 to 75 mi ) above Earth. They usually disintegrate at altitudes of 50 to 95 km ( 30 to 60 mi ). Meteors have roughly a fifty percent chance of a daylight ( or near daylight ) collision with Earth. Most meteors are, however, observed at night, when darkness allows fainter objects to be recognized. For bodies with a size scale larger than 10 cm to several meters meteor visibility is due to the atmospheric ram pressure ( not friction ) that heats the meteoroid so that it glows and creates a shining trail of gases and melted meteoroid particles. The gases include vaporised meteoroid material and atmospheric gases that heat up when the meteoroid passes through the atmosphere. Most meteors glow for about a second. History Although meteors have been known since ancient times, they were not known to be an astronomical phenomenon until early in the nineteenth century. Prior to that, they were seen in the West as an atmospheric phenomenon, like lightning, and were not connected with strange stories of rocks falling from the sky. In 1807, Yale University chemistry professor Benjamin Silliman investigated a meteorite that fell in Weston, Connecticut. Silliman believed the meteor had a cosmic origin, but meteors did not attract much attention from astronomers until the spectacular meteor storm of November 1833. People all across the eastern United States saw thousands of meteors, radiating from a single point in the sky. Astute observers noticed that the radiant, as the point is now called, moved with the stars, staying in the constellation Leo. The astronomer Denison Olmsted made an extensive study of this storm, and concluded that it had a cosmic origin. After reviewing historical records, Heinrich Wilhelm Matthias Olbers predicted the storm 's return in 1867, which drew the attention of other astronomers to the phenomenon. Hubert A. Newton 's more thorough historical work led to a refined prediction of 1866, which proved to be correct. With Giovanni Schiaparelli 's success in connecting the Leonids ( as they are now called ) with comet Tempel - Tuttle, the cosmic origin of meteors was now firmly established. Still, they remain an atmospheric phenomenon, and retain their name `` meteor '' from the Greek word for `` atmospheric ''. Fireball Main article : List of bolides Play media Footage of a superbolide, a very bright fireball that exploded over Chelyabinsk Oblast, Russia in 2013 A fireball is a brighter - than - usual meteor. The International Astronomical Union ( IAU ) defines a fireball as `` a meteor brighter than any of the planets '' ( apparent magnitude − 4 or greater ). The International Meteor Organization ( an amateur organization that studies meteors ) has a more rigid definition. It defines a fireball as a meteor that would have a magnitude of − 3 or brighter if seen at zenith. This definition corrects for the greater distance between an observer and a meteor near the horizon. For example, a meteor of magnitude − 1 at 5 degrees above the horizon would be classified as a fireball because, if the observer had been directly below the meteor, it would have appeared as magnitude − 6. Fireballs reaching apparent magnitude − 14 or brighter are called bolides. The IAU has no official definition of `` bolide '', and generally considers the term synonymous with `` fireball ''. Astronomers often use `` bolide '' to identify an exceptionally bright fireball, particularly one that explodes. They are sometimes called detonating fireballs ( also see List of meteor air bursts ). It may also be used to mean a fireball which creates audible sounds. In the late twentieth century, bolide has also come to mean any object that hits Earth and explodes, with no regard to its composition ( asteroid or comet ). The word bolide comes from the Greek βολίς ( bolis ) which can mean a missile or to flash. If the magnitude of a bolide reaches − 17 or brighter it is known as a superbolide. A relatively small percentage of fireballs hit Earth 's atmosphere and then pass out again : these are termed Earth - grazing fireballs. Such an event happened in broad daylight over North America in 1972. Another rare phenomena is a meteor procession, where the meteor breaks up into several fireballs traveling nearly parallel to the surface of Earth. A steadily growing number of fireballs are recorded at the American Meteor Society every year. There are probably more than 500,000 fireballs a year, but most will go unnoticed because most will occur over the ocean and half will occur during daytime. Fireball Sightings reported to the American Meteor Society Year 2008 2009 2011 2012 2013 2014 2015 2016 2017 2018 Number 724 668 941 1,653 2,172 3,556 3,778 4,233 5,371 5,470 4,301 Effect on atmosphere `` Ionization trail '' and `` Dark flight ( astronomy ) '' redirect here. For the movie, see Dark Flight. Ionization trail of a Perseid meteor seen against the constellation Corona Borealis with its ring of stars The entry of meteoroids into Earth 's atmosphere produces three main effects : ionization of atmospheric molecules, dust that the meteoroid sheds, and the sound of passage. During the entry of a meteoroid or asteroid into the upper atmosphere, an ionization trail is created, where the air molecules are ionized by the passage of the meteor. Such ionization trails can last up to 45 minutes at a time. Small, sand - grain sized meteoroids are entering the atmosphere constantly, essentially every few seconds in any given region of the atmosphere, and thus ionization trails can be found in the upper atmosphere more or less continuously. When radio waves are bounced off these trails, it is called meteor burst communications. Meteor radars can measure atmospheric density and winds by measuring the decay rate and Doppler shift of a meteor trail. Most meteoroids burn up when they enter the atmosphere. The left - over debris is called meteoric dust or just meteor dust. Meteor dust particles can persist in the atmosphere for up to several months. These particles might affect climate, both by scattering electromagnetic radiation and by catalyzing chemical reactions in the upper atmosphere. Meteoroids or their fragments may achieve dark flight after deceleration to terminal velocity. Dark flight starts when they decelerate to about 2 -- 4 km / s ( 4,500 -- 8,900 mph ). Larger fragments will fall further down the strewn field. Colours A meteor of the Leonid meteor shower, the photograph shows the meteor, afterglow, and wake as distinct components The visible light produced by a meteor may take on various hues, depending on the chemical composition of the meteoroid, and the speed of its movement through the atmosphere. As layers of the meteoroid abrade and ionize, the colour of the light emitted may change according to the layering of minerals. Colours of meteors depend on the relative influence of the metallic content of the meteoroid versus the superheated air plasma, which its passage engenders : Orange - yellow ( sodium ) Yellow ( iron ) Blue - green ( magnesium ) Violet ( calcium ) Red ( atmospheric nitrogen and oxygen ) Acoustic manifestations Sound generated by a meteor in the upper atmosphere, such as a sonic boom, typically arrives many seconds after the visual light from a meteor disappears. Occasionally, as with the Leonid meteor shower of 2001, `` crackling '', `` swishing '', or `` hissing '' sounds have been reported, occurring at the same instant as a meteor flare. Similar sounds have also been reported during intense displays of Earth 's auroras. Theories on the generation of these sounds may partially explain them. For example, scientists at NASA suggested that the turbulent ionized wake of a meteor interacts with Earth 's magnetic field, generating pulses of radio waves. As the trail dissipates, megawatts of electromagnetic power could be released, with a peak in the power spectrum at audio frequencies. Physical vibrations induced by the electromagnetic impulses would then be heard if they are powerful enough to make grasses, plants, eyeglass frames, and other conductive materials vibrate. This proposed mechanism, although proven to be plausible by laboratory work, remains unsupported by corresponding measurements in the field. Sound recordings made under controlled conditions in Mongolia in 1998 support the contention that the sounds are real. ( Also see Bolide. ) Meteor shower Main articles : Meteor shower and List of meteor showers Multiple meteors photographed over an extended exposure time during a meteor shower Meteor shower on chart A meteor shower is the result of an interaction between a planet, such as Earth, and streams of debris from a comet or other source. The passage of Earth through cosmic debris from comets and other sources is a recurring event in many cases. Comets can produce debris by water vapor drag, as demonstrated by Fred Whipple in 1951, and by breakup. Each time a comet swings by the Sun in its orbit, some of its ice vaporizes and a certain amount of meteoroids will be shed. The meteoroids spread out along the entire orbit of the comet to form a meteoroid stream, also known as a `` dust trail '' ( as opposed to a comet 's `` dust tail '' caused by the very small particles that are quickly blown away by solar radiation pressure ). The frequency of fireball sightings increases by about 10 - 30 % during the weeks of vernal equinox. Even meteorite falls are more common during the northern hemisphere 's spring season. Although this phenomenon has been known for quite some time, the reason behind the anomaly is not fully understood by scientists. Some researchers attribute this to an intrinsic variation in the meteoroid population along Earth 's orbit, with a peak in big fireball - producing debris around spring and early summer. Others have pointed out that during this period the ecliptic is ( in the northern hemisphere ) high in the sky in the late afternoon and early evening. This means that fireball radiants with an asteroidal source are high in the sky ( facilitating relatively high rates ) at the moment the meteoroids `` catch up '' with Earth, coming from behind going in the same direction as Earth. This causes relatively low relative speeds and from this low entry speeds, which facilitates survival of meteorites. It also generates high fireball rates in the early evening, increasing chances of eye witness reports. This explains a part, but perhaps not all of the seasonal variation. Research is in progress for mapping the orbits of the meteors to gain a better understanding of the phenomenon. Notable meteors See also : Near - Earth object § Notable objects 1992 -- Peekskill, New York The Peekskill Meteorite was filmed on October 9, 1992 by at least 16 independent videographers. Eyewitness accounts indicate the fireball entry of the Peekskill meteorite started over West Virginia at 23 : 48 UT ( ± 1 min ). The fireball, which traveled in a northeasterly direction, had a pronounced greenish colour, and attained an estimated peak visual magnitude of − 13. During a luminous flight time that exceeded 40 seconds the fireball covered a ground path of some 700 to 800 km. One meteorite recovered at Peekskill, New York, for which the event and object gained their name, had a mass of 12.4 kg ( 27 lb ) and was subsequently identified as an H6 monomict breccia meteorite. The video record suggests that the Peekskill meteorite had several companions over a wide area. The companions are unlikely to be recovered in the hilly, wooded terrain in the vicinity of Peekskill. 2009 -- Bone, Indonesia A large fireball was observed in the skies near Bone, Indonesia on October 8, 2009. This was thought to be caused by an asteroid approximately 10 meters in diameter. The fireball contained an estimated energy of 50 kilotons of TNT, or about twice the Nagasaki atomic bomb. No injuries were reported. 2009 -- Southwestern US A large bolide was reported on 18 November 2009 over southeastern California, northern Arizona, Utah, Wyoming, Idaho and Colorado. At 00 : 07 local time a security camera at the high altitude W.L. Eccles Observatory ( 2930 m above sea level ) recorded a movie of the passage of the object to the north. Of particular note in this video is the spherical `` ghost '' image slightly trailing the main object ( this is likely a lens reflection of the intense fireball ), and the bright fireball explosion associated with the breakup of a substantial fraction of the object. An object trail can be seen to continue northward after the bright fireball event. The shock from the final breakup triggered seven seismological stations in northern Utah ; a timing fit to the seismic data yielded a terminal location of the object at 40.286 N, - 113.191 W, altitude 27 km. This is above the Dugway Proving Grounds, a closed Army testing base. 2013 -- Chelyabinsk Oblast, Russia The Chelyabinsk meteor was an extremely bright, exploding fireball, known as superbolide, measuring about 17 to 20 meters across, with an estimated initial mass of 11,000 tonnes, as the relatively small asteroid entered Earth 's atmosphere. It was the largest known natural object to have entered Earth 's atmosphere since the Tunguska event in 1908. Over 1,500 people were injured mostly by glass from shattered windows caused by the air burst approximately 25 to 30 km above the environs of Chelyabinsk, Russia on 15 February 2013. An increasingly bright streak was observed during morning daylight with a large contrail lingering behind. At no less than 1 minute and up to at least 3 minutes after the object peaked in intensity ( depending on distance from trail ), a large concussive blast was heard that shattered windows and set - off car alarms, which was followed by a number of smaller explosions. Gallery of meteors Orionid meteor Sporadic bolide over the desert of Central Australia and a Lyrid ( top edge ) Meteor ( center ) seen from the International Space Station Possible meteor ( center ) photographed from Mars, March 7, 2004, by MER Spirit Comet Shoemaker -- Levy 9 colliding with Jupiter : The sequence shows fragment W turning into a fireball on the planet 's dark side Meteorites Main article : Meteorite Murnpeowie meteorite, an iron meteorite with regmaglypts resembling thumbprints ( Australia, 1910 ) A meteorite is a portion of a meteoroid or asteroid that survives its passage through the atmosphere and hits the ground without being destroyed. Meteorites are sometimes, but not always, found in association with hypervelocity impact craters ; during energetic collisions, the entire impactor may be vaporized, leaving no meteorites. Geologists use the term, `` bolide '', in a different sense from astronomers to indicate a very large impactor. For example, the USGS uses the term to mean a generic large crater - forming projectile in a manner `` to imply that we do not know the precise nature of the impacting body... whether it is a rocky or metallic asteroid, or an icy comet for example ''. Meteoroids also hit other bodies in the solar system. On such stony bodies as the Moon or Mars that have little or no atmosphere, they leave enduring craters. Frequency of impacts See also : Planet Earth collision probability with near - Earth objects The diameter of the largest impactor to hit Earth on any given day is likely to be about 40 centimeters ( 16 inches ), in a given year about 4 meters, and in a given century about 20 meters. These statistics are obtained by the following : Over at least the range from 5 centimeters ( 2.0 inches ) to roughly 300 meters ( 980 feet ), the rate at which Earth receives meteors obeys a power - law distribution as follows : N ( > D ) = 37 D − 2.7 ( displaystyle N ( > D ) = 37D ^ ( - 2.7 ) ) where N ( > D ) is the expected number of objects larger than a diameter of D meters to hit Earth in a year. This is based on observations of bright meteors seen from the ground and space, combined with surveys of near - Earth asteroids. Above 300 meters in diameter, the predicted rate is somewhat higher, with a two - kilometer asteroid ( one million - megaton TNT equivalent ) every couple of million years -- about 10 times as often as the power - law extrapolation would predict. Impact craters Main article : Impact crater Meteoroid collisions with solid Solar System objects, including the Moon, Mercury, Callisto, Ganymede, and most small moons and asteroids, create impact craters, which are the dominant geographic features of many of those objects. On other planets and moons with active surface geological processes, such as Earth, Venus, Mars, Europa, Io, and Titan, visible impact craters may become eroded, buried, or transformed by tectonics over time. In early literature, before the significance of impact cratering was widely recognised, the terms cryptoexplosion or cryptovolcanic structure were often used to describe what are now recognised as impact - related features on Earth. Molten terrestrial material ejected from a meteorite impact crater can cool and solidify into an object known as a tektite. These are often mistaken for meteorites. Gallery of meteorites Two tektites, molten terrestrial ejecta from a meteorite impact A partial slice of the Esquel pallasite Willamette Meteorite, from Oregon, USA Meteorite, which fell in Wisconsin in 1868 Marília Meteorite, a chondrite H4, which fell in Marília, Brazil ( 1971 ) Children posing behind the Tucson Meteorite at the Arizona Museum of Natural History Meteorite with brecciation and carbon inclusions from Tindouf, Algeria See also Glossary of meteoritics Relating to meteoroids Interplanetary dust Micrometeoroid Near - Earth object Relating to meteors American Meteor Society Bolide Desert Fireball Network Green fireballs Hydrometeor International Meteor Organization Leonids List of meteor air bursts List of meteor showers Lyrids North American Meteor Network Orionids Perseids Tollmann 's hypothetical bolide Relating to meteorites Baetylus -- Sacred stones made from meteorites Impact crater Impact event Interplanetary dust cloud § Collecting interplanetary dust on Earth Meteorite Micrometeorite Tektite References Jump up ^ `` meteoroid Meaning in the Cambridge English Dictionary ''. dictionary.cambridge.org. ^ Jump up to : Rubin, Alan E. ; Grossman, Jeffrey N. 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Retrieved 7 February 2016. Full text archive. Jump up ^ Riley, Chris ( 1999 - 04 - 21 ). `` Sound of shooting stars ''. BBC News. Retrieved 2011 - 09 - 16. Jump up ^ Whipple, Fred ( 1951 ). `` A Comet Model. II. Physical Relations for Comets and Meteors '' ( PDF ). Astrophysical Journal. pp. 464 -- 474. Bibcode : 1951ApJ... 113... 464W. doi : 10.1086 / 145416. Jump up ^ Phillips, Tony. `` Spring is Fireball Season ''. science.nasa.gov. Retrieved 2011 - 09 - 16. Jump up ^ Langbroek, Marco ; Seizoensmatige en andere variatie in de valfrequentie van meteorieten, Radiant ( Journal of the Dutch Meteor Society ), 23 : 2 ( 2001 ), p. 32 Jump up ^ Coulter, Dauna ( 2011 - 03 - 01 ). `` What 's Hitting Earth ? ''. science.nasa.gov. Retrieved 2011 - 09 - 16. Jump up ^ `` The Peekskill Meteorite 9 October 1992 Videos ''. Jump up ^ Brown, Peter ; Ceplecha, Zedenek ; Hawkes, Robert L. ; Wetherill, George W. ; Beech, Martin ; Mossman, Kaspar ( 1994 ). `` The orbit and atmospheric trajectory of the Peekskill meteorite from video records ''. Nature. 367 ( 6464 ) : 624 -- 626. Bibcode : 1994Natur. 367... 624B. doi : 10.1038 / 367624a0. Jump up ^ Wlotzka, Frank ( 1994 ). `` Meteoritics ''. Meteoritical Bulletin # 75. 28 ( 5 ) : 692. doi : 10.1111 / j. 1945 - 5100.1993. tb00641. x. Jump up ^ Yeomans, Donald K. ; Chodas, Paul ; Chesley, Steve ( October 23, 2009 ). `` Asteroid Impactor Reported over Indonesia ''. NASA / JPL Near - Earth Object Program Office. Retrieved 2009 - 10 - 30. Jump up ^ `` W.L. Eccles Observatory, November 18, 2009, North Camera ''. YouTube. 2009 - 11 - 18. Retrieved 2011 - 09 - 16. Jump up ^ `` W.L. Eccles Observatory, November 18, 2009, North West Camera ''. YouTube. 2009 - 11 - 18. Retrieved 2011 - 09 - 16. Jump up ^ Yeomans, Don ; Chodas, Paul ( 1 March 2013 ). `` Additional Details on the Large Fireball Event over Russia on Feb. 15, 2013 ''. NASA / JPL Near - Earth Object Program Office. Retrieved 2 March 2013. Jump up ^ JPL ( 2012 - 02 - 16 ). `` Russia Meteor Not Linked to Asteroid Flyby ''. Retrieved 2013 - 02 - 19. Jump up ^ `` Meteorite slams into Central Russia injuring 1100 - as it happened ''. Guardian. 15 February 2013. Retrieved 16 February 2013. Jump up ^ The Oxford Illustrated Dictionary. 1976. Second Edition. Oxford University Press. page 533 Jump up ^ `` What is a Bolide ? ''. woodshole.er.usgs.gov. Retrieved 2011 - 09 - 16. Jump up ^ Brown, Peter ; Spalding, Richard E. ; ReVelle, Douglas O. ; Tagliaferri, Edward ; Worden, Simon P. ( 21 September 2002 ). `` The flux of small near - Earth objects colliding with the Earth ''. Nature. Retrieved 2009 - 06 - 22. Jump up ^ French, Bevan M. ( 1998 ). `` Traces of Catastrophe : A Handbook of Shock - Metamorphic Effects in Terrestrial Meteorite Impact Structures ''. Washington, DC : Smithsonian Institution. p. 97. Jump up ^ `` Northwest Africa 869 ''. Meteoritical Bulletin Database. The Meteoritical Society. External links Wikimedia Commons has media related to Meteor. Wikisource has original works on the topic : Meteoroids Look up meteoroid or meteor in Wiktionary, the free dictionary. A History of Meteors and Other Atmospheric Phenomena American Meteor Society British Astronomical Society meteor page International Meteor Organization Live Meteor Screen Meteoroids Page at NASA 's Solar System Exploration Meteor shower predictions Meteor Showers and Viewing Tips Society for Popular Astronomy - Meteor Section Minor Planet Center : Asteroid Hazards, Part 2 : The Challenge of Detection on YouTube ( min. 7 : 14 ) Small Solar System bodies Minor planets Designation Groups List Moon Meanings of names Asteroid Aten asteroid Asteroid belt Family Jupiter trojan Near - Earth Spectral types Distant minor planet Centaur Damocloid Neptune trojan Trans - Neptunian object Detached Kuiper belt Oort cloud Scattered disc Comets Extinct Great Halley - type Hyperbolic Long - period Lost Main - belt Near - parabolic Periodic Sungrazing Other Meteoroids The Solar System The Sun Mercury Venus Earth Mars Ceres Jupiter Saturn Uranus Neptune Pluto Haumea Makemake Eris Planets Terrestrial planets Mercury Venus Earth Mars Giant planets Jupiter Saturn Uranus Neptune Dwarf planets Ceres Pluto Haumea Makemake Eris Rings Jovian Saturnian ( Rhean ) Charikloan Chironean Uranian Neptunian Haumean Moons Terrestrial Moon other near - Earth objects Martian Phobos Deimos Jovian Ganymede Callisto Io Europa all 79 Saturnian Titan Rhea Iapetus Dione Tethys Enceladus Mimas Hyperion Phoebe all 62 Uranian Titania Oberon Umbriel Ariel Miranda all 27 Neptunian Triton Proteus Nereid all 14 Plutonian Charon Nix Hydra Kerberos Styx Haumean Hiʻiaka Namaka Makemakean S / 2015 ( 136472 ) 1 Eridian Dysnomia Exploration ( outline ) Discovery astronomy timeline Space probes list timeline Human spaceflight space stations list Colonization Mercury Venus Moon Mars Ceres Asteroids mining Comets Jupiter Saturn Uranus Neptune Pluto Deep space Small Solar System bodies Meteoroids Minor planets moons Comets Damocloids Mercury - crossers Venus - crossers Venus trojans Near - Earth objects Earth - crossers Earth trojans Mars - crossers Mars trojans Asteroid belt Asteroids Ceres Pallas Juno Vesta more Families Notable asteroids Kirkwood gap Main - belt comets Jupiter trojans Jupiter - crossers Centaurs Saturn - crossers Uranus trojans Uranus - crossers Neptune trojans Cis - Neptunian objects Trans - Neptunian objects Neptune - crossers Plutoids Kuiper belt Plutinos Cubewanos Scattered disc Detached objects Sednoids Hills cloud Oort cloud Hypothetical objects Vulcan Vulcanoids Theia Phaeton Planet V Fifth giant Planet X Planet Nine Tyche Nemesis Subsatellites Lists Solar System objects by size by discovery date Minor planets names Gravitationally rounded objects Possible dwarf planets Natural satellites Comets Outline of the Solar System Portals Solar System Astronomy Earth sciences Mars Jupiter Uranus Cosmology Solar System → Local Interstellar Cloud → Local Bubble → Gould Belt → Orion Arm → Milky Way → Milky Way subgroup → Local Group → Local Sheet → Virgo Supercluster → Laniakea Supercluster → Observable universe → Universe Each arrow ( → ) may be read as `` within '' or `` part of ''. Modern impact events On Earth Pre-2000 1490 Ch'ing - yang 1783 Great Meteor 1860 Great Meteor 1908 Tunguska 1913 Great Meteor Procession 1930 Curuçá River 1938 Chicora meteor 1947 Sikhote - Alin meteorite 1969 Murchison meteorite 1972 Great Daylight Fireball 1990 Earth - grazing meteoroid Post-2000 2002 Eastern Mediterranean 2002 Vitim 2007 Carancas 2008 TC3 impact 2008 Buzzard Coulee meteorite 2009 Sulawesi superbolide 2012 Sutter 's Mill meteorite 2012 UK meteoroid 2012 Novato meteorite 2013 Chelyabinsk meteor Chelyabinsk meteorite 2014 AA impact 2014 Ontario fireball 2015 Kerala meteorite 2015 Thailand bolide WT1190F impact 2017 China bolide 2018 LA impact On Jupiter 1994 Comet Shoemaker -- Levy 9 2009 Jupiter impact 2010 Jupiter impact Lists Asteroid close approaches to Earth Comets Bolides Meteor air bursts Meteorite falls Minor planets crossing Earth 's orbit See also Asteroid impact prediction Asteroid impact avoidance Bolide Earth - grazing fireball Meteor procession Meteor shower Meteorite Meteoroid Near - Earth object Potentially hazardous object Planetary defense Main topics Asteroid Bolide Earth - grazing fireball Impact event List of meteor air bursts Meteor procession Meteor shower Meteorite Meteoroid Near - Earth object Potentially hazardous object Defense Asteroid impact avoidance Asteroid laser ablation Gravity tractor Ion - beam shepherd Asteroid close approaches Earth - crossing minor planets Damage scales Palermo scale Torino scale Space probes Dawn Deep Impact AIDA Hera DART Halley Armada Hayabusa Hayabusa2 MASCOT NEAR Shoemaker NEA Scout New Horizons OSIRIS - REx PROCYON Rosetta Philae Stardust NEO tracking ATLAS Catalina Sky Survey LINEAR LONEOS NEAT NEOSSat NEOCam NEODyS OGS Telescope Orbit@home Pan-STARRS SCAP Sentinel Space Telescope Sentry Spacewatch WISE Organizations B612 Foundation Japan Spaceguard Association Meteoritical Society NEOShield Spaceguard The Spaceguard Foundation Space Situational Awareness Programme Planetary Defense Coordination Office Potential threats 1950 DA 1994 WR 101955 Bennu 2002 MN ( 410777 ) 2009 FD 2010 RF 99942 Apophis Films / video The End of the World ( 1916 ) When Worlds Collide ( 1951 ) Gorath ( 1962 ) The Green Slime ( 1968 ) The Paradise Syndrome ( 1968 ) A Fire in the Sky ( 1978 ) Meteor ( 1979 ) NOVA : Doomsday Asteroid ( 1995 ) Asteroid ( 1997 ) Deep Impact ( 1998 ) Armageddon ( 1998 ) Judgment Day ( 1999 ) Post Impact ( 2004 ) Deadly Skies ( 2006 ) Super Comet : After the Impact ( 2007 ) Impact ( 2009 ) NOVA : Last Extinction ( 2009 ) Meteor Storm ( 2010 ) HORIZON : Asteroids -- The Good, the Bad and the Ugly ( 2010 ) Melancholia ( 2011 ) NOVA : Meteor Strike ( 2013 ) NOVA : Asteroid : Doomsday or Payday ? ( 2013 ) Impact Earth ( 2015 ) Avengers : Age of Ultron ( 2015 ) GND : 4202315 - 4 Retrieved from `` https://en.wikipedia.org/w/index.php?title=Meteoroid&oldid=866324343 '' Categories : Meteoroids Hidden categories : All articles with unsourced statements Articles with unsourced statements from January 2016 Wikipedia articles with GND identifiers Articles containing video clips Talk Contents About Wikipedia Afrikaans Asturianu Avañe'ẽ বাংলা Беларуская Беларуская ( тарашкевіца ) ‎ Български Boarisch Bosanski Català Čeština Cymraeg Dansk Deutsch Eesti Ελληνικά Español Esperanto Euskara فارسی Français Gaeilge Gàidhlig Galego ગુજરાતી 한국어 Հայերեն हिन्दी Hrvatski Ido Bahasa Indonesia Italiano עברית ಕನ್ನಡ Къарачай - малкъар Қазақша Kiswahili Kreyòl ayisyen Latina Latviešu Lëtzebuergesch Lietuvių Limburgs Magyar Македонски മലയാളം मराठी Bahasa Melayu Монгол မြန်မာဘာသာ Nederlands नेपाली 日本 語 Norsk Norsk nynorsk Oʻzbekcha / ўзбекча پنجابی Plattdüütsch Polski Português Română Русский Scots සිංහල سنڌي Slovenčina Slovenščina کوردی Српски / srpski Srpskohrvatski / српскохрватски Suomi Svenska Tagalog தமிழ் తెలుగు ไทย Tsetsêhestâhese Українська اردو Tiếng Việt 粵語 中文 74 more Edit links This page was last edited on 29 October 2018, at 17 : 43 ( UTC ). 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Question: how far away can you see a meteor
Answer: between about 75 to 120 km (45 to 75 mi)