meteoric

　 　 　

WordNet

1. pertaining to or consisting of meteors or meteoroids; "meteoric shower"; "meteoric impacts"
2. like a meteor in speed or brilliance or transience; "a meteoric rise to fame"
3. of or relating to micrometeorites
4. a streak of light in the sky at night that results when a meteoroid hits the earths atmosphere and air friction causes the meteoroid to melt or vaporize or explode (同)shooting_star

PrepTutorEJDIC

1. 流星の,流星を含む / (速さ・はかなさ・輝きなどの点で)流星のような / 大気の;気象上の
2. 流星のように;ぱっとはなばなしく
3. 流星 / 隕石(いんせき)

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出典(authority):フリー百科事典『ウィキペディア（Wikipedia）』「2016/06/22 17:14:45」(JST)

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See also: Meteor and Meteorite

From a meteoroid to a meteor and meteorite.

Animated illustration of different phases as a meteoroid enters the atmosphere to become visible as a meteor and impact the Earth's surface as a meteorite.

A meteoroid is a small rocky or metallic body travelling through outer space. Meteoroids are significantly smaller than asteroids, and range in size from small grains to 1 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 comet, asteroid, or meteoroid enters the 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.

Around 15,000 tonnes of meteoroids, micrometeoroids and different forms of space dust enter Earth's atmosphere each year.

Meteoroids

See also: Micrometeoroid

Meteoroid embedded in aerogel. The meteoroid is 10 µm in diameter and its track is 1.5 mm long.

2008 TC3 meteorite fragments found on February 28, 2009, in the Nubian Desert, Sudan

In 1961, the International Astronomical Union 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 revised 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 TS₂₆ with H = 33.2 and 2011 CQ1 with H = 32.1 both with an estimated size of 1 meter. Objects smaller than meteoroids are classified as micrometeoroids and cosmic dust. The Minor Planet Center does not use the term "meteoroid".

Composition

Almost all meteoroids contain extraterrestrial nickel and irons. They have three main classifications: irons, stones and stony-irons. Some stone meteoroids contain grain-like inclusions known as chondrules and are called chondrites. Stoney 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 the 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

Meteoroids travel around the Sun in a variety of orbits and at various velocities. The fastest ones move at about 42 kilometers per second through space in the vicinity of Earth's orbit. The Earth travels at about 29.6 kilometers per second. Thus, when meteoroids meet Earth's 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. 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 a wide area in 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, and collided head-on with Earth 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 the Earth's atmosphere at night, they are likely to become visible as meteors. If meteoroids survive the entry through the atmosphere and reach the 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 TC3, was observed in space on a collision course with the Earth on 6 October 2008 and entered the 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 the Earth. NASA has produced a map showing the most notable asteroid collisions with the 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 passage of a meteoroid, micrometeoroid, comet or asteroid into the Earth's atmosphere, heated from collisions with air particles in the upper atmosphere and shedding glowing material in its wake sufficiently to create a visible streak of light. Meteors typically occur in the mesosphere at altitudes from 76 to 100 km (47 to 62 mi). The root word meteor comes from the Greek meteōros, meaning "high in the air".

Millions of meteors occur in the Earth's atmosphere daily. Most meteoroids that cause meteors are about the size of a grain of sand. Meteors may occur in showers, which arise when the 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 (47 to 75 mi) above the Earth. They usually disintegrate at altitudes of 50 to 95 km (31 to 59 mi). Meteors have roughly a fifty percent chance of a daylight (or near daylight) collision with the 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 19th 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. Thomas Jefferson wrote "I would more easily believe that (a) Yankee professor would lie than that stones would fall from heaven." He was referring to Yale chemistry professor Benjamin Silliman's investigation of an 1807 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

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 the 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 the 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 the Earth.

For 2014, there were 3,751 fireballs recorded at the American Meteor Society. 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	2010	2011	2012	2013	2014
Number	726	692	948	1,629	2,326	3,556	3,751

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 the 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. Larger meteors can enter dark flight after deceleration where the meteorite (or fragments) fall at terminal velocity. Dark flight starts when the meteorite(s) 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 the 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 the 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 the 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

• Orionid

• Two Orionids and Milky Way

• Multi-colored Orionid

• Orionid

• The brightest meteor, a fireball, leaves a smoky, persistent trail drifting in high-altitude winds, which is seen at the right-hand side of the image left by Orionid.

• A fireball seen over the desert of Central Australia. Although this occurred during the Lyrids, its North-East entry angle indicates it is sporadic.

• Looking down from the International Space Station at a meteor as it passes through the atmosphere

• Possible meteor 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 planets'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)=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
• 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

External links

• 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)

English Journal

• Oxygen isotope anomaly observed in water vapor from Alert, Canada and the implication for the stratosphere.

• Lin Y, Clayton RN, Huang L, Nakamura N, Lyons JR.SourceDepartment of Geochemistry and Environment Science, School of Earth and Space Sciences, University of Science and Technology of China, Hefei, Anhui 230026, China.
• Proceedings of the National Academy of Sciences of the United States of America.Proc Natl Acad Sci U S A.2013 Sep 5. [Epub ahead of print]
• To identify the possible anomalous oxygen isotope signature in stratospheric water predicted by model studies, 25 water vapor samples were collected in 2003-2005 at Alert station, Canada (82°30'N), where there is downward transport of stratospheric air to the polar troposphere, and were analyzed fo
• PMID 24009339

• Stable isotope composition of the meteoric precipitation in Croatia.

• Hunjak T, Lutz HO, Roller-Lutz Z.Sourcea Stable Isotope Laboratory, Medical Faculty , Rijeka University , Rijeka , Croatia.
• Isotopes in environmental and health studies.Isotopes Environ Health Stud.2013 Aug 13. [Epub ahead of print]
• The precipitation is the input into the water system. Its stable isotope composition has to be known for the proper use and management of water resources. Croatia is not well represented in the Global Network of Isotopes in Precipitation (GNIP) database, and the geomorphology of the country causes s
• PMID 23937110

• Using hydrochemical data and modelling to enhance the knowledge of groundwater flow and quality in an alluvial aquifer of Zagreb, Croatia.

• Marković T, Brkić Ž, Larva O.SourceCroatian Geological Survey, Department of Hydrogeology and Engineering Geology, Milana Sachsa 2, Zagreb, Croatia. tmarkovic@hgi-cgs.hr
• The Science of the total environment.Sci Total Environ.2013 Aug 1;458-460:508-16. doi: 10.1016/j.scitotenv.2013.04.013. Epub 2013 May 21.
• The Zagreb alluvial aquifer system is located in the southwest of the Pannonian Basin in the Sava Valley in Croatia. It is composed of Quaternary unconsolidated deposits and is highly utilised, primarily as a water supply for the more than one million inhabitants of the capital city of Croatia. To d
• PMID 23707721

• Hydrochemical and isotopic investigation of atmospheric precipitation in Beijing, China.

• Zhai Y, Wang J, Zhang Y, Teng Y, Zuo R, Huan H.SourceCollege of Water Sciences, Beijing Normal University, Beijing 100875, China. diszyz@163.com
• The Science of the total environment.Sci Total Environ.2013 Jul 1;456-457:202-11. doi: 10.1016/j.scitotenv.2013.03.091. Epub 2013 Apr 17.
• Precipitation water samples were collected at an urban site in Beijing in a hydrological cycle (July 2008-July 2009), and analyzed for TDS, total alkalinity, total hardness, free CO₂, soluble SiO₂, bromide, sulfide, phosphate, major ions (K(+), Na(+), Ca(2+), Mg(2+), NH₄(+), HCO₃(-), Cl(-),
• PMID 23602973

Japanese Journal

• 青森県津軽平野を対象とした生育水と精米の軽元素安定同位体比の相関性

• 富山 眞吾,鈴木 彌生子,中下 留美子,相川 良雄
• 分析化学 = Japan analyst 60(7), 563-570, 2011-07-05
• 近年社会問題化しているコメの産地偽装問題に対し，科学的根拠に基づいた判別技術の確立が求められており，そのためにはコメと生育水の軽元素安定同位体比の相関性を確認する必要がある．本研究は，青森県津軽平野を対象に生育水の酸素・水素安定同位体比及び炭素安定同位体比の空間的分布を明らかにし，その上でコメの安定同位体比との相関性を検討した．津軽平野の中央部では平野縁辺部と比較して生育水の酸素・水素安定同位体比 …
• NAID 10029140541

• 地球化学的手法と数値解析を用いた埼玉県狭山市の飲料工場で使用する地下水起源の判別

• 富山 眞吾,上田 晃,北井 亜希子,葵 守一
• 分析化学 = Japan analyst 60(2), 131-142, 2011-02-05
• 食品原材料となる地下水の品質管理の問題が起きており，地下水の起源について水質特徴などの科学的根拠に基づいて判別する技術が必要とされている．本研究は，埼玉県狭山市にある株式会社フードケミファ新埼玉工場の井戸で採水している地下水と周辺河川水を対象に，水素・酸素安定同位体比等の地球化学的手法と3次元数値モデルによる地下水流動解析を用いて地下水の起源や流れを予測した．地下水の水質は関東平野西縁辺部の河川水 …
• NAID 10027410103

• Mixing of magmatic CO2 into volcano groundwater flow at Aso volcano assessed combining carbon and water stable isotopes

• Yamada Makoto,Ohsawa Shinji,Kazahaya Kohei,Yasuhara Masaya,Takahashi Hiroshi,Amita Kazuhiro,Mawatari Hideo,Yoshikawa Shin
• Journal of Geochemical Exploration 108(1), 81-87, 2011-01
• … The waters' stable hydrogen and oxygen isotope ratios (δD and δ18O) reflect the meteoric-water origin of that region's deep groundwater. …
• NAID 120002709542

Related Links

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Meteoric Life Sciences excels in manufacturing and marketing of Enzymes & Enzymatic Preparations, Pre & Probiotics, Feed supplements & Additives, Nutraceuticals, Animal Healthcare & Nutrition, Industrial Enzymes ...

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