Asteroidal water is water[1][2][3] or water precursor deposits such as hydroxide (OH−[4]) that exist in asteroids (i.e., small Solar System bodies (SSSBs) not explicitly in the subcategory of comets).[5] The "snow line" of the Solar System lies outside of the main asteroid belt, and the majority of water is expected in minor planets (e.g. Kuiper belt objects (KBOs) and Centaurs). Nevertheless, a significant amount of water is also found inside the snow line, including in near-earth objects (NEOs).

The formation of asteroidal water mirrors that of water formation in the Solar System, either from transfer via bombardment, migration, ejection, or other means. Asteroidal water has recently been pursued as a resource to support deep space exploration activities, for example, for use as a rocket propellant, human consumption, or for agricultural production.

History

Meteorites

Since the early 1800s, meteorites have been assumed to be "space rocks", not terrestrial or atmospheric phenomena. At this time, asteroids were first discovered, then in increasing numbers and categories.

Many meteorites show signs of previous water. The petrological scale, numbered 1 through 7, indicates increasing aqueous alteration from type 2 to 1. Signs of water include phyllosilicates ("clay" and serpentinites), sulfides and sulfates, and carbonates,[6] as well as structural signs: veins,[7][8] and alteration or total erasure of individual chondrules.[9][10]

Some meteorites, particularly the CI class,[11] currently contain water.[12] As these include both finds (with their Earth entry and impact unobserved) and falls (meteorites from a known, recent meteor event), that water cannot be entirely terrestrial contamination. As the precision of isotopic abundance analyses grew, they confirmed that meteorite water differs from Earth water.[13] As water at Earth (especially its atmosphere) is well-mixed, significantly different isotope levels would indicate a separate water source.

Water content of the CI and CM types are often in double-digit percentages.

Much telescopic observation and hypothesizing attempted to link meteorite classes to asteroid types.[14] The Galileo and NEAR missions then established S-type asteroids as the parent bodies of ordinary chondrites; the Dawn mission confirmed hypotheses that 4 Vesta was the HED parent. Ongoing projects are sending spacecraft to C-,[15][16] M-, D-,[17] and P-type bodies.

Versus comets

The planets, and to an extent the asteroid belt, were previously held to be static and unchanging; the belt was a former or stalled planet.

In the late 1860s, Hubert Newton and Giovanni Schiaparelli simultaneously showed that meteor showers (and by implication, meteorites) were comet debris.

After the discovery of many near-Earth asteroids, not in the belt, it was apparent they had planet-crossing, unstable orbits. Their number could not have survived from the Solar System's formation, and required replenishment from some other population. Some, such as Opik and Wetherill, hypothesized that most or all NEOs were actually extinct or dormant comets, requiring no ejection process from the main belt. The comets' orbits had become more circular after encounters with planets, possibly augmented by comet jetting. Centaurs, too, required some similar model.

A growing understanding of Solar System dynamics, including more observations, of more bodies, replicated by faster computer models, eliminated this requirement. Kirkwood Gaps were evidence of loss from the main belt, via resonances with the planets. Later, the Yarkovsky effect, insignificant to a planet, could augment mechanisms.

Empirically, meteor cameras began tracing meteor trajectories, which led back to the asteroid belt. The Příbram (1959), Lost City (1970), and Innisfree (1977) meteorites had arrived via Apollo-like, belt-tangent orbits. Even afterward, some maintained that comets best explained carbonaceous chondrite meteorites[18][19] or even ordinary chondrites.[20]

As comets

The issue of asteroids versus comets reemerged with observations of active asteroids- that is, emission from small bodies in what were considered asteroidal orbits, not comet-like orbits (high eccentricity and inclination). This includes both Centaurs, past the snow line, and main belt objects, inside the line and previously assumed dry. Activity could, in some cases, be explained by ejecta, escaping from an impact. However, some asteroids showed activity at perihelion, then at subsequent perihelia. The probability of impacts with this timed pattern was considered unlikely versus a model of comet-like volatile emissions.

Observations of the Geminid meteor shower linked it to (3200) Phaeton, a body in a cometary orbit but with no visible coma or tail, and thus defined as an asteroid. Phaeton was a rock comet, whose emissions are largely discrete particles and not visible.

Observations of (1) Ceres emitting hydroxide (OH), the product of water after exposure to the Sun's ultraviolet levels, were further evidence. Ceres is well within the snow line, exposed to ultraviolet, and Cererean water was considered speculative, at least on its surface.

The IAU General Assembly of 2006 addressed this issue. Overshadowed by Pluto was the creation of Small Solar System Body (SSSB), a category needing no comet-asteroid distinction, nor establishment/disestablishment of volatile emission.

Hydrology and morphology

Micro- and nanoscale water occurs as fluid inclusions in both carbonaceous[8] and ordinary[21] chondrites. However, as "bubble" diameters decrease, search costs increase geometrically. Their characterization is at the state of the art for most analytical techniques,[22] and the method had seen slow progress to this point.[23] Independently-confirmed fluid inclusions are, at minimum, Peetz[24] and Jilin,[25] with many other reports.[26][27]

Minerals which appear waterless to the eye or hand may nevertheless be hydrated. Unfrozen water consists of molecular layers (one to possibly fifteen molecules thick[28]) bound to, and kept from crystallizing by the equal or stronger attraction of the mineral of adsorption.[9][10][6]

Water can persist at higher temperatures than normal in the form of hydrated minerals: those minerals which can bind water molecules at the crystalline level. Salts, including halite (table salt, NaCl) are ionic and attract individual, polar water molecules with electrostatic forces. Alternately, the parent mineral may be e. g., sulfate, and that mineral may retain hydroxide (OH). When freed from the crystal structure, hydroxide reverts to water and oxygen. These are considered water, in the usage of geochemistry and Solar System science.[29][30][31]

Short of this binding, a surface may retain a monolayer or bilayer of water molecules or hydroxide. Phyllosilicate minerals assemble into microscopic plates, sheets, or fibers, rather than bulk crystals. The layers trap water between them; the large surface area created can hold much water. This is also considered water, in the geotechnical, geochemical, and astronomical usages.[32][33][34]

On an even finer level, most rocks are silicates, or in some cases metal oxides, containing an oxygen fraction. Hydrogen content, as substitutions or interstitials, can react with oxygen (displacing its existing cation) to form hydroxide or water. The solar wind is a reducing environment, containing hydrogen atoms and protons (effectively hydrogen, in the form of hydrogen nuclei).[35] Either may be implanted into exposed surfaces, as the small hydrogen atom is highly soluble. A lesser contribution may come from the proton component of cosmic rays. Both pyroxene and olivine, common asteroid minerals, can hydrate in this manner. This, too, is considered water within the geochemistry and geophysics fields.[36][37][38]

Solar System science and asteroid mining ascribe hydrated minerals as containing water,[4][39] in a similar sense as ice giant.[40]

On a macroscopic scale, some thickness of crust may shelter water from evaporation, photolysis and radiolysis, meteoric bombardment, etc. Even where a crust does not originally exist, impurities in ice may form a crust after its parent ice escapes: a lag deposit.

On a geologic scale, the larger asteroids can shield water, phyllosilicate, ice, etc. contents in their interiors via a high thermal mass. Below some depth, the diurnal temperature variation becomes negligible, and the effect of solar insolation- a daytime temperature peak- does not boil out water. A low obliquity helps; while the tropics take solar insolation, two polar regions see little sunlight and can help maintain a low average temperature.

Water parent materials

Phyllosilicates

CI meteorites are mostly phyllosilicates. The phyllosilicates serpentinite, montmorillonite and saponite (clay), tochilinite,[6] chamosite, cronstedtite, and mica have been identified in meteorites.

Sulfates and sulfides

Sulfur is found in meteorites; it has a fairly high cosmic abundance. The abundance in common (chondrite) meteorites is greater than that in Earth's crust; as a differentiated body, our crust has lost some sulfur to an iron core, and some to space as hydrogen sulfide gas. The element is present in all meteorites; carbonaceous chondrites and enstatite chondrites in particular have higher sulfur contents than the ordinary chondrites. In C1 and C2 chondrites, sulfur is found predominantly as free sulfur, sulfate minerals, and in organic compounds at a net 2–5 percent.[41] A slight enrichment is due to cosmic-ray produced S36 and S33.[42]

Sulfur-bearing, hydrated minerals identified via meteorites include epsomite, bloedite, gypsum/bassanite, and jarosite.

Carbonate

As the name implies, carbonaceous chondrites formed with chondrules and carbon. The carbonates whewellite/vaterite, hydromagnesite, calcite/dolomite, aragonite, and breunnerite have been found in meteorites.

By meteorite classification

Type123456
Overall TextureNo chondritesVery sharply defined chondritesVery sharply defined chondritesWell-defined chondritesChondrites readily delineatedPoorly defined chondrites
Texture of matrixAll fine-grained, opaqueMuch opaque matrixOpaque matrixTransparent, micro-crystalline matrixRecrystallized matrixRecrystallized matrix
Bulk carbon content~2.8%~0.6–2.8%~0.2–1.0%<0.2%<0.2%<0.2%
Bulk water content~20%~4-18%<0.2%<0.2%<0.2%<0.2%

-Petrological Scale (Van Schmus, Wood 1967). Since this time, a type seven has been added.

This taxonomy was preceded (Wiik 1956: Type I 20.08% water, Type II 13.35% water[43]) and followed (Keil 1969,[44] Mason 1971[45]), with all in general agreement on these levels.

Meteorites are valuable ground truth. Studies, such as neutron activation analysis, can be performed without the mass and volume constraints of space flight. Meteorites also sample multiple depths of their parent bodies, not just dehydrated crusts or space-weathered rinds.

Yet meteorites are not sufficient. The body of meteoritics is dominated by durable examples,[46][47] and deficient in classes and subclasses;[48] one or more types may be missing entirely.[49] Earth entry and exposure may then alter or remove some materials, while contaminating others.[23][50] Such meteorites have speculative or unknown parent bodies, and no wider context of the sample versus the rest of that parent body.[2]

Carbonaceous chondrites

Different carbonaceous chondrites show different signs of water, including extant water.[51][52] Identifying parent bodies for CC meteorites is an ongoing subject, but they are generally held to be the low-albedo bodies: the C-complex (C-, B-, F-, G-, and D/P-types).[53][54]

As darker bodies, generally farther out in the asteroid belt (or beyond) than the S-types, these are more difficult to study. Carbonaceous materials have flatter, less revealing spectra. CC parentage is also complicated by space weathering. C-complex bodies weather to different types and degrees than the silicate (S-type, and lunar) surfaces.

CI chondrites

The rare CI chondrites are so severely altered by water, they consist predominantly (~90%) of phyllosilicate matrix; chondrules are entirely dissolved, or very faint. All are type 1 (CI1), per the above scale. Berzelius first reported clay in the Orgueil meteorite, causing him to at first doubt it was extraterrestrial.

On a macroscopic scale, CI material is layered serpentinite/saponite. Microscopically, CI material appearance was first described as "spinach."[6][55] These layers trap significant amounts of water; CI hydration is over 10%, at times ~20%.

As phyllosilicates are brittle, they are less likely to survive Earth entry and impact. Being water-soluble, they are unlikely to survive exposure, and there were no CI finds until the Antarctic meteorite era.

CM chondrites

CM meteorites loosely resemble CI, but altered to lesser extents. More chondrules appear, leaving less matrix. Accordingly, they are more mineralized and less hydrous. CMs are often, but not always, petrologic type 2. Cronstedtite tends to replace saponite, though as the most common CC subclass, properties range widely.[8][56][57][58]

CR chondrites

CR meteorites loosely resemble CM, but appear to have formed in a reducing environment, not an oxidizing one. It is held that they formed in a similar manner but different zone of the Solar System than CMs. Water content is lower than in CM; still, serpentinites, chlorite, and carbonates appear. GRO 95577 and Al Rais meteorites are exceptional CRs.[59][60]

CV chondrites

The CV chondrites show signs of prior water. However, surviving water is low.[61][62]

Ordinary chondrites

Though clearly drier, ordinary chondrites nevertheless show trace phyllosilicates. The Semarkona meteorite is an exceptionally wet OC.[63] Salts (halite and the related sylvite) carry brine inclusions; while the community first posited that the salts must be exogenous, the issue is ongoing.[64][21] In parallel, OC minerals show evidence of water formations.[65][66][67]

The parents of OCs are generally taken as the S-type asteroids.

R chondrites

R chondrites contain amphibole minerals, and lesser biotites and apatites. As with the other classes and subclasses, the R chondrites show clasts of foreign materials, including phyllosilicate (water-bearing serpentinite-saponite) inclusions.[68] The LAP 04840 and MIL 11207 meteorites are particularly hydrous R chondrites.[69][70]

Achondrite meteorites

HED meteorites

Like ordinary chondrites, the HEDs (howardites, eucrites, and diogenites) were assumed to have formations and histories that would prevent water contents. Actual measurements of clasts and elements indicate the HED parent body received carbonaceous chondrite materials, including their water.[71][72]

The parent body of HEDs is a V-type asteroid, of which (4) Vesta is widely assumed.

Angrite meteorites

Like ordinary chondrites, the angrites were assumed to have formations and histories that would prevent water contents. Actual measurements of clasts and elements indicate the angrite parent body received carbonaceous chondrite materials, including their water.[73][74]

Micrometeorites and dust particles

The smallest solid objects can have water. At Earth, falling particles returned by high-altitude planes and balloons show water contents. In the outer Solar System, atmospheres show water spectra where water should have been depleted. The atmospheres of giant planets and Titan are replenished by infall from an external source. Micrometeorites and interplanetary dust particles contain H
2O, some CO, and possibly CO2.[75][76][77]

It was assumed that monolithic minerals are asteroid debris, while dust particles, with a "fluffy", fractal-like aggregated structure, were assumed to be cometary. But these micro-impactors have asteroid-like isotopic ratios, not comet-like.[63][78][79]

Via remote sensing

Visible/near-infrared spectroscopy

The spectrum of water and water-bearing minerals have diagnostic features. Two such signs, in the near-infrared, extending somewhat into visible light, are in common use.

Water, hydroxyl, and some hydrated minerals have spectral features at wavelengths of 2.5–3.1 micrometers (um). Besides fundamental lines or bands is an overtone of a longer-wave (~6 um) feature. Wavelengths may shift in mineral combinations, or with temperature. The result is a wide absorption band in the light reflecting from such bodies.[33][80][81]

Asteroid (162173) Ryugu, the target of the Hayabusa 2 mission, is expected to be hydrated where (25143) Itokawa was not. Hayabusa 1's NIRS (Near-Infrared Spectrometer) design was then shifted from its maximum wavelength of 2.1 um,[82] to Hayabusa 2's NIRS3 (1.8-3.2 um), to cover this spectral range.[83]

An absorption feature at ~0.7 micrometer is from the Fe2+ to Fe3+ transition, in iron-bearing phyllosilicates.[84][85] The 0.7 um feature is not taken as sufficient. While many phyllosilicates contain iron, other hydrated minerals do not, including non-phyllosilicates. In parallel, some non-hydrated minerals have absorption features at 0.7 um. The advantage of such observing is that 0.7 um is in the sensitivity range of common silicon detectors, where 3 um requires more exotic sensors.

Other spectral ranges

Lesser signs of water include ultraviolet/visible (OH 0-0, 308 Å[86]), mid-infrared,[87] and longer.

Neutron spectroscopy

The hydrogen nucleus- one proton- is essentially the mass of one neutron. Neutrons striking hydrogen then rebound with a characteristic speed. Such thermal neutrons indicate hydrogen versus other elements, and hydrogen often indicates water. Neutron fluxes are low, so detection from Earth is infeasible. Even flyby missions are poor; orbiters and landers are needed for significant integration times.

Direct imaging

Most small bodies are dots or single pixels in most telescopes. If such a body appears as an extended object, a coma of gas and dust is suspected, especially if it shows radial falloff, a tail, temporal variation, etc. Though other volatiles exist, water is often assumed to be present.

Native ice is difficult to image. Ice, particularly as small grains, is translucent, and tends to be masked by a parent material, or even sufficient levels of some impurities.

Sample science

A sample in hand can be checked for fluid inclusions ("bubbles")[64][8] versus remote sensing, or even contact science; most volatiles are lost at a depth greater than the skin depth. Near- and mid-IR spectroscopy are also easier at benchtop range. Other measurements of water include nuclear magnetic resonance (NMR), nanoSIMS; energy dispersive X-ray spectroscopy (EDS), and eventually thermogravimetric analysis (TGA)- driving off any water content.

Examples

(2060) Chiron

The Centaur 2060 Chiron, in a generally circular orbit, was assumed to be asteroidal, and given an asteroid number. However, at its first perihelion since its discovery and presumably warmer, it formed a coma, indicating loss of volatiles like a comet.

Mercury polar deposits

Asteroidal impacts have sufficient water to form Mercury's polar ices, without invoking comets. Any cometary water (including dormant, transitional objects) would be additional.[88][89] Not only are asteroids sufficient, but micrometeoroids/dust particles have the required water content; conversely, many of the asteroids in Mercury-crossing orbits may actually be defunct comets.[90]

Earth/Moon system

Claimed water at the lunar poles was, at first, attributed to comet impacts over the eons. This was an easy explanation. Subsequent analyses, including analyses of Earth-Moon isotopes versus comet isotopes, showed that comet water does not match Earth-Moon isotopes, while meteoritic water is very close.[53][91][92][93] The cometary water contribution may be as little as zero.[94] At Earth's Moon, comet impact velocities are too high for volatile materials to remain, while asteroid orbits are shallow enough to deposit their water.[95][96] Traces of carbonaceous chondrites- and thus, water- are observable in lunar samples.[97] Only a small portion (if any) of comets contributed to the volatile content of the inner Solar System bodies.[73][98]

(24) Themis

Water on Themis, an outer-belt object, was directly observed. It is hypothesized that a recent impact exposed an ice deposit.[99][100] Other members of the Themis family, likely fragments of Themis itself or a larger parent now lost, also show signs of water.[101][102][103]

Active asteroids Elst-Pizarro, (118401)1999 RE70,[104] and possibly 238P/Read[105] are family members.

(65) Cybele

As with Themis, Cybele is an outer-belt, C-type or C-complex object at which a spectra of volatiles has been observed.[99][106]

(4) Vesta

Vesta was thought to be dry; it is in an inner, warmer zone of the asteroid belt, and its minerals (identified by spectroscopy) had volcanic origins which were assumed to have driven off water. For the Dawn mission, it would serve as a counterexample to hydrated (1) Ceres. However, at Vesta, Dawn found significant water. Reddy estimates the total Vestan water at 30 to 50 times that of Earth's Moon.[107] Scully et al. also claim that slumping on Vesta indicates the action of volatiles.[108]

(1) Ceres

The Herschel telescope observed far-infrared emission spectra from Ceres indicating water loss. Though debatable at the time, the subsequent Dawn probe would use a different method (thermal neutrons) to detect subsurface hydrogen (in water or ammonium[109]) at high Cererean latitudes, and a third method (near-infrared spectra) for likely local emissions. A fourth line of evidence, relaxation of large craters, suggests a mechanically weak subsurface such as frozen volatiles.

The feature Ahuna Mons is most likely cryovolcanic: a Cererean pingo.

(16)Psyche

Psyche, despite being an M-type asteroid, shows the spectral signs of hydrated minerals.[110]

(25143) Itokawa

Water has been found in samples retrieved by the Hayabusa 1 mission. Despite being an S-type near-Earth asteroid, assumed dry, Itokawa is hypothesized to have been "a water-rich asteroid" before its disruption event. This remaining hydration is likely asteroidal, not terrestrial contamination. The water shows isotopic levels similar to carbonaceous chondrite water,[111] and the sample canister was sealed with double O-rings.[112][113]

(101955) Bennu

Maltagliati proposed that Bennu has significant volatiles content, similar to Ceres.[114] This was confirmed in the mechanical sense, with activity observed in separate events, not associated with impacts.[115][116]

The OSIRIS-REx spacecraft, on arriving at Bennu, found its surface to be mostly phyllosilicates[117] that hold water.[118][119]

(162173) Ryugu

Ryugu, the target of the Hayabusa2 mission, showed activity which may be an impact, escape of volatiles, or both.[120]

Hayabusa2, after an initial calibration adjustment, confirmed "The decision to choose Ryugu as the destination, based on the prediction that there is some water, was not wrong" (-Kohei Kitazato[121]).[122]

Indirect candidates

Jupiter trojans

The snow line of this system is inside of Jupiter, making the Jupiter Trojans likely candidates for high water contents. Yet few signs of water have been found in spectroscopes. The hypothesis is that, past the snow line on a small body, such water is bound as ice. Ice is unlikely to participate in reactions to form hydrated minerals, or to escape as water/OH, both of which are spectrally distinct where solid ice is not.

The exception is 617 Patroclus; it may also have formed farther out, then been captured by Jupiter.

2 Pallas

Broadly similar to Ceres, 2 Pallas is a very large SSSB in the cooler, middle main belt. While the exact typing of Pallas is somewhat arbitrary, it, like Ceres, is not S-, M-, or V-type. The C-complex bodies are considered more likely to contain significant water.[123][124]

Dormant comets

The category of Damocloids is defined as high-inclination, high-eccentricity bodies with no visible activity. In other words, they appear asteroid-like, but travel in cometary orbits.

107P/Wilson-Harrington is the first unambiguous ex-comet. After its 1949 discovery, Wilson-Harrington was not observed again in what should have been perihelion passages. In 1979, an asteroid was found and given the provisional designation 1979 VA, until its orbit could be determined to a sufficient level. That orbit matched that of comet Wilson-Harrington; the body is now dual-designated as (4015) Wilson-Harrington, too.

Other candidates include 944 Hidalgo, 1983 SA, (2101) Adonis, (2201) Oljato, (3552) Don Quijote

Weak comets, perhaps not to the stage of Wilson-Harrington, include Arend-Rigauz and Neujmin 1.

(4660) Nereus, the original target of the Hayabusa mission, was selected both for its very accessible orbit, and the possibility that it is an extinct or dormant comet.

331P/Gibbs

Active asteroid 331P/Gibbs also has a small, close, and dynamically stable family (cluster) of other objects.[125][126]

(6478) Gault

Asteroid (6478) Gault showed activity in late October/early November 2018; however, this alone could be impact ejecta. Activity subsided in December, but resumed in January 2019, making it unlikely to be solely one impact.

As a resource

Propellant

The Tsiolkovskiy equation governs rocket travel. Given the velocities involved with space flight, the equation dictates that mission mass is dominated by propellant requirements, increasing as missions progress beyond low-Earth orbit.

Asteroidal water can be used as a resistojet propellant. The application of large amounts of electricity (electrolysis) may decompose water into hydrogen and oxygen, which can be used in chemical rockets. When combined with the carbon present in carbonaceous chondrites (more likely to have high water content), these can synthesize oxygen and methane (both storable in space with a passive thermal design, unlike hydrogen), oxygen and methanol, etc. As an in-space resource, asteroidal mass does not need to be lifted out of a gravity well. The cost of propellant then, in terms of other propellant, is lower by a multiplier set by the Tsiolkovskiy equation.

Multiple organizations have and intend to use water propellants.[127][128][129]

Radiation shielding

Water, as a reasonably dense material, can be used as a radiation shield. In microgravity, bags of water or water-filled spaces need little structural support. Another benefit is that water, having elements with moderate and low Z, generates little secondary radiation when struck. It can be used to block the secondary radiation from higher-Z materials, forming a graded-Z shield. This other material may be the spoil or gangue/tailings from asteroid processing.[130][131][132]

Growth medium

Carbonaceous chondrites contain water, carbon, and minerals necessary for plant growth.[133]

See also

Bibliography

  • Kerridge J, Bunch T (1979). "Aqueous Activity on Asteroids: Evidence from Carbonaceous Meteorites in Asteroids.". In Gehrels T, Mathews M (eds.). Asteroids. University of Arizona Press. ISBN 978-0-8165-0695-8.
  • Roedder E, ed. (1984). Fluid Inclusions. Mineralogical Society of America. ISBN 0-939950-16-2.
  • Zolensky M, McSween H (1988). "Aqueous Alteration". In Kerridge J, Matthews M (eds.). Meteorites and the early solar system. University of Arizona Press. p. 114. OCLC 225496581.
  • Lewis J, Hutson M (1993). "Asteroidal Resource Opportunities Suggested by Meteorite Data". In Lewis J, Matthews M, Guerrieri M (eds.). Resources of Near-Earth Space. University of Arizona Press. p. 523. ISBN 978-0-8165-1404-5.
  • Nichols C (1993). "Volatile Products from Carbonaceous Asteroids". In Lewis J, Matthews M, Guerrieri M (eds.). Resources of Near-Earth Space. University of Arizona Press. p. 543. ISBN 978-0-8165-1404-5.
  • Lodders K, Osborne R (1999). "Perspectives on the Comet-Asteroid-Meteorite Link". In Altwegg K, Ehrenfreund P, Geiss J, Huebner WF, Geiss J (eds.). Composition and Origin of Cometary Materials. Dordrecht: Springer. pp. 289–297. ISBN 978-0-7923-6154-1.
  • Jewitt D, Chizmadia L, Grimm R, Prialnik D (2002). "Water in the Small Bodies of the Solar System". In Bottke WF, Cellino A, Paolicchi P, Binzel RP (eds.). Asteroids III. University of Arizona Press. p. 863. ISBN 978-0-8165-2281-1.
  • Keppler H, Smyth JR (2006). Keppler H, Smyth J (eds.). Water in Nominally Anhydrous Minerals. ISBN 978-0-939950-74-4.
  • Rivkin AS, Campins H, Emery J, Howell E (2015). "Astronomical Observations of Volatiles on Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. pp. 65–88. ISBN 978-0-8165-3218-6.
  • Binzel R, Reddy V, Dunn T (2015). "The Active Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. p. 221. ISBN 978-0-8165-3218-6.
  • Wilson L, Bland PA, Buczkowski D, Keil K, Krot AN (2015). "Hydrothermal and Magmatic Fluid Flow in Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. p. 553. ISBN 978-0-8165-3218-6.
  • Krot AN, Nagashima K, Alexander CM, Ciesla FJ, Fujiya W, Bonal L (2015). "Sources of Water and Aqueous Activity on the Chondrite Parent Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. p. 635. ISBN 978-0-8165-3218-6.
  • Snodgrass C, Agarwal J, Combi M, Fitzsimmons A, Guilbert-Lepoutre A, Hsieh HH, et al. (November 2017). "The main belt comets and ice in the solar system". The Astronomy and Astrophysics Review. 25 (1): 5. arXiv:1709.05549. Bibcode:2017A&ARv..25....5S. doi:10.1007/s00159-017-0104-7. S2CID 7683815.

References

  1. ↑ Rubin, A (1997). "Mineralogy of Meteorite Groups". Meteoritics & Planetary Science. 32 (2): 231–247. Bibcode:1997M&PS...32..231R. doi:10.1111/j.1945-5100.1997.tb01262.x.
  2. 1 2 "Extraterrestrial H2O hunters". Retrieved 14 Jan 2019.
  3. ↑ Dudley, J; Greenwood, J; Sakamoto, N; Abe, K; Kuroda, M; Yurimoto, H (2018). Water contents of angrites, eucrites, and ureilites and new methods for measuring hydrogen in pyroxene using SIMS. 49th LPSC.
  4. 1 2 Crawford, I (Feb 2015). "Lunar Resources: A Review". Progress in Physical Geography: Earth and Environment. 39 (2): 137–167. arXiv:1410.6865. Bibcode:2015PrPhG..39..137C. doi:10.1177/0309133314567585. S2CID 54904229.
  5. ↑ Keppler H, Smyth JR (2006). Keppler H, Smyth J (eds.). Water in Nominally Anhydrous Minerals. ISBN 978-0-939950-74-4.
  6. 1 2 3 4 Zolensky M, McSween H (1988). "Aqueous Alteration". In Kerridge JF, Matthews MS (eds.). Meteorites and the early solar system. University of Arizona Press. p. 114. OCLC 225496581.
  7. ↑ Tomeoka, K; Buseck, P (1990). "Phyllosilicate veins in a CI meteorite: evidence for queous alteration on the parent body". Nature. 345 (6271): 138–40. Bibcode:1990Natur.345..138T. doi:10.1038/345138a0. S2CID 4326128.
  8. 1 2 3 4 Saylor, J; Zolensky, M; Bodnar, R; Le, L; Schwandt, C (2001). Fluid inclusions in carbonaceous chondrites. Lunar and Planetary Science Conference. p. 1875.
  9. 1 2 Gooding J (1984). "Aqueous alteration on meteorite parent bodies: Possible role of "unfrozen" water and the Antarctic meteorite analogy". Meteoritics. 9: 228. Bibcode:1984Metic..19Q.228G.
  10. 1 2 Rietmeijer F (1985). "A model for diagenesis in proto-planetary bodies". Nature. 313 (6000): 293–294. Bibcode:1985Natur.313..293R. doi:10.1038/313293a0. S2CID 4314270.
  11. ↑ Bland PA, Alard O, Benedix GK, Kearsley AT, Menzies ON, Watt LE, Rogers NW (September 2005). "Volatile fractionation in the early solar system and chondrule/matrix complementarity". Proceedings of the National Academy of Sciences. 102 (39): 13755–60. Bibcode:2005PNAS..10213755B. doi:10.1073/pnas.0501885102. PMC 1224360. PMID 16174733.
  12. ↑ Clayton RN (August 1999). "Primordial water". Science. 285 (5432): 1364–5. doi:10.1126/science.285.5432.1364. PMID 10490412. S2CID 32334341.
  13. ↑ Robert, F; Deloule, E (2002). Using the D/H ratio to estimate the terrestrial water contamination in chondrites. LPS XXXIII.
  14. ↑ McSween H (1996). "The role of meteoritics in spaceflight missions and vice versa". Meteoritics & Planetary Science. 31 (6): 727–738. Bibcode:1996M&PS...31..727M. doi:10.1111/j.1945-5100.1996.tb02108.x.
  15. ↑ "OSIRIS-REx: Asteroid Sample Return Mission". Arizona Board of Regents. Retrieved 17 Jan 2019.
  16. ↑ "Asteroid Explorer "Hayabusa2"". Japan Aerospace Exploration Agency. Retrieved 17 Jan 2019. "thus we expect to clarify the origin of life by analyzing samples acquired from a primordial celestial body such as a C-type asteroid to study organic matter and water in the solar system..."
  17. ↑ "MMX: Martian Moons Exploration". Japan Aerospace Exploration Agency. Archived from the original on 14 August 2017. Retrieved 17 Jan 2019.
  18. ↑ Wasson J, Wetherill G (1979). Gehrels T, Mathews M (eds.). Asteroids. University of Arizona Press. p. 926. ISBN 978-0-8165-0695-8.
  19. ↑ Wetherill, G; Revelle, D (1982). Comets, Wilkening L. University of Arizona Press. p. 297.
  20. ↑ Wood, C. Fall statistics of H chondrites: Evidence of cometary origins from ordinary chondrites. LPSC XIII. pp. 873–874.
  21. 1 2 Chan, Q (Jan 2018). "Organic matter in extraterrestrial water-bearing salt crystals". Science Advances. 4 (1): eaao3521. doi:10.1126/sciadv.aao3521. PMC 5770164. PMID 29349297.
  22. ↑ Bodnar, R; Dolocan, A; Zolensky, M; Lamadrid, H; Kebukawa, Y; Chan, Q (2019). First Direct Measurements Of Compositions Of Early Solar System Aqueous Fluids. 50th LPSC.
  23. 1 2 Zolensky, M (17 Apr 2017). "The Search for and Analysis of Direct Samples of Early Solar System Aqueous Fluids". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 375 (2094): 20150386. Bibcode:2017RSPTA.37550386Z. doi:10.1098/rsta.2015.0386. PMC 5394253. PMID 28416725.
  24. ↑ Warner, J; Ashwal, L; Bergman, S; Gibson, E; Henry, D; Lee‐Berman, R; Roedder, E; Belkin, H (10 February 1983). "Fluid inclusions in stony meteorites". Journal of Geophysical Research: Solid Earth. 88 (S02): A731-35. Bibcode:1983LPSC...13..731W. doi:10.1029/JB088iS02p0A731.
  25. ↑ Rudnick, R; Ashwal, L; Henery, D; Gibson, E; Roedder, E; Belkin, H (15 Feb 1985). "Fluid inclusions in stony meteorites - A cautionary note". Journal of Geophysical Research. 90: C669-75. Bibcode:1985JGR....90..669R. doi:10.1029/JB090iS02p0C669. PMID 11542002.
  26. ↑ Guilhaumou, N (May 2006). Fluid and melt inclusions in meteorites: clues to the petrology of asteroids and planets in the solar system. ACROFI I.
  27. ↑ Zolensky, M; Bodnar, R; Yurimoto, H; Itoh, S; Fries, M; Steele, A; Chan, Q; Tsuchiyama, A; Kebukawa, Y; Ito, M (17 April 2017). "The search for and analysis of direct samples of early Solar System aqueous fluids". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 375 (2094): 20150386. Bibcode:2017RSPTA.37550386Z. doi:10.1098/rsta.2015.0386. PMC 5394253. PMID 28416725.
  28. ↑ Franks, Felix (1981). Water: A Comprehensive Treatise v. 5 (2nd ed.). New York: Plenum Press. p. 100. ISBN 0-306-37185-5. 4.3.4 Silicas
  29. ↑ Kaplan, I. Handbook of Elemental Abundances in Meteorites. p. 21.Chapter: Hydrogen (1)
  30. ↑ Hamilton, V (2014-05-18). "The OSIRIS-REx Thermal Emission Spectrometer (OTES) – Our Heat Sensor and Mineral Mapper". Life on the Asteroid Frontier. Retrieved 24 Mar 2019. "...minerals of particular interest, such as those that contain water"
  31. ↑ Hamilton, V Simon A Christensen P Reuter D Clark B Barucci M Bowles N Boynton W Brucato J Cloutis E Connolly H Donaldson Hanna K Emery J Enos H Fornasier S Haberle C Hanna R Howell E; Kaplan H Keller L (Mar 2019). "Evidence for widespread hydrated minerals on asteroid (101955) Bennu" (PDF). Nature Astronomy. 3 (332–340): 332–340. Bibcode:2019NatAs...3..332H. doi:10.1038/s41550-019-0722-2. hdl:1721.1/124501. PMC 6662227. PMID 31360777.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  32. ↑ Palme, H; Boynton, W (1993). Protostars and Planets. University of Arizona Press. p. 979. ISBN 9780816513345.Chapter: Meteoritic constraints on conditions in the solar nebula
  33. 1 2 Milliken R, Mustard J (2005). "Quantifying absolute water content of minerals using near-infrared reflectance spectroscopy". J. Geophys. Res. 110 (E12): E12001. Bibcode:2005JGRE..11012001M. CiteSeerX 10.1.1.654.2409. doi:10.1029/2005JE002534.
  34. ↑ Russell S; Ballentine C; Grady M (17 Apr 2017). "The origin, history and role of water in the evolution of the inner Solar System". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 375 (2094): 20170108. Bibcode:2017RSPTA.37570108R. doi:10.1098/rsta.2017.0108. PMC 5394259. PMID 28416731. "Water in chondrites is contained within clay minerals"
  35. ↑ Rivkin A, Howell E, Emery J, Sunshine J (Apr 2018). "Evidence for OH or H2O on the surface of 433 Eros and 1036 Ganymed". Icarus. 304: 74. arXiv:1704.04776. Bibcode:2018Icar..304...74R. doi:10.1016/j.icarus.2017.04.006. S2CID 118823980.
  36. ↑ S, Mackwell; Kohlstedt, D (1985). "The role of water in the deformation of olivine single crystals". Journal of Geophysical Research. 90 (B13): 1319–1333. Bibcode:1985JGR....9011319M. doi:10.1029/JB090iB13p11319.
  37. ↑ Kurosawa, M; Yurimoto, Y; Sueno, S (Jan 1993). Water in Earth's mantle: Hydrogen analysis of mantle olivine, pyroxenes and garnet using the SIMS. 24th LPSC. pp. 839–840.
  38. ↑ Griffin, J; Berry, A; Frost, D; Wimperis, S; Ashbrook, S (2013). "Water in the Earth's mantle: a solid-state NMR study of hydrous wadsleyite". Chemical Science. 4 (4): 1523. doi:10.1039/c3sc21892a. hdl:1885/77486.
  39. ↑ Lewis, J (2014). "VIII. Asteroid Resources". Asteroid Mining 101: Wealth for the New Space Economy. ISBN 9780990584216.
  40. ↑ Williams, M. "The gas (and ice) giant Neptune". Phys.org. Retrieved 25 Jan 2019.
  41. ↑ Moore C (1971). Ch.: Sulfur, in Handbook of Elemental Abundances in Meteorites, B. Mason ed. Gordon and Breach. p. 137. ISBN 978-0-677-14950-9.
  42. ↑ Hulston J, Thode H (1965). "Cosmic-ray produced S36 and S33 in the metallic phase of iron meteorites". Journal of Geophysical Research. 70 (18): 4435. Bibcode:1965JGR....70.4435H. doi:10.1029/JZ070i018p04435.
  43. ↑ Wiik, H (1956). "The Chemical Composition of Some Stony Meteorites". Geochimica et Cosmochimica Acta. 9 (5): 279. Bibcode:1956GeCoA...9..279W. doi:10.1016/0016-7037(56)90028-X.
  44. ↑ Keil, K (1969). "4". The Handbook of Geochemistry, Part 1. Springer.
  45. ↑ Mason, B (1971). Handbook of Elemental Abundances in Meteorites. Gordon Breach, Science Publishers, Inc. ISBN 0-677-14950-6.chapter: Introduction
  46. ↑ remo, J (1994). Hazards Due to Comets & Asteroids. pp. 552–554.
  47. ↑ Heck, P; Schmidz, B; Bottke, B; Rout, S; Kita, N; Anders, A; Defouilloy, C; Dronov, A; Terfelt, F (Jan 2017). "Rare meteorites common in the Ordovician period". Nature Astronomy. 1 (2): 0035. Bibcode:2017NatAs...1E..35H. doi:10.1038/s41550-016-0035. S2CID 102488048.
  48. ↑ Chan Q, Chikaraishi Y, et al. (Jan 2016). "Amino acid compositions in heated carbonaceous chondrites and their compound-specific nitrogen isotope ratios". Earth and Planetary Science Letters. 68: 7. Bibcode:2016EP&S...68....7C. doi:10.1186/s40623-016-0382-8.
  49. ↑ Krot AN, Nagashima K, Alexander CM, Ciesla FJ, Fujiya W, Bonal L (2015). "Sources of Water and Aqueous Activity on the Chondrite Parent Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. p. 635. ISBN 978-0-8165-3218-6.
  50. ↑ Dworkin, J (2018). "OSIRIS-REx Contamination Control Strategy and Implementation". Space Science Reviews. 214 (1): 19. arXiv:1704.02517. Bibcode:2018SSRv..214...19D. doi:10.1007/s11214-017-0439-4. PMC 6350808. PMID 30713357.
  51. ↑ Vdovykin, G (1973). "The Mighei Meteorite". Space Science Reviews. 14 (6): 832–79. Bibcode:1973SSRv...14..832V. doi:10.1007/bf00224777. S2CID 120513472. section A. Major Elements
  52. ↑ Rudraswami, N (2019). "Chemical, isotopic and amino acid composition of Mukundpura CM2.0 (CM1) chondrite: Evidence of parent body aqueous alteration". Geoscience Frontier. 10 (2): 495–504. Bibcode:2019GeoFr..10..495R. doi:10.1016/j.gsf.2018.02.001. "The water content of ~9.8 WT.% is similar to that found in many CM chondrites." "...presence of abundant water"
  53. 1 2 Alexander CM, Bowden R, Fogel ML, Howard KT, Herd CD, Nittler LR (August 2012). "The provenances of asteroids, and their contributions to the volatile inventories of the terrestrial planets". Science. 337 (6095): 721–3. Bibcode:2012Sci...337..721A. doi:10.1126/science.1223474. PMID 22798405. S2CID 206542013.
  54. ↑ Marrocchi, Y; Bekaert, D; Piani, L (2018). "Origin and abundance of water in carbonaceous asteroids" (PDF). Earth and Planetary Science Letters. 482: 23–32. Bibcode:2018E&PSL.482...23M. doi:10.1016/j.epsl.2017.10.060.
  55. ↑ Buseck, P; Hua, X (1993). "Matrices Of Carbonaceous Chondrite Meteorites". Annu. Rev. Earth Planet. Sci. 21: 255–305. Bibcode:1993AREPS..21..255B. doi:10.1146/annurev.ea.21.050193.001351.
  56. ↑ de Leuw, S; Rubin, A; Wasson, J (Jul 2010). "Carbonates in CM chondrites: Complex formation histories and comparison to carbonates in CI chondrites". Meteoritics & Planetary Science. 45 (4): 513. Bibcode:2010M&PS...45..513D. doi:10.1111/j.1945-5100.2010.01037.x. S2CID 14208785.
  57. ↑ Piani, L; Yurimoto, H; Remusat, L (2018). "A dual origin for water in carbonaceous asteroids revealed by CM chondrites". Nature Astronomy. 2 (4): 317–323. arXiv:1802.05893. Bibcode:2018NatAs...2..317P. doi:10.1038/s41550-018-0413-4. S2CID 54818758.
  58. ↑ Fujiya, W (2018). "Oxygen isotopic ratios of primordial water in carbonaceous chondrites". Earth and Planetary Science Letters. 481: 264. Bibcode:2018E&PSL.481..264F. doi:10.1016/j.epsl.2017.10.046.
  59. ↑ Weisberg, M; Prinz, M; Clayton, R; Mayeda, T (Apr 1993). "The CR (Renazzo-type) carbonaceous chondrite group and its implications". Geochim. Cosmochim. Acta. 57 (7): 1567–1586. Bibcode:1993GeCoA..57.1567W. doi:10.1016/0016-7037(93)90013-M.
  60. ↑ Bonal, L; Alexander, C; Huss, G; Nagashima, K; Quirico, E; Beck, P (2013). "Hydrogen isotopic composition of the water in CR chondrites". Geochimica et Cosmochimica Acta. 106: 111–133. Bibcode:2013GeCoA.106..111B. doi:10.1016/j.gca.2012.12.009. S2CID 95276139.
  61. ↑ Keller, L; McKay, D (1993). "Aqueous alteration of the Grosnaja CV3 carbonaceous chondrite". Meteoritics. 23 (3): 378. Bibcode:1993Metic..28R.378K.
  62. ↑ Piani, L; Marrocchi, Y (Dec 2018). "Hydrogen isotopic composition of water in CV-type carbonaceous chondrites". Earth and Planetary Science Letters. 504: 64–71. Bibcode:2018E&PSL.504...64P. doi:10.1016/j.epsl.2018.09.031.
  63. 1 2 Alexander, C; Barber, D; Hutchinson, R (1989). "The microstructure of Semarkona and Bishunpur". Geochimica et Cosmochimica Acta. 53 (11): 3045–57. Bibcode:1989GeCoA..53.3045A. doi:10.1016/0016-7037(89)90180-4.
  64. 1 2 Zolensky, M; Bodnar, R; Gibson, E; Nyquist, L (27 Aug 1999). "Asteroidal water within fluid inclusion-bearing halite in an H5 chondrite, Monahans". Science. 285 (5432): 1377–9. doi:10.1126/science.285.5432.1377. PMID 10464091. S2CID 12819160.
  65. ↑ Doyle, P (23 Jun 2015). "Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite". Nature Communications. 6: 7444. Bibcode:2015NatCo...6.7444D. doi:10.1038/ncomms8444. PMID 26100451.
  66. ↑ Jones, R (2016). "Phosphate Minerals in the H Group of Ordinary Chondrites, and Fluid Activity Recorded in Apatite Heterogeneity in the Zag H3-6 Regolith Breccia". American Mineralogist. 101 (11): 2452–2467. Bibcode:2016AmMin.101.2452J. doi:10.2138/am-2016-5728. S2CID 99985776.
  67. ↑ Deloule, E; Robert, F (Nov 1995). "Interstellar water in meteorites?". Geochim. Cosmochim. Acta. 59 (22): 4695–4706. Bibcode:1995GeCoA..59.4695D. doi:10.1016/0016-7037(95)00313-4. PMID 11539426.
  68. ↑ Greshake, A (May 2014). "A strongly hydrated microclast in the Rumuruti chondrite NWA 6828: Implications for the distribution of hydrous material in the solar system". Meteoritics & Planetary Science. 49 (5): 824–841. Bibcode:2014M&PS...49..824G. doi:10.1111/maps.12295.
  69. ↑ McCanta, M; Treiman, A; Dyar, M; Alexander, C; Rumble, D; Essene, E (Dec 2008). "The LaPaz Icefield 04840 meteorite: Mineralogy, metamorphism, and origin of an amphibole- and biotite-bearing R chondrite". Geochimica et Cosmochimica Acta. 72 (23): 5757–5780. Bibcode:2008GeCoA..72.5757M. doi:10.1016/j.gca.2008.07.034.
  70. ↑ Gross, J; Treiman, A; Connolly, H (2013). A New Subgroup Of Amphibole-Bearing R-Chondrite: Evidence From The New R-Chondrite MIL 11207. 80th Annual Meteoritical Society.
  71. ↑ Sarafian, A; Roden, M; Patino-Douce, E (2013). "The volatile content of Vesta: Clues from apatite in eucrites". Meteoritics & Planetary Science. 48 (11): 2135–2154. Bibcode:2013M&PS...48.2135S. doi:10.1111/maps.12124.
  72. ↑ Barrett, T (2016). "The abundance and isotopic composition of water in eucrites" (PDF). Meteoritics & Planetary Science. 51 (6): 1110–1124. Bibcode:2016M&PS...51.1110B. doi:10.1111/maps.12649.
  73. 1 2 Sarafian, A (17 Apr 2017). "Early Accretion of Water and Volatile Elements to the Inner Solar System: Evidence from Angrites". Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences. 375 (2094): 20160209. Bibcode:2017RSPTA.37560209S. doi:10.1098/rsta.2016.0209. PMC 5394258. PMID 28416730.
  74. ↑ Sarafian, A (7 June 2017). "Angrite meteorites record the onset and flux of water to the inner solar system". Geochimica et Cosmochimica Acta. 212: 156–166. Bibcode:2017GeCoA.212..156S. doi:10.1016/j.gca.2017.06.001.
  75. ↑ Rietmeijer, Frans J. M.; MacKinnon, Ian D. R. (1985). "Layer silicates in a chondritic porous interplanetary dust particle". Journal of Geophysical Research. 90: 149–155. Bibcode:1985JGR....90..149R. doi:10.1029/JB090iS01p00149.
  76. ↑ Engrand, C (1999). "Extraterrestrial water in micrometeorites and cosmic spherules from Antarctica: an ion microprobe study". Meteoritics & Planetary Science. 34 (5): 773–786. Bibcode:1999M&PS...34..773E. doi:10.1111/j.1945-5100.1999.tb01390.x. S2CID 128466002.
  77. ↑ Aleon, J; Engrand; Robert, F; Chaussidon, M (2001). "Clues to the origin of interplanetary dust particles from the isotopic study of their hydrogen-bearing phases". Geochimica et Cosmochimica Acta. 65 (23): 4399–4412. Bibcode:2001GeCoA..65.4399A. doi:10.1016/S0016-7037(01)00720-7.
  78. ↑ Aleon, J; Engrand, C; Robert, F; Chaussidon, M (2001). "Clues on the origin of interplanetary dust particles form the isotopic study of their hydrogen-bearing phases". Geochimica et Cosmochimica Acta. 65 (23): 4399–4412. Bibcode:2001GeCoA..65.4399A. doi:10.1016/S0016-7037(01)00720-7.
  79. ↑ Ishii, H; et al. (2008). "Comparison of Comet 81P/Wild 2 dust with interplanetary dust from comets". Science. 319 (5862): 447–50. Bibcode:2008Sci...319..447I. doi:10.1126/science.1150683. PMID 18218892. S2CID 24339399.
  80. ↑ Garenne, A; Beck, P; Montes-Hernandez, G; Brissaud, O (Jan 2016). "Bidirectional reflectance spectroscopy of carbonaceous chondrites: Implications for water quantification and primary composition". Icarus. 264: 172–183. Bibcode:2016Icar..264..172G. doi:10.1016/j.icarus.2015.09.005.
  81. ↑ Usui F, Hasegawa S, Ootsubo T, Onaka T (17 December 2018). "Akari/IRC near-infrared asteroid spectroscopic survey: AcuA spec". Publ. Astron. Soc. Jpn. 71 (1): 142. arXiv:1810.03828. Bibcode:2019PASJ...71....1U. doi:10.1093/pasj/psy125. S2CID 119479797.
  82. ↑ Abe M, Takagi Y, Kitazato K, Abe S, Hiroi T, Vilas F, Clark BE, Abell PA, Lederer SM, Jarvis KS, Nimura T, Ueda Y, Fujiwara A (June 2006). "Near-infrared spectral results of asteroid Itokawa from the Hayabusa spacecraft". Science. 312 (5778): 1334–8. Bibcode:2006Sci...312.1334A. doi:10.1126/science.1125718. PMID 16741108. S2CID 206508289.
  83. ↑ Matsuoka M, Nakamura T, Osawa T, Iwata T, Kitazato K, Abe M, et al. (4 Sep 2017). "An evaluation method of reflectance spectra to be obtained by Hayabusa2 Near-Infrared Spectrometer (NIRS3) based on laboratory measurements of carbonaceous chondrites". Earth, Planets and Space. 69 (1): 120. Bibcode:2017EP&S...69..120M. doi:10.1186/s40623-017-0705-4.
  84. ↑ Vilas F (1994). "A Cheaper, Faster, Better way to Detect Water of Hydration on Solar System Bodies". Icarus. 111 (2): 456–67. Bibcode:1994Icar..111..456V. doi:10.1006/icar.1994.1156.
  85. ↑ Fornasier S, Lantz C, Barucci M, Lazzarin M (2014). "Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy". Icarus. 233: 163. arXiv:1402.0175. Bibcode:2014Icar..233..163F. doi:10.1016/j.icarus.2014.01.040. S2CID 119234996.
  86. ↑ A'Hearn M, Feldman P (1992). "Water Vaporization on Ceres". Icarus. 98 (1): 54–60. Bibcode:1992Icar...98...54A. doi:10.1016/0019-1035(92)90206-M.
  87. ↑ Rivkin AS, Campins H, Emery J, Howell E (2015). "Astronomical Observations of Volatiles on Asteroids". In Michel P, DeMeo FE, Bottke WP (eds.). Asteroids IV. University of Arizona Press. pp. 65–88. ISBN 978-0-8165-3218-6.
  88. ↑ Rawlins K, Moses JI, Zahnle KJ (1995). "Exogenic sources of water for Mercury's polar ice". Bull. Am. Astron. Soc. 27: 1117–1118. Bibcode:1995DPS....27.2112R.
  89. ↑ Killen RM, Benkhoff J, Morgan TH (1997). "Mercury's polar caps and the generation of an OH exosphere". Icarus. 125 (1): 195–211. Bibcode:1997Icar..125..195K. doi:10.1006/icar.1996.5601.
  90. ↑ Moses JI, Rawlins K, Zahnle K, Dones L (1999). "External Sources of Water for Mercury's Putative Ice Deposits". Icarus. 137 (2): 197–221. Bibcode:1999Icar..137..197M. doi:10.1006/icar.1998.6036. S2CID 27144278.
  91. ↑ Albarede F, Ballhaus C, Blichert-Toft J, Lee CT, Marty B, Moynier F, Yin QZ (2013). "Asteroidal impacts and the origin of terrestrial and lunar volatiles". Icarus. 222 (1): 44. Bibcode:2013Icar..222...44A. doi:10.1016/j.icarus.2012.10.026.
  92. ↑ Saal AE, Hauri EH, Van Orman JA, Rutherford MJ (14 Jun 2013). "Hydrogen Isotopes in Lunar Volcanic Glasses and Melt Inclusions Reveal a Carbonaceous Chondrite Heritage". Science. 340 (6318): 1317–20. Bibcode:2013Sci...340.1317S. doi:10.1126/science.1235142. PMID 23661641. S2CID 9092975.
  93. ↑ Sarafian AR, Nielsen SG, Marschall HR, McCubbin FM, Monteleone BD (October 2014). "Early solar system. Early accretion of water in the inner solar system from a carbonaceous chondrite-like source". Science. 346 (6209): 623–6. Bibcode:2014Sci...346..623S. doi:10.1126/science.1256717. PMID 25359971. S2CID 30471982.
  94. ↑ Dauphas, N; Robert, F; Marty, B (Dec 2000). "The Late Asteroidal and Cometary Bombardment of Earth as Recorded in Water Deuterium to Protium Ratio". Icarus. 148 (2): 508–512. Bibcode:2000Icar..148..508D. doi:10.1006/icar.2000.6489. S2CID 85555707.
  95. ↑ Ong, L; Asphaug, E; Korycansky, D; Coker, R (Jun 2010). "Volatile retention from cometary impacts on the Moon". Icarus. 207 (2): 578–589. Bibcode:2010Icar..207..578O. doi:10.1016/j.icarus.2009.12.012.
  96. ↑ Svetsov VV, Shuvalov VV (Sep 2015). "Water Delivery to the Moon by Asteroidal and Cometary Impacts". Planetary and Space Science. 117: 444–452. Bibcode:2015P&SS..117..444S. doi:10.1016/j.pss.2015.09.011.
  97. ↑ Zolensky M, Weisberg M, Buchanan P, Mittelfehldt D (1996). "Mineralogy of carbonaceous chondrite clasts in HED achondrites and the moon". Meteoritics & Planetary Science. 31 (4): 518–537. Bibcode:1996M&PS...31..518Z. doi:10.1111/j.1945-5100.1996.tb02093.x.
  98. ↑ Elsila, J; Callahan, M; Dworkin, J; Glavin, D; McLain, H; Noble, S; Gibson, E (2016). "The origin of amino acids in lunar regolith samples". Geochimica et Cosmochimica Acta. 172: 357–69. Bibcode:2016GeCoA.172..357E. doi:10.1016/j.gca.2015.10.008.
  99. 1 2 Jewitt D, Guilbert-Lepoutre A (Jan 2012). "Limits to Ice on Asteroids (24) Themis and (65) Cybele". Astronomical Journal. 143 (1): 21. arXiv:1111.3292. Bibcode:2012AJ....143...21J. doi:10.1088/0004-6256/143/1/21. S2CID 12423969.
  100. ↑ McKay AJ, Bodewits D, Li JY (Sep 2016). "Observational Constraints on Water Sublimation from 24 Themis and 1 Ceres". Icarus. 286: 308–313. arXiv:1609.07156. Bibcode:2017Icar..286..308M. doi:10.1016/j.icarus.2016.09.032. S2CID 119121785.
  101. ↑ Castillo-Rogez JC, Schmidt BE (May 2010). "Geophysical evolution of the Themis family parent body". Geophysical Research Letters. 37 (10): n/a. Bibcode:2010GeoRL..3710202C. doi:10.1029/2009GL042353.
  102. ↑ Florczak M, Lazzaro D, Mothé-Diniz T, Angeli CA, Betzler AS (1999). "A spectroscopic study of the Themis family". Astronomy and Astrophysics Supplement. 134 (3): 463. Bibcode:1999A&AS..134..463F. doi:10.1051/aas:1999150.
  103. ↑ Marsset M, Vernazza P, Birlan M, DeMeo F, Binzel RP, Dumas C, Milli J, Popescu M (2016). "Compositional characteristics of the Themis family". Astronomy & Astrophysics. 586: A15. arXiv:1601.02405. Bibcode:2016A&A...586A..15M. doi:10.1051/0004-6361/201526962. S2CID 55479080.
  104. ↑ Hsieh HH, Novaković B, Kim Y, Brasser R (2018). "Asteroid Family Associations of Active Asteroids". Astronomical Journal. 155 (2): 96. arXiv:1801.01152. Bibcode:2018AJ....155...96H. doi:10.3847/1538-3881/aaa5a2. S2CID 119336304.
  105. ↑ Haghighipour N (2009). "Dynamical constraints on the origin of Main Belt Comets". Meteoritics & Planetary Science. 44 (12): 1863–1869. arXiv:0910.5746. Bibcode:2009M&PS...44.1863H. doi:10.1111/j.1945-5100.2009.tb01995.x. S2CID 56206203.
  106. ↑ Licandro J, Campins H, Kelley M, Hargrove K, Pinilla-Alonso N, Cruikshank D, et al. (2011). "(65) Cybele: detection of small silicate grains, water-ice, and organics". Astronomy & Astrophysics. 525: A34. Bibcode:2011A&A...525A..34L. doi:10.1051/0004-6361/201015339.
  107. ↑ Reddy (2018). "A". LPSC.
  108. ↑ Scully JE, Russell CT, Yin A, Jaumann R, Carey E, Castillo-Rogez J, et al. (Feb 2015). "Geomorphological Evidence for Transient Water Flow on Vesta". Earth and Planetary Science Letters. 411: 151. Bibcode:2015E&PSL.411..151S. doi:10.1016/j.epsl.2014.12.004.
  109. ↑ De Sanctis, M; Ammannito, E; et al. (10 Dec 2015). "Ammoniated phyllosilicates with a likely outer Solar System origin on (1) Ceres" (PDF). Nature. 528 (7581): 241–4. Bibcode:2015Natur.528..241D. doi:10.1038/nature16172. PMID 26659184. S2CID 1687271.
  110. ↑ Takir D, Reddy V, Sanchez JA, Shepard MK, Emery JP (Oct 2016). "Detection of water and/or hydroxyl on Asteroid (16) Psyche". Astronomical Journal. 153 (1): 31. arXiv:1610.00802. Bibcode:2017AJ....153...31T. doi:10.3847/1538-3881/153/1/31. S2CID 118611420.
  111. ↑ Jin ZL, Bose M, Peeters Z (2019). "New Clues to Ancient Water on Itokawa". Lunar and Planetary Science Conference. 5 (2083): 1670. Bibcode:2018LPI....49.1670J. doi:10.1126/sciadv.aav8106. PMC 6527261. PMID 31114801.
  112. ↑ Kawaguchi JI, Uesugi KT, Fujiwara A, Saitoh H (1999). "The MUSES-C, Mission Description and its Status". Acta Astronautica. 45 (4): 397. Bibcode:1999AcAau..45..397K. doi:10.1016/S0094-5765(99)00159-9.
  113. ↑ Yada T, Fujimura A, Abe M, Nakamura T, Noguchi T, Okazaki R, et al. (February 2014). "Hayabusa‐returned sample curation in the Planetary Material Sample Curation Facility of JAXA". Meteoritics & Planetary Science. 49 (2): 135–53. Bibcode:2014M&PS...49..135Y. doi:10.1111/maps.12027.
  114. ↑ Maltagliati L (Oct 2018). "Cometary Bennu?". Nature Astronomy. 2 (10): 761. Bibcode:2018NatAs...2..761M. doi:10.1038/s41550-018-0599-5. S2CID 189930305.
  115. ↑ "Feb 11, 2019 [Mission Status]". OSIRIS-REx: Asteroid Sample Return Mission. Retrieved 24 Mar 2019.
  116. ↑ Witze, A (2019). "Asteroid's bumpiness threatens US plan to return a sample to Earth". Nature. Springer Nature Publishing AG. doi:10.1038/d41586-019-00859-7. PMID 32203348. S2CID 134983567. Retrieved 24 Mar 2019.
  117. ↑ Hamilton, V Simon A Christensen P Reuter D Clark B Barucci M Bowles N Boynton W Brucato J Cloutis E Connolly H Donaldson Hanna K Emery J Enos H Fornasier S Haberle C Hanna R Howell E; Kaplan H Keller L (Mar 2019). "Evidence for widespread hydrated minerals on asteroid (101955) Bennu" (PDF). Nature Astronomy. 3 (332–340): 332–340. Bibcode:2019NatAs...3..332H. doi:10.1038/s41550-019-0722-2. hdl:1721.1/124501. PMC 6662227. PMID 31360777.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  118. ↑ Sears, D (2004). The Origin of Chondrules and Chondrites. Cambridge University Press. ISBN 978-1107402850.
  119. ↑ "OSIRIS-REx at AGU 2018". asteroidmission.org. 10 December 2018. Retrieved 13 December 2018.
  120. ↑ Busarev VV, Makalkin AB, Vilas F, Barabanov SI, Scherbina MP (2017). "New Candidates for Active Asteroids: (145) Adeona, (704) Interamnia, (779) Nina, (1474) Beira, and Near-Earth (162173) Ryugu". Icarus. 304: 83–94. arXiv:1705.09086. Bibcode:2018Icar..304...83B. doi:10.1016/j.icarus.2017.06.032. S2CID 119344402.
  121. ↑ anon (Mar 20, 2019). "Japan's Hayabusa2 probe finds water on Ryugu asteroid". Kyodo News. Retrieved 17 Nov 2019.
  122. ↑ Kitazao, K; Milliken, R; Iwata, T; Abe, M; Ohtake, M; Matsuura, S; Arai, T; Nakauchi, Y; Nakamura, T (19 Mar 2019). "The surface composition of asteroid 162173 Ryugu from Hayabusa2 near-infrared spectroscopy". Science. 364 (6437): 272–75. Bibcode:2019Sci...364..272K. doi:10.1126/science.aav7432. PMID 30890589.
  123. ↑ Feierberg MA, Lebofsky LA, Tholen DJ (1985). "The Nature of C-Class Asteroids from 3-um Spectrophotometry". Icarus. 63 (2): 183–91. Bibcode:1985Icar...63..183F. doi:10.1016/0019-1035(85)90002-8.
  124. ↑ Grimm R, McSween H (1989). "Water and the thermal evolution of carbonaceous parent bodies". Icarus. 82 (2): 244. Bibcode:1989Icar...82..244G. doi:10.1016/0019-1035(89)90038-9.
  125. ↑ Novaković B, Hsieh HH, Cellino A, Micheli M, Pedani M (2014). "Discovery of a young asteroid cluster associated with P/2012 F5 (Gibbs)". Icarus. 231: 300–09. arXiv:1401.2966. Bibcode:2014Icar..231..300N. doi:10.1016/j.icarus.2013.12.019. S2CID 119216225.
  126. ↑ Busarev VV, Makalkin AB, Vilas F, Barabanov SI, Scherbina MP (2018). "Asteroid clusters similar to asteroid pairs". Icarus. 304: 110–26. Bibcode:2018Icar..304..110P. doi:10.1016/j.icarus.2017.08.008.
  127. ↑ "地球―月ラグランジュ点探査機EQUULEUSによる深宇宙探査CubeSat実現への挑戦". 宇宙科学最前線. JAXA. Retrieved 2 Apr 2019.
  128. ↑ "Propulsion". University of Surrey. Retrieved 17 Feb 2019.
  129. ↑ "DSI to provide Comet satellite propulsion for Astro Digital". Deep Space Industries. Archived from the original on 17 March 2018. Retrieved 17 Feb 2018.
  130. ↑ Matloff GL, Wilga M (2011). "NEOs as stepping stones to Mars and main-belt asteroids". Acta Astronautica. 68 (5–6): 599. Bibcode:2011AcAau..68..599M. doi:10.1016/j.actaastro.2010.02.026.
  131. ↑ Pohl, L (Mar 2017). "The radiation shielding potential of CI and CM chondrites". Advances in Space Research. 59 (6): 1473–1485. Bibcode:2017AdSpR..59.1473P. doi:10.1016/j.asr.2016.12.028.
  132. ↑ Green, Marc; Hess, Justin (13 June 2013). "Near Earth Asteroids: The Celestial Chariots". arXiv:1306.3118.
  133. ↑ Mautner M (2002). "Planetary Bioresources and Astroecology 1. Planetary Microcosm Bioassays of Martian and Carbonaceous Chondrite Materials: Nutrients, Electrolyte Solutions, and Algal and Plant Responses". Icarus. 158 (1): 72. Bibcode:2002Icar..158...72M. doi:10.1006/icar.2002.6841.
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