Organic matter and water from asteroid Itokawa

Abstract Understanding the true nature of extra-terrestrial water and organic matter that was present at the birth of our solar system, and their subsequent evolution, necessitates the study of pristine astromaterials. In this study, we have studied both the water and organic contents from a dust particle recovered from the surface of near-Earth asteroid 25143 Itokawa by the Hayabusa mission, which represents one of the most uncontaminated astromaterial samples in Earth’s collection. The organic matter is presented as both nanocrystalline graphite and disordered polyaromatic carbon with high D/H and 15N/14N ratios (δD = +4,868 ± 2,288‰; δ15N = +344 ± 20‰) signifying an explicit extra-terrestrial origin. The contrasting organic feature (graphitic and disordered) substantiates the rubble-pile asteroid model of Itokawa, and offers support for material mixing in the asteroid belt that occurred in scales from small dust infall to cartographic impacts of large asteroidal parent bodies. Our analysis of Itokawa water indicates that the asteroid has incorporated D-poor water ice at the abundance on par with inner solar system bodies. The asteroid was metamorphosed and dehydrated on the formerly large asteroid, and was subsequently evolved via late-stage hydration, modified by D-enriched extraneous organics and water derived from a carbonaceous parent body.

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Aqueous alteration without initial water: Possibility of organic-induced hydration of anhydrous silicates in meteorite parent bodies

10.21203/rs.3.rs-50113/v3 ◽

2021 ◽

Author(s):

Naoki Hirakawa ◽

Yoko Kebukawa ◽

Yoshihiro Furukawa ◽

Masashi Kondo ◽

Hideyuki Nakano ◽

...

Keyword(s):

Organic Matter ◽

Solar System ◽

Organic Compounds ◽

Parent Body ◽

Ordinary Chondrites ◽

Aqueous Alteration ◽

Initial Water ◽

Water Ice ◽

Silicate Formation ◽

Snow Line

Abstract Early evolution of Solar System small bodies proceeded through interactions of mineral and water. Melting of water ice accreted with mineral particles to the parent body results in the formation of secondary minerals, the so-called aqueous alteration. Formation of phyllosilicates from anhydrous silicates is a typical alteration effect recorded in primitive meteorites. In addition to mineral and water, organic matter could have been also a significant component in meteorite parent bodies. However, the role of organic matter in the alteration of silicates is not well understood. We conducted a heating experiment of anhydrous silicate (olivine) with a mixture of organic compounds which simulated primordial organic matter in the Solar System. Dissolution and precipitation features were confirmed on the olivine surface after heating at 300 °C for 10 days, and proto-phyllosilicates were formed in the precipitation area. Magnesite was also detected as concomitant mineral phase. These minerals could be the evidence of aqueous alteration and carbonation of olivine induced by water generated through decomposition of the organic compounds with hydroxy groups. Our result showed that the in-situ formation of hydrated silicates through a mineral-organic interaction without the initial presence of water. It further implies that formation of phyllosilicates on the olivine surface in contact with organic matter can occur in meteorite parent bodies which formed inside the H2O snow line but accreted with organic matter, initially without water. Water formed through decomposition of organic matter could be one candidate for hydrous silicate formation, for example in ordinary chondrites from S-type asteroids inside the H2O snow line. Although the origin of water in ordinary chondrites is under debate, water generation from organic matter may also explain the D-rich water in ordinary chondrites because primordial organic matter is known to be D-rich.

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Aqueous alteration without initial water: Possibility of organic-induced hydration of anhydrous silicates in meteorite parent bodies

10.21203/rs.3.rs-50113/v2 ◽

2020 ◽

Author(s):

Naoki Hirakawa ◽

Yoko Kebukawa ◽

Yoshihiro Furukawa ◽

Masashi Kondo ◽

Hideyuki Nakano ◽

...

Keyword(s):

Organic Matter ◽

Solar System ◽

Organic Compounds ◽

Parent Body ◽

Ordinary Chondrites ◽

Aqueous Alteration ◽

Initial Water ◽

Water Ice ◽

Silicate Formation ◽

Snow Line

Abstract Early evolution of Solar System small bodies proceeded through interactions of mineral and water. Melting of water ice accreted with mineral particles to the parent body results in the formation of secondary minerals, the so-called aqueous alteration. Formation of phyllosilicates from anhydrous silicates is a typical alteration effect recorded in primitive meteorites. In addition to mineral and water, organic matter could have been also a significant component in meteorite parent bodies. However, the role of organic matter in the alteration of silicates is not well understood. We conducted a heating experiment of anhydrous silicate (olivine) with a mixture of organic compounds which simulated primordial organic matter in the Solar System. Dissolution and precipitation features were confirmed on the olivine surface after heating at 300 °C for 10 days, and proto-phyllosilicates were formed in the precipitation area. Magnesite was also detected as concomitant mineral phase. These minerals could be the evidence of aqueous alteration and carbonation of olivine induced by water generated through decomposition of the organic compounds with hydroxy groups. Our result showed that the in-situ formation of hydrated silicates through a mineral-organic interaction without the initial presence of water. It further implies that formation of phyllosilicates on the olivine surface in contact with organic matter can occur in meteorite parent bodies which formed inside the H2O snow line but accreted with organic matter, initially without water. Water formed through decomposition of organic matter could be one candidate for hydrous silicate formation, for example in ordinary chondrites from S-type asteroids inside the H2O snow line. Although the origin of water in ordinary chondrites is under debate, water generation from organic matter may also explain the D-rich water in ordinary chondrites because primordial organic matter is known to be D-rich.

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The Grand Tack model: a critical review

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314008254 ◽

2014 ◽

Vol 9 (S310) ◽

pp. 194-203 ◽

Cited By ~ 12

Author(s):

Sean N. Raymond ◽

Alessandro Morbidelli

Keyword(s):

Solar System ◽

Building Blocks ◽

Protoplanetary Disk ◽

Giant Planets ◽

Asteroid Belt ◽

Terrestrial Planets ◽

Saturn’S Satellites ◽

Internal Inconsistency ◽

Solar System Bodies ◽

Gas Accretion

AbstractThe “Grand Tack” model proposes that the inner Solar System was sculpted by the giant planets' orbital migration in the gaseous protoplanetary disk. Jupiter first migrated inward then Jupiter and Saturn migrated back outward together. If Jupiter's turnaround or “tack” point was at ~ 1.5 AU the inner disk of terrestrial building blocks would have been truncated at ~ 1 AU, naturally producing the terrestrial planets' masses and spacing. During the gas giants' migration the asteroid belt is severely depleted but repopulated by distinct planetesimal reservoirs that can be associated with the present-day S and C types. The giant planets' orbits are consistent with the later evolution of the outer Solar System.Here we confront common criticisms of the Grand Tack model. We show that some uncertainties remain regarding the Tack mechanism itself; the most critical unknown is the timing and rate of gas accretion onto Saturn and Jupiter. Current isotopic and compositional measurements of Solar System bodies – including the D/H ratios of Saturn's satellites – do not refute the model. We discuss how alternate models for the formation of the terrestrial planets each suffer from an internal inconsistency and/or place a strong and very specific requirement on the properties of the protoplanetary disk.We conclude that the Grand Tack model remains viable and consistent with our current understanding of planet formation. Nonetheless, we encourage additional tests of the Grand Tack as well as the construction of alternate models.

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No evidence for interstellar planetesimals trapped in the Solar system

Monthly Notices of the Royal Astronomical Society Letters ◽

10.1093/mnrasl/slaa111 ◽

2020 ◽

Vol 497 (1) ◽

pp. L46-L49 ◽

Cited By ~ 2

Author(s):

A Morbidelli ◽

K Batygin ◽

R Brasser ◽

S N Raymond

Keyword(s):

Solar System ◽

Oort Cloud ◽

Giant Planets ◽

Asteroid Belt ◽

Interstellar Space ◽

Fast Decay ◽

Early Solar System ◽

The Past ◽

Solar System Bodies ◽

Main Asteroid Belt

ABSTRACT In two recent papers published in MNRAS, Namouni and Morais claimed evidence for the interstellar origin of some small Solar system bodies, including: (i) objects in retrograde co-orbital motion with the giant planets and (ii) the highly inclined Centaurs. Here, we discuss the flaws of those papers that invalidate the authors’ conclusions. Numerical simulations backwards in time are not representative of the past evolution of real bodies. Instead, these simulations are only useful as a means to quantify the short dynamical lifetime of the considered bodies and the fast decay of their population. In light of this fast decay, if the observed bodies were the survivors of populations of objects captured from interstellar space in the early Solar system, these populations should have been implausibly large (e.g. about 10 times the current main asteroid belt population for the retrograde co-orbital of Jupiter). More likely, the observed objects are just transient members of a population that is maintained in quasi-steady state by a continuous flux of objects from some parent reservoir in the distant Solar system. We identify in the Halley-type comets and the Oort cloud the most likely sources of retrograde co-orbitals and highly inclined Centaurs.

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The Distribution of Asteroidal Dust in the Inner Solar System

Symposium - International Astronomical Union ◽

10.1017/s0074180900217798 ◽

2004 ◽

Vol 202 ◽

pp. 184-186

Author(s):

Keith Grogan ◽

S.F. Dermott ◽

T.J.J. Kehoe

Keyword(s):

Solar System ◽

Parent Body ◽

Asteroid Belt ◽

Dust Particles ◽

Secular Resonances ◽

Level Of Confidence ◽

Asteroidal Dust

In this paper we demonstrate how the action of secular resonances near the inner edge of the asteroid belt strongly effects the inclinations and eccentricities of asteroidal dust particles, such that they lose the orbital characteristics of their parent body and are dispersed into the zodiacal background. As a consequence, it may not be possible to relate the distribution of interplanetary material at 1 AU to given asteroidal or cometary sources with the level of confidence previously imagined.

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Photolysis and radiolysis of water ice on outer solar system bodies

Journal of Geophysical Research Atmospheres ◽

10.1029/97je00068 ◽

1997 ◽

Vol 102 (E5) ◽

pp. 10985-10996 ◽

Cited By ~ 135

Author(s):

R. E. Johnson ◽

T. I. Quickenden

Keyword(s):

Solar System ◽

Outer Solar System ◽

Water Ice ◽

Solar System Bodies

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The Locations of Secular Resonances and the Evolution of Small Solar System Bodies

Symposium - International Astronomical Union ◽

10.1017/s0074180900091026 ◽

1992 ◽

Vol 152 ◽

pp. 123-132

Author(s):

Ch Froeschle ◽

P. Farinella ◽

C. Froeschle ◽

Z. Knežević ◽

A. Milani

Keyword(s):

Perturbation Theory ◽

Solar System ◽

Small Body ◽

Kuiper Belt ◽

Dynamical Evolution ◽

Asteroid Belt ◽

Secular Resonances ◽

Outer Planets ◽

Proper Elements ◽

Solar System Bodies

Generalizing the secular perturbation theory of Milani and Knežević (1990), we have determined in the a — e — I proper elements space the locations of the secular resonances between the precession rates of the longitudes of perihelion and node of a small body and the corresponding eigenfrequencies of the secular perturbations of the four outer planets. We discuss some implications of the results for the dynamical evolution of small solar system bodies. In particular, our findings include: (i) the fact that the g = g6 resonance in the inner asteroid belt lies closer than previously assumed to the Flora region, providing a plausible dynamical route to inject asteroid fragments into planet-crossing orbits; (ii) the possible presence of some low-inclination “stable islands” between the orbits of the outer planets; (iii) the fact that none of the secular resonances considered in this work exists for semimajor axes > 50 AU, so that these resonances do not provide a mechanism for transporting inwards possible Kuiper–belt comets.

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Arrival and magnetization of carbonaceous chondrites in the asteroid belt before 4562 million years ago

Communications Earth & Environment ◽

10.1038/s43247-020-00055-w ◽

2020 ◽

Vol 1 (1) ◽

Author(s):

Timothy O’Brien ◽

John A. Tarduno ◽

Atma Anand ◽

Aleksey V. Smirnov ◽

Eric G. Blackman ◽

...

Keyword(s):

Solar System ◽

Arrival Time ◽

Carbonaceous Chondrite ◽

Parent Body ◽

Asteroid Belt ◽

Carbonaceous Chondrites ◽

Early Solar System ◽

Outer Disk ◽

Main Asteroid Belt ◽

Insight Into

AbstractMeteorite magnetizations can provide rare insight into early Solar System evolution. Such data take on new importance with recognition of the isotopic dichotomy between non-carbonaceous and carbonaceous meteorites, representing distinct inner and outer disk reservoirs, and the likelihood that parent body asteroids were once separated by Jupiter and subsequently mixed. The arrival time of these parent bodies into the main asteroid belt, however, has heretofore been unknown. Herein, we show that weak CV (Vigarano type) and CM (Mighei type) carbonaceous chondrite remanent magnetizations indicate acquisition by the solar wind 4.2 to 4.8 million years after Ca-Al-rich inclusion (CAI) formation at heliocentric distances of ~2–4 AU. These data thus indicate that the CV and CM parent asteroids had arrived near, or within, the orbital range of the present-day asteroid belt from the outer disk isotopic reservoir within the first 5 million years of Solar System history.

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