Insight into the silicate and organic reservoirs of the comet forming region

Starkey, N. A.; Franchi, I. A.

doi:10.1016/j.gca.2012.11.040

Cited by 34 publications

(151 citation statements)

References 75 publications

Supporting

Mentioning

133

Contrasting

Order By: Relevance

“…The H 2 O may have had a mass-independent anomaly as high as 17 O ≈ 80‰ [105]. By some still poorly understood process, fractionation of silicates and H 2 O ice from CO in the gas, followed by isotopic exchange between the silicates and H 2 O, would explain why all inner Solar System materials, as well as IDPs and comet Wild 2 dust, have O isotopic compositions that fall fairly close to the TFL [106][107][108][109]. Much of this exchange has to have occurred prior to accretion of the chondrite and comet parent bodies because most of their components, other than refractory inclusions, have O isotopic compositions that lie closer to the TFL than to the solar composition.…”

Section: Hydrogen Isotopes: Indicators Of Formation Distance?mentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Of the potential volatile sources for the terrestrial planets, the CI and CM carbonaceous chondrites are closest to the planets' bulk H and N isotopic compositions. For the Earth, the addition of approximately 2–4 wt% of CI/CM material to a volatile-depleted proto-Earth can explain the abundances of many of the most volatile elements, although some solar-like material is also required. Two dynamical models of terrestrial planet formation predict that the carbonaceous chondrites formed either in the asteroid belt (‘classical’ model) or in the outer Solar System (5–15 AU in the Grand Tack model). To test these models, at present the H isotopes of water are the most promising indicators of formation location because they should have become increasingly D-rich with distance from the Sun. The estimated initial H isotopic compositions of water accreted by the CI, CM, CR and Tagish Lake carbonaceous chondrites were much more D-poor than measured outer Solar System objects. A similar pattern is seen for N isotopes. The D-poor compositions reflect incomplete re-equilibration with H 2 in the inner Solar System, which is also consistent with the O isotopes of chondritic water. On balance, it seems that the carbonaceous chondrites and their water did not form very far out in the disc, almost certainly not beyond the orbit of Saturn when its moons formed (approx. 3–7 AU in the Grand Tack model) and possibly close to where they are found today. This article is part of the themed issue ‘The origin, history and role of water in the evolution of the inner Solar System’.

show abstract

Section: Hydrogen Isotopes: Indicators Of Formation Distance?mentioning

confidence: 99%

The origin of inner Solar System water

Alexander¹

2017

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

show abstract

“…The O isotopic composition of carbonaceous chondrites is related to that of chondritic porous IDPs, Stardust grains and UCAMMs (Sect. 3.3), and suggests a genetic continuum between carbonaceous chondrites and comets (Aléon 2010;Nakashima et al 2012;Davidson et al 2012;Starkey and Franchi 2013, and references therein).…”

Section: Interplanetary Dust Particlesmentioning

confidence: 88%

Cometary Isotopic Measurements

et al. 2015

View full text Add to dashboard Cite

“…Computational chemistry studies about complex organic molecules that forms the bases of life have led to the theory that such molecules might have been formed in the protoplanetary disc, in the nanoparticles that revolved around the Sun, before the formation of the Earth [43]. According to computer models, the process could be the same around any star that acquires planets through a mechanism similar to their formation around the Sun [44].…”

Section: Cosmic Dustmentioning

confidence: 99%

Natural Sources of Nanoparticles

Strambeanu¹,

Demetrovici²,

Dragoş

2014

Nanoparticles' Promises and Risks

View full text Add to dashboard Cite

This chapter deals with the major natural sources of nanoparticles in the atmosphere: volcanic eruptions, desert surfaces, dust from cosmic sources located in the solar system or outside it. Details are given about the composition of very fine particles according to their type, the successive or parallel chemical transformations that can occur among them or when they meet the major components of the atmosphere (nitrogen, oxygen, carbon dioxide). The authors specify possible ways of evolution from the mineral kingdom to organic substances through nanoparticles originating from cosmic dust, based on suppositions that are provided in the literature of the field and accepted based on physical and chemical computational models.

show abstract

Insight into the silicate and organic reservoirs of the comet forming region

Cited by 34 publications

References 75 publications

The origin of inner Solar System water

The origin of inner Solar System water

Cometary Isotopic Measurements

Natural Sources of Nanoparticles

Contact Info

Product

Resources

About