Constraints on the Formation Regions of Comets from their D:H Ratios

Horner, Jonathan; Mousis, O.; Hersant, F.

doi:10.1007/s11038-006-9096-4

Cited by 42 publications

(44 citation statements)

References 36 publications

(11 reference statements)

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“…Balsiger et al (1995) and Eberhardt et al (1995) Simulations of the D/H gradient using upper limits for the ice D/H from the analysis of meteorite samples, managed to verify these observations (e.g. Drouart et al 1999;Mousis et al 2000;Horner et al 2007 andKavelaars et al 2011). Therefore, models appear to be compatible with the assumption that OCCs formed in the vicinity of the gas giants.…”

Section: Water and D/hmentioning

confidence: 74%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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Section: Water and D/hmentioning

confidence: 74%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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“…These simulations suggest that, irrespective of the employed solar nebula model, photophoresis is a mechanism that can explain the presence of hot-temperature minerals at early epochs of the disk's evolution in the formation region of comets (from 10 to 30 AU according to the different scenarios -see, e.g., Horner et al 2007, for a review). Because comets have presumably accreted within a few hundred thousand years (Weidenschilling 1997), i.e., a timescale shorter than the one probably required to form an inner gap in the disk and to allow the photophoretic transport of particles formed close to the Sun, they probably had the time to essentially trap the dust transported from the inner solar system in the form of shell surrounding their surface if their accretion ended before A106, page 8 of 11 particles reached their formation location.…”

Section: Disk's Structure and Evolutionmentioning

confidence: 99%

Photophoretic transport of hot minerals in the solar nebula

Moudens¹,

Mousis²,

Petit³

et al. 2011

A&A

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Context. Hot temperature minerals have been detected in a large number of comets and were also identified in the samples of Comet Wild 2 that were returned by the Stardust mission. Meanwhile, observations of the distribution of hot minerals in young stellar systems suggest that these materials were produced in the inner part of the primordial nebula and have been transported outward in the formation zone of comets. Aims. We investigate the possibility that photophoresis provides a viable mechanism to transport high-temperature materials from the inner solar system to the regions in which the comets were forming. Methods. We use a grid of time-dependent disk models of the solar nebula to quantify the distance range at which hot minerals can be transported from the inner part of the disk toward its outer regions as a function of their size (10 −5 to 10 −1 m) and density (500 and 1000 kg m −3 ). These models will also yield information on the disk properties (radius of the inner gap, initial mass, and lifetime of the disk). The particles considered here are in the form of aggregates that presumably were assembled from hot mineral individual grains ranging down to submicron sizes and formed by condensation within the hottest portion of the solar nebula. Our particle-transport model includes the photophoresis, radiation pressure, and gas drag. Results. Depending on the postulated disk parameters and the density of particles, 10 −2 to 10 −1 m aggregates can reach heliocentric distances up to ∼35 AU in the primordial nebula over very short timescales (no more than a few hundred thousand years). 10 −3 m particles follow the same trajectory as the larger ones but their maximum migration distance does not exceed ∼26 AU and is reached at later epochs in the disks. On the other hand, 10 −5 to 10 −4 m aggregates are continuously pushed outward during the evolution of the solar nebula. Depending on the adopted disk parameters, these particles can reach the outer edge of the nebula well before its dissipation. Conclusions. Our simulations suggest that irrespective of the employed solar nebula model, photophoresis is a mechanism that can explain the presence of hot temperature minerals in the formation region of comets. Comets probably had the time to trap the dust transported from the inner solar system either in their interior during accretion or in the form of shells surrounding their surface if they ended their growth before the particles reached their formation location.

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“…The red line shows Kuiper-belt objects, and the black Oort-cloud objects. From [66]. Table 1.7: Nitrogen and carbon isotopic ratios in comets from observations of the CN radical.…”

Section: Isotopic Ratiosmentioning

confidence: 99%

High-resolution infrared spectroscopic measurements of Comet 2P/Encke: Unusual organic composition and low rotational temperatures

Radeva

Mumma

Villanueva

et al. 2013

Icarus

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Comets are classified from their orbital characteristics into two separate classes:nearly-isotropic, mainly long-period comets and ecliptic, short-period comets. Members from the former class are coming from the Oort cloud. Those of the latter class were first believed to have migrated from the Kuiper belt where they could have been accreted in situ, but recent orbital evolution simulations showed that they rather come from the trans-Neptunian scattered disc. These two reservoirs are not where the comets formed: they were expelled from the inner Solar System following interaction with the giant planets. If comets formed at different places in the Solar System, one would expect they show different chemical and physical properties. In the present paper, I review which differences are effectively observed: chemical and isotopic compositions, spin temperatures, dust particle properties, nucleus properties... and investigate whether these differences are correlated with the different dynamical classes. The difficulty of such a study is that long-period, nearly-isotropic comets from the Oort cloud are better known, from Earth-based observations, than the weak nearly-isotropic, short-period comets. On the other hand, only the latter are easily accessed by space missions.

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Constraints on the Formation Regions of Comets from their D:H Ratios

Cited by 42 publications

References 36 publications

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

Photophoretic transport of hot minerals in the solar nebula

High-resolution infrared spectroscopic measurements of Comet 2P/Encke: Unusual organic composition and low rotational temperatures

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