Distribution and Evolution of Water Ice in the Solar Nebula: Implications for Solar System Body Formation

Cyr, K. E.; Sears, W. D.; Lunine, Jonathan I.

doi:10.1006/icar.1998.5959

Cited by 117 publications

(119 citation statements)

References 27 publications

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“…They also calculated the simultaneous evolution of the viscous protoplanetary disk, accounting for the changes in surface density and temperature. They reached similar conclusions to Stevenson and Lunine (1988) and Cyr et al (1998) in that a large pile-up of ice would occur just outside of the snow line. If massive, compact (extending to ∼20 AU) disks were investigated, the solids rapidly migrated to the inner region of the disk before planetesimals could form and were lost.…”

Section: Previous Models Of Water Transport In the Solar Nebulasupporting

confidence: 62%

“…Cuzzi and Zahnle (2004) argued that until planetesimals grow outside the snow line, bodies from the outer nebula will continuously migrate into the inner nebula and vaporize, enriching the gas with water and suggest that this could explain the presence of oxidized species in primitive meteorites. Once the immobile planetesimals form, they act as a sink by accreting material rather than allowing it to drift inwards, and the inner nebula begins to dehydrate as was found by Stevenson and Lunine (1988) and Cyr et al (1998).…”

Section: Previous Models Of Water Transport In the Solar Nebulamentioning

confidence: 86%

“…Morfill and Völk (1984) on the other hand, did not assume material was trapped on immobile planetesimals, so their solutions did not show these substantial effects. Cyr et al (1998) extended this model to examine the diffusion of water vapor along with the migration of the freshly formed ice particles into the inner nebula via gas drag. As the ice particles drifted inwards, they vaporized at a finite rate (Lichtenegger and Komle, 1991) and could drift significant distances inwards before completely vaporizing.…”

Section: Previous Models Of Water Transport In the Solar Nebulamentioning

confidence: 99%

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The evolution of the water distribution in a viscous protoplanetary disk

Ciesla

Cuzzi

2006

Icarus

322

356

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Astronomical observations have shown that protoplanetary disks are dynamic objects through which mass is transported and accreted by the central star. This transport causes the disks to decrease in mass and cool over time, and such evolution is expected to have occurred in our own solar nebula. Age dating of meteorite constituents shows that their creation, evolution, and accumulation occupied several Myr, and over this time disk properties would evolve significantly. Moreover, on this timescale, solid particles decouple from the gas in the disk and their evolution follows a different path. It is in this context that we must understand how our own solar nebula evolved and what effects this evolution had on the primitive materials contained within it. Here we present a model which tracks how the distribution of water changes in an evolving disk as the water-bearing species experience condensation, accretion, transport, collisional destruction, and vaporization. Because solids are transported in a disk at different rates depending on their sizes, the motions will lead to water being concentrated in some regions of a disk and depleted in others. These enhancements and depletions are consistent with the conditions needed to explain some aspects of the chemistry of chondritic meteorites and formation of giant planets. The levels of concentration and depletion, as well as their locations, depend strongly on the combined effects of the gaseous disk evolution, the formation of rapidly migrating rubble, and the growth of immobile planetesimals. Understanding how these processes operate simultaneously is critical to developing our models for meteorite parent body formation in the solar system and giant planet formation throughout the galaxy. We present examples of evolution under a range of plausible assumptions and demonstrate how the chemical evolution of the inner region of a protoplanetary disk is intimately connected to the physical processes which occur in the outer regions.

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Section: Previous Models Of Water Transport In the Solar Nebulasupporting

confidence: 62%

Section: Previous Models Of Water Transport In the Solar Nebulamentioning

confidence: 86%

Section: Previous Models Of Water Transport In the Solar Nebulamentioning

confidence: 99%

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The evolution of the water distribution in a viscous protoplanetary disk

Ciesla

Cuzzi

2006

Icarus

322

356

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“…1d). We suggest that the inferred low abundance of water ices in ordinary, CO and CV chondrite parent bodies resulted from their accretion close to the snow line, possibly slightly inside it, where only the relatively large ice-bearing particles could have avoided instantaneous evaporation and survived to be accreted to the parent body 43 . The location of the snow line in the protoplanetary disk is uncertain; it likely did not reside at a single location, but rather migrated with time as the luminosity of the proto-Sun, the mass transport rate through the disk, and the disk opacity all evolved with time.…”

Section: Discussionmentioning

confidence: 93%

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

et al. 2015

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Chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric 53 Cr dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first 53 Mn-53 Cr ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2:4 þ 1:8 À 1:3 Myr after calcium-aluminium-rich inclusions (CAIs), the oldest Solar System solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed 4:2 þ 0:8 À 0:7 and 5:1 þ 0:5 À 0:4 Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and 53 Cr ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies B1.8 À 2.5 Myr after CAIs.

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“…Most solar nebula models suggested that the growth zones of the terrestrial planets were too hot for hydrous minerals to form (e.g., Cyr, Sears & Lunine 1998;Delsemme 2000;Cuzzi & Zahnle 2004). Ciesla & Lauretta (2004) suggest that hydrous minerals were formed in the outer asteroid belt region of the solar nebula and were then transported to the hotter regions of the nebula (i.e., Earth and Mars) by gas drag, where they were incorporated into the planetesimals that formed there.…”

Section: Early Accretion Of Water From Inward Migration Of Hydrated Pmentioning

confidence: 99%

Origin of water on the terrestial planets

Drake

Campins

2005

Proc. IAU

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Abstract. We examine the origin of water in the terrestrial planets. We list various geochemical measurements that may be used to discriminate between different endogenous and exogenous sources of water. Late stage delivery of significant quantities of water from asteroidal and cometary sources appears to be ruled out by isotopic and molecular ratio considerations, unless either comets and asteroids currently sampled spectroscopically and by meteorites are unlike those falling to Earth 4.5 Ga ago or our measurements are not representative of those bodies. The dust in the accretion disk from which terrestrial planets formed was bathed in a gas of H, He and O. The dominant gas phase species were H 2, He, H2O, and CO. Thus grains in the accretion disk must have been exposed to and adsorbed H2 and water. We examine the efficacy of nebular gas adsorption as a mechanism by which the terrestrial planets accreted "wet". A simple model suggests that grains accreted to Earth could have adsorbed 1 -3 Earth oceans of water. The fraction of this water retained during accretion is unknown, but these results suggest that at least some of the water in the terrestrial planets may have originated by adsorption.

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Distribution and Evolution of Water Ice in the Solar Nebula: Implications for Solar System Body Formation

Cited by 117 publications

References 27 publications

The evolution of the water distribution in a viscous protoplanetary disk

The evolution of the water distribution in a viscous protoplanetary disk

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

Origin of water on the terrestial planets

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