Structure and Transport in the Solar Nebula from Constraints on Deuterium Enrichment and Giant Planets Formation

Drouart, A.; Dubrulle, B.; Gautier, D.; Robert, François

doi:10.1006/icar.1999.6137

Cited by 155 publications

(166 citation statements)

References 74 publications

Supporting

Mentioning

160

Contrasting

Order By: Relevance

“…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: 73%

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

et al. 2015

View full text Add to dashboard Cite

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.

show abstract

Section: Water and D/hmentioning

confidence: 73%

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

et al. 2015

View full text Add to dashboard Cite

show abstract

“…For example, low-temperature ion-molecule reactions in the cores of molecular clouds can enhance the D/H ratio in icy grains by as much as two orders of magnitude above that observed in the interstellar medium (e.g., Gensheimer, Mauersberger & Wilson 1996). In our solar system, there is evidence for more than one reservoir of hydrogen (Drouart, Dubrulle, Gautier, et al 1999;Mousis et al 2000;Robert 2001;Hersant, Gautier & Hure 2001 and references therein). The solar nebula gas D/H ratio is estimated from observations of CH 4 in Jupiter and Saturn to be a low 2.1 ± 0.4 × 10 −5 (Lellouch et al 2001).…”

Section: D/h Ratiosmentioning

confidence: 96%

Origin of water on the terrestial planets

Drake

Campins

2005

Proc. IAU

View full text Add to dashboard Cite

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.

show abstract

“…This equation contains terms relating to both the dynamics and thermodynamics of the protoplanetary nebula. The forcing function that drives the equation may include nonequilibrium chemical reactions (Drouart et al 1999), systems of coupled reactions (Aikawa & Herbst 1999), or rate of depletion models (Cassen 1996). On the other hand, coefficients of the transport terms arise from the dynamic evolution of the nebula.…”

Section: Introductionmentioning

confidence: 99%

“…There are a wide variety of disk models available for this purpose. They include simple quasi-steady models (Drouart et al 1999;Gail 2001;Stevenson 1990), numerical solutions of the full equations using the -viscosity formulation (Ruden & Lin 1986;Ruden & Pollack 1991), analytical fits to observational data (Stepinski 1998), general similarity solutions (Hartmann et al 1998), and functional models (Cassen 1996(Cassen , 2001.…”

Section: Introductionmentioning

confidence: 99%

“…Such models could be useful for large-scale physical-chemical hydrodynamic analysis of an evolving nebula where the evolutionary model serves as just one component of a complex process. For example, Drouart et al (1999) used a model consisting of a simple power-law form of the mass accretion rate combined with the quasi-steady disk evolution model of Dubrulle (1993) to approximate the dynamic terms in the convection-diffusion equation. Gail (2001) used a steady state version of the disk evolution equations to compute radial mixing in protoplanetary disks.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

A Simplified Model for an Evolving Protoplanetary Nebula

Davis¹

2003

ApJ

View full text Add to dashboard Cite

The dynamic evolution of a protoplanetary nebula is investigated using analytical solutions of the surface density transport equations. Constant-and so-called -viscosity turbulence models are compared with a functional analytical model and the well-known -viscosity formulation. The model presented here is related to a number of simplified disk evolution models but is also associated with -viscosity models based on hydrodynamic generation of turbulence. The -viscosity model, heretofore used for steady state disks, is shown to be a useful approximation for disk evolution problems.

show abstract

Structure and Transport in the Solar Nebula from Constraints on Deuterium Enrichment and Giant Planets Formation

Cited by 155 publications

References 74 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

Origin of water on the terrestial planets

A Simplified Model for an Evolving Protoplanetary Nebula

Contact Info

Product

Resources

About