Constraints on terrestrial planet formation timescales and equilibration processes in the Grand Tack scenario from Hf-W isotopic evolution.

@article{Zube2019ConstraintsOT,
  title={Constraints on terrestrial planet formation timescales and equilibration processes in the Grand Tack scenario from Hf-W isotopic evolution.},
  author={N. Zube and F. Nimmo and R. Fischer and S. Jacobson},
  journal={Earth and planetary science letters},
  year={2019},
  volume={522},
  pages={
          210-218
        }
}
We examine 141 N-body simulations of terrestrial planet late-stage accretion that use the Grand Tack scenario, coupling the collisional results with a hafnium-tungsten (Hf-W) isotopic evolution model. Accretion in the Grand Tack scenario results in faster planet formation than classical accretion models because of higher planetesimal surface density induced by a migrating Jupiter. Planetary embryos which grow rapidly experience radiogenic ingrowth of mantle tungsten which is inconsistent with… Expand
View on PubMed
ncbi.nlm.nih.gov
4 Citations
Background Citations
1

4 Citations

Citation Type

Citation Type

Timing of Martian Core Formation from Models of Hf–W Evolution Coupled with N-body Simulations
11 Determining how and when Mars formed has been a long-standing challenge for 12 planetary scientists. The size and orbit of Mars are difficult to reproduce in classical simulations 13 of planetary… Expand
Planet formation: key mechanisms and global models
Models of planet formation are built on underlying physical processes. In order to make sense of the origin of the planets we must first understand the origin of their building blocks. This review… Expand
The origin of the Moon’s Earth-like tungsten isotopic composition from dynamical and geochemical modeling
TLDR
The authors find that traditional models of Moon formation are very unlikely to reproduce the Moon's Earth-like isotopic composition, and conclude that alternate explanations for the Moon’s isotopic compositions are likely more plausible. Expand
Metal–silicate partitioning of W and Mo and the role of carbon in controlling their abundances in the bulk silicate earth
Abstract The liquid metal–liquid silicate partitioning of molybdenum and tungsten during core formation must be well-constrained in order to understand the evolution of Earth and other planetary… Expand

References

SHOWING 1-10 OF 56 REFERENCES
Isotopic outcomes of N-body accretion simulations: Constraints on equilibration processes during large impacts from Hf/W observations
Abstract Most estimates of planetary core formation timescales using hafnium–tungsten (Hf–W) isotopes employ analytical expressions assuming either continuous planetary growth or instantaneous core… Expand
Tungsten isotopic evolution during late-stage accretion: Constraints on Earth–Moon equilibration
Abstract We couple the results of N-body simulations of late-stage accretion (O'Brien et al., 2006) to a hafnium–tungsten (Hf–W) isotopic evolution code to investigate the evolution of planetary… Expand
Turbulent Mixing of Metal and Silicate during Planet Accretion – and interpretation of the Hf-W chronometer
In the current view of planet formation, the final assembly of the Earth involved giant collisions between proto-planets (> 1000 km radius), with the Moon formed as a result of one such impact. At… Expand
Fast accretion of the Earth with a late Moon-forming giant impact
TLDR
A model of the 182W isotopic evolution of the accreting Earth, including constraints from partitioning of refractory siderophile elements (Ni, Co, W, V, and Nb) during core formation, which can explain the discrepancy in the timing of the Moon-forming giant impact (MGI). Expand
Rapid accretion and early core formation on asteroids and the terrestrial planets from Hf–W chronometry
TLDR
It is concluded that core formation in the terrestrial planets and the formation of the Moon must have occurred during the first ∼30 million years of the life of the Solar System. Expand
Bulk chemical and Hf{W isotopic consequences of incomplete accretion during planet formation
Late-stage accretion involves collisions which may result in complete or incomplete merging of the two objects, hit-and-run encounters, or mass loss from the target. We use a recent N-body study… Expand
Accretion and differentiation of the terrestrial planets with implications for the compositions of early-formed Solar System bodies and accretion of water
Abstract In order to test accretion simulations as well as planetary differentiation scenarios, we have integrated a multistage core–mantle differentiation model with N-body accretion simulations.… Expand
A short timescale for terrestrial planet formation from Hf–W chronometry of meteorites
TLDR
Measurements of tungsten isotope compositions and hafnium–tungsten ratios of several meteorites indicate that the bulk of metal–silicate separation in the Solar System was completed within <30 Myr, completely consistent with other evidence for rapid planetary formation. Expand
Radial mixing and Ru-Mo isotope systematics under different accretion scenarios.
TLDR
This model starts by applying an initial step function in Ru-Mo isotopic composition, with compositions reflecting those in meteorites, and traces compositional evolution as planets accrete, and gives testable predictions that Mars has zero Ru anomaly and small or zero Mo anomaly, and the Moon has zero Mo anomalies. Expand
Effects of core formation on the Hf-W isotopic composition of the Earth and dating of the Moon-forming impact.
TLDR
The Hf-W isotopic evolution of the Earth is improved over previous studies by combining a large number of N-body simulations of planetary accretion with a core formation model that includes self-consistent evolution of oxygen fugacity and a partition coefficient of tungsten that evolves with changing pressure, temperature, composition, and oxygen fugacious. Expand
...
1
2
3
4
5
...