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

Abstract

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 that grow rapidly experience radiogenic ingrowth of mantle ${}^{182}$W that is inconsistent with the measured terrestrial composition, unless much of the tungsten is removed by an impactor core that mixes thoroughly with the target mantle. For physically Earth-like surviving planets, we find that the fraction of equilibrating impactor core $k_{\text{core}}\ge 0.6$ is required to produce results agreeing with observed terrestrial tungsten anomalies (assuming equilibration with relatively large volumes of target mantle material; smaller equilibrating mantle volumes would require even larger $k_{\text{core}}$). This requirement of substantial core re-equilibration may be difficult to reconcile with fluid dynamical predictions and hydrocode simulations of mixing during large impacts, and hence this result does not favor the rapid planet building that results from Grand Tack accretion.

34 pages, 5 figures, published in EPSL

References in corpus (3)

• Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
• Highly Siderophile Elements in the Earth's Mantle as a Clock for the Moon-forming Impact
• Lunar and Terrestrial Planet Formation in the Grand Tack Scenario

Cited by in corpus (5)

• Metal-silicate partitioning of W and Mo and the role of carbon in controlling their abundances in the Bulk Silicate Earth
• The Effect of Inefficient Accretion on Planetary Differentiation
• The early instability scenario: Mars' mass explained by Jupiter's orbit
• Mercury's formation within the Early Instability Scenario
• Evidence of a primordial isotopic gradient in the inner region of the solar protoplanetary disc