The terrestrial planet formation paradox inferred from high-resolution N-body simulations

Abstract

Recent improvements to GPU hardware and the symplectic N-body code GENGA allow for unprecedented resolution in simulations of planet formation. In this paper, we report results from high-resolution N-body simulations of terrestrial planet formation that are mostly direct continuation of our previous 10 Myr simulations (Woo et al. 2021a) until 150 Myr. By assuming that Jupiter and Saturn have always maintained their current eccentric orbits (EJS), we are able to achieve a reasonably good match to the current inner solar system architecture. However, due to the strong radial mixing that occurs in the EJS scenario, it has difficulties in explaining the known isotopic differences between bodies in the inner solar system, most notably between Earth and Mars. On the other hand, assuming initially circular orbits for Jupiter and Saturn (CJS) can reproduce the observed low degree of radial mixing in the inner solar system, while failing to reproduce the current architecture of the inner solar system. These outcomes suggest a possible paradox between dynamical structure and cosmochemical data for the terrestrial planets within the classical formation scenario.

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Cited by in corpus (20)

• Nucleation and growth of iron pebbles explains the formation of iron-rich planets akin to Mercury
• Terrestrial planet formation from a ring
• Comparisons of the core and mantle compositions of earth analogs from different terrestrial planet formation scenarios
• Mercury's formation within the Early Instability Scenario
• Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation
• The cosmochemistry of planetary systems
• How the presence of a giant planet affects the outcome of terrestrial planet formation simulations
• Accretion regions of meteorite parent bodies inferred from a two-endmember isotopic mixing model
• Mid-infrared time-domain study of recent dust production events in the extreme debris disc of TYC 4209-1322-1
• Forming rocky exoplanets around K-dwarf stars
• Constraining the Origin of Mars via Simulations of Multi-Stage Core Formation
• Abundant sub-micron grains revealed in newly discovered extreme debris discs
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• Probabilities of collisions of bodies ejected from forming Earth with the terrestrial planets
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• Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery
• Spatial distribution of isotopes and compositional mixing in the inner protoplanetary disk
• Migration of celestial bodies in the Solar system and in several exoplanetary systems
• Evolution of gas envelopes and outgassed atmospheres of rocky planets formed via pebble accretion
• Coupling dynamical accretion and chemical differentiation: A unified framework for the diversity of Earth and Mars