Growing Mars fast: High-resolution GPU simulations of embryo formation

Abstract

Recent high precision meteoritic data improve constraints on the formation timescale and bulk composition of the terrestrial planets. High resolution N-body simulations allow direct comparison of embryo growth timescale and accretion zones to these constraints. In this paper, we present results of high resolution simulations for embryo formation from a disc of up to 41,000 fully-self gravitating planetesimals with the GPU-based N-body code GENGA. Our results indicate that the growth of embryos are highly dependent on the initial conditions. More massive initial planetesimals, a shorter gas disc decay timescale and initially eccentric Jupiter and Saturn (EJS) all lead to faster growth of embryos. Asteroid belt material can thereby be implanted into the terrestrial planet region via sweeping secular resonances. This could possibly explain the rapid growth of Mars within 10 Myr inferred from its Hf-W chronology. The sweeping secular resonance almost completely clears the asteroid belt and deposits this material in the Mercury-Venus region, altering the composition of embryos there. This could result in embryos in the Mercury-Venus region accreting an unexpectedly high mass fraction from beyond 2 AU. Changing the initial orbits of Jupiter and Saturn to more circular (CJS) or assuming embryos formed in a gas free environment removes the sweeping secular resonance effect and thus greatly decreases material accreted from beyond 2 AU for Mercury-Venus region embryos. We therefore propose that rock samples from Mercury and Venus could aid greatly in deducing the condition and lifetime of the initial protoplanetary gas disc during planetesimal and embryo formation, as well as the initial architecture of the giant planets.

Accepted for publication in Icarus

References in corpus (63)

• Disk Frequencies and Lifetimes in Young Clusters
• Rapid planetesimal formation in turbulent circumstellar discs
• A low mass for Mars from Jupiter's early gas-driven migration
• Rapid growth of gas-giant cores by pebble accretion
• Catastrophic disruptions revisited
• Asteroids Were Born Big
• Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
• Towards planetesimals: dense chondrule clumps in the protoplanetary nebula
• High-resolution simulations of the final assembly of Earth-like planets 1: terrestrial accretion and dynamics
• On the orbital evolution and growth of protoplanets embedded in a gaseous disc
• Formation of the Terrestrial Planets from a Narrow Annulus
• Models of Jupiter's Growth Incorporating Thermal and Hydrodynamic Constraints
• Growing the gas-giant planets by the gradual accumulation of pebbles
• The Extreme Ultraviolet and X-Ray Sun in Time: High-Energy Evolutionary Tracks of a Solar-Like Star
• Constraints on the mass of a habitable planet with water of nebular origin
• Close-in planetesimal formation by pile-up of drifting pebbles
• Growing the terrestrial planets from the gradual accumulation of sub-meter sized objects
• Terrestrial Planet Formation I. The Transition from Oligarchic Growth to Chaotic Growth
• Mars' Growth Stunted by an Early Giant Planet Instability
• From planetesimals to terrestrial planets: N-body simulations including the effects of nebular gas and giant planets
• Origin and Loss of nebula-captured hydrogen envelopes from "sub"- to "super-Earths" in the habitable zone of Sun-like stars
• Type I Planetary Migration with MHD Turbulence
• The Evolution of Stellar Rotation and the hydrogen atmospheres of habitable-zone Terrestrial Planets
• On the evolution of eccentric and inclined protoplanets embedded in protoplanetary disks
• Lunar and Terrestrial Planet Formation in the Grand Tack Scenario
• 60Fe-60Ni chronology of core formation in Mars
• Dispersion in the lifetime and accretion rate of T Tauri discs
• The Frequency of Giant impacts on Earth-like Worlds
• The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
• Dynamical evidence for an early giant planet instability
• The GENGA Code: Gravitational Encounters in N-body simulations with GPU Acceleration
• Onset of giant planet migration before 4480 million years ago
• Planetary Growth with Collisional Fragmentation and Gas Drag
• Accretion of Terrestrial Planets from Oligarchs in a Turbulent Disk
• Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt
• The Feeding Zones of Terrestrial Planets and Insights into Moon Formation
• Compositional evolution during rocky protoplanet accretion
• Terrestrial Planet Formation in a protoplanetary disk with a local mass depletion: A successful scenario for the formation of Mars
• The Ecological Impact of High-performance Computing in Astrophysics
• The origin of s-process isotope heterogeneity in the solar protoplanetary disk
• Planetesimals to Terrestrial Planets: collisional evolution amidst a dissipating gas disk
• Escape and fractionation of volatiles and noble gases from Mars-sized planetary embryos and growing protoplanets
• Hydrodynamic simulations of captured protoatmospheres around Earth-like planets
• Gravitational Instabilities in Gaseous Protoplanetary Disks and Implications for Giant Planet Formation
• Growth of Dust as the Initial Step Toward Planet Formation
• Analysis of terrestrial planet formation by the Grand Tack model: System architecture and tack location
• A Lagrangian Integrator for Planetary Accretion and Dynamics (LIPAD)
• An ancient and a primordial collisional family as the main sources of X-type asteroids of the inner Main Belt
• Terrestrial Planet Formation During the Migration and Resonance Crossings of the Giant Planets
• Gravitational fragmentation and formation of giant protoplanets on tens-of-au orbits
• Small Planetesimals in a Massive Disk Formed Mars
• The cool and distant formation of Mars
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• Jupiter's influence on the building blocks of Mars and Earth
• N-body simulations of oligarchic growth of Mars: Implications for Hf-W chronology
• Planetesimal clearing and size-dependent asteroid retention by secular resonance sweeping during the depletion of the solar nebula
• Constraining the Formation of the Four Terrestrial Planets in the Solar System
• Planetesimals to Protoplanets II: Effect of Debris on Terrestrial Planet Formation
• Stochasticity & Predictability in Terrestrial Planet Formation
• The curious case of Mars formation
• Isotopically distinct terrestrial planets via local accretion
• A particle-based hybrid code for planet formation
• N-body simulations of terrestrial planet growth with resonant dynamical friction

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• The terrestrial planet formation paradox inferred from high-resolution N-body simulations
• Terrestrial planet formation from a ring
• Reduced late bombardment on rocky exoplanets around M-dwarfs
• Dynamical avenues for Mercury's origin I: The lone survivor of a primordial generation of short-period proto-planets
• Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants
• The Role of Giant Impacts in Planet Formation
• Dynamical avenues for Mercury's origin II: in-situ formation in the inner terrestrial disk
• The early instability scenario: Mars' mass explained by Jupiter's orbit
• Effects of pebble accretion on the growth and composition of planetesimals in the inner Solar System
• Mercury as the relic of Earth and Venus' outward migration
• Comparisons of the core and mantle compositions of earth analogs from different terrestrial planet formation scenarios
• Mercury's formation within the Early Instability Scenario
• Mars' formation can constrain the primordial orbits of the gas giants
• Accretion regions of meteorite parent bodies inferred from a two-endmember isotopic mixing model
• Terrestrial planet formation during giant planet formation and giant planet migration I: The first 5 million years
• Forming rocky exoplanets around K-dwarf stars
• Constraining the Origin of Mars via Simulations of Multi-Stage Core Formation
• Evidence of a primordial isotopic gradient in the inner region of the solar protoplanetary disc
• Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery
• Forming Earth-like and Low-Mass Rocky Exoplanets Through Pebble and Planetesimal Accretion
• Spatial distribution of isotopes and compositional mixing in the inner protoplanetary disk
• GENGA II: GPU planetary N-body simulations with non-Newtonian forces and high number of particles
• Impact chronology of leftover planetesimals
• Episodic planetesimal disruptions triggered by dissipation of gas disk
• Coupling dynamical accretion and chemical differentiation: A unified framework for the diversity of Earth and Mars