Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery

Abstract

The Jupiter-Saturn chaotic excitation (JSCE) scenario proposes that the protoplanetary disk was dynamically excited and depleted beyond ~1-1.5 au in a few Myr, offering a new and plausible explanation for several observed properties of the inner solar system. Here, we expanded our previous work by conducting a comprehensive analysis of 37 optimal terrestrial planet systems obtained in the context of the JSCE scenario. Each optimal system harbored exactly four terrestrial planets analogs to Mercury, Venus, Earth, and Mars. We further investigated water delivery, feeding zones, and accretion history for the planet analogs, which allowed us to better constrain the water distribution in the disk. The main findings of this work are as follows: 1) the formation of four terrestrial planets with orbits and masses similar to those observed in our solar system in most of our sample, as evidenced by the dynamically colder and hotter orbits of Venus-Earth and Mercury-Mars analogs, and the high success rates of similar mutual orbital separations (~40-85%) and mass ratios of the planets (~70-90%) among the 37 systems; and 2) water was delivered to all terrestrial planets during their formation through the accretion of water-bearing disk objects from beyond ~1-1.5 au. The achievement of Earth's estimated bulk water content required the disk to contain sufficient water mass distributed within those objects initially. This requirement implies that Mercury, Venus, and Mars acquired water similar to the amount on Earth during their formation. Several of our planet analogs also matched additional constraints, such as the timing of Moon formation by a giant impact, Earth's late accretion mass and composition, and Mars's formation timescale.

arXiv commentManuscript accepted for publication in Icarus

References in corpus (59)

• A low mass for Mars from Jupiter's early gas-driven migration
• The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
• Building Terrestrial Planets
• Building the Terrestrial Planets: Constrained Accretion in the Inner Solar System
• Formation of the Terrestrial Planets from a Narrow Annulus
• Dynamical Evolution of the Early Solar System
• Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
• Close-in planetesimal formation by pile-up of drifting pebbles
• Neptune's Migration into a Stirred-Up Kuiper Belt: A Detailed Comparison of Simulations to Observations
• 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
• Chaotic diffusion in the Solar System
• Multiple Impact Origin for the Moon
• Lunar and Terrestrial Planet Formation in the Grand Tack Scenario
• Terrestrial planet formation from lost inner solar system material
• Planetesimal rings as the cause of the Solar System's planetary architecture
• Evolution of Water Reservoirs on Mars: Constraints from Hydrogen Isotopes in Martian Meteorites
• The Delivery of Water During Terrestrial Planet Formation
• 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
• Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt
• Formation, stratification, and mixing of the cores of Earth and Venus
• The Fragility of the Terrestrial Planets During a Giant Planet Instability
• Constraining the giant planets' initial configuration from their evolution: implications for the timing of the planetary instability
• Forming Mercury by Giant Impacts
• Early Solar System instability triggered by dispersal of the gaseous disk
• Planetesimals to Terrestrial Planets: collisional evolution amidst a dissipating gas disk
• Analysis of terrestrial planet formation by the Grand Tack model: System architecture and tack location
• The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
• Terrestrial Planet Formation from an Annulus
• Constraining the primordial orbits of the Terrestrial Planets
• Excitation and depletion of the asteroid belt in the early instability scenario
• Terrestrial Planet Formation During the Migration and Resonance Crossings of the Giant Planets
• The Asteroid Belt as a Relic From a Chaotic Early Solar System
• Bayesian Inference on the Isotopic Building Blocks of Mars and Earth
• Nucleation and growth of iron pebbles explains the formation of iron-rich planets akin to Mercury
• Formation of Venus, Earth and Mars: Constrained by isotopes
• Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals
• Terrestrial planet formation by torque-driven convergent migration of planetary embryos
• Setting the Stage: Planet formation and Volatile Delivery
• Growing Mars fast: High-resolution GPU simulations of embryo formation
• Instabilities in the Early Solar System due to a Self-gravitating Disk
• Dynamical Constraints on Mercury's Collisional Origin
• Jumping Jupiter can explain Mercury's orbit
• Constraining the Formation of the Four Terrestrial Planets in the Solar System
• Realistic collisional water transport during terrestrial planet formation: Self-consistent modeling by an N-body--SPH hybrid code
• Terrestrial planet formation from a ring
• The terrestrial planet formation paradox inferred from high-resolution N-body simulations
• Composition and Size Dependent Sorting in Preplanetary Growth: Seeding the Formation of Mercury-like Planets
• Formation of Terrestrial Planets in Disks with Different Surface Density Profiles
• The Role of Giant Impacts in Planet Formation
• The early instability scenario: Mars' mass explained by Jupiter's orbit
• Dynamical avenues for Mercury's origin II: in-situ formation in the inner terrestrial disk
• A race against the clock: Constraining the timing of cometary bombardment relative to Earth's growth
• Rethinking the role of the giant planet instability in terrestrial planet formation models
• Mercury's formation within the Early Instability Scenario
• Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation
• Onset of oligarchic growth and implication for accretion histories of dwarf planets
• Can narrow disks in the inner solar system explain the four terrestrial planets?

Cited by in corpus (1)

• Probabilities of collisions of bodies ejected from forming Earth with the terrestrial planets