Planetesimal rings as the cause of the Solar System's planetary architecture

Abstract

Astronomical observations reveal that protoplanetary disks around young stars commonly have ring- and gap-like structures in their dust distributions. These features are associated with pressure bumps trapping dust particles at specific locations, which simulations show are ideal sites for planetesimal formation. Here we show that our Solar System may have formed from rings of planetesimals -- created by pressure bumps -- rather than a continuous disk. We model the gaseous disk phase assuming the existence of pressure bumps near the silicate sublimation line (at $T\sim$1400~K), water snowline (at $T\sim$170~K), and CO-snowline (at $T\sim$30~K). Our simulations show that dust piles up at the bumps and forms up to three rings of planetesimals: a narrow ring near 1~au, a wide ring between $\sim$3-4~au and $\sim$10-20~au, and a distant ring between $\sim$20~au and $\sim$45~au. We use a series of simulations to follow the evolution of the innermost ring and show how it can explain the orbital structure of the inner Solar System and provides a framework to explain the origins of isotopic signatures of Earth, Mars and different classes of meteorites. The central ring contains enough mass to explain the rapid growth of the giant planets' cores. The outermost ring is consistent with dynamical models of Solar System evolution proposing that the early Solar System had a primordial planetesimal disk beyond the current orbit of Uranus.

arXiv commentPublished in Nature Astronomy on Dec 30, 2021. Authors' version including Methods and Supplementary Information

References in corpus (59)

• The chemical composition of the Sun
• Rapid planetesimal formation in turbulent circumstellar discs
• A low mass for Mars from Jupiter's early gas-driven migration
• The false positive rate of Kepler and the occurrence of planets
• A simple model for the evolution of the dust population in protoplanetary disks
• The effect of gas drag on the growth of protoplanets -- Analytical expressions for the accretion of small bodies in laminar disks
• Solar System evolution from compositional mapping of the asteroid belt
• The Disk Substructures at High Angular Resolution Project (DSHARP): II. Characteristics of Annular Substructures
• Making other Earths: Dynamical Simulations of Terrestrial Planet Formation and Water Delivery
• Separating gas-giant and ice-giant planets by halting pebble accretion
• The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
• Trapping dust particles in the outer regions of protoplanetary disks
• Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Imaging of the CO Snow Line in a Solar Nebula Analog
• The stickiness of micrometer-sized water-ice particles
• Formation of the Terrestrial Planets from a Narrow Annulus
• Concentrating small particles in protoplanetary disks through the streaming instability
• 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
• Planetesimal formation starts at the snow line
• The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Growing the gas-giant planets by the gradual accumulation of pebbles
• Fossilized condensation lines in the Solar System protoplanetary disk
• Close-in planetesimal formation by pile-up of drifting pebbles
• How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
• The radial dependence of pebble accretion rates: A source of diversity in planetary systems I. Analytical formulation
• Magnetic Flux Concentration and Zonal Flows in Magnetorotational Instability Turbulence
• Dust Density Distribution and Imaging Analysis of Different Ice Lines in Protoplanetary Disks
• Gravoturbulent Planetesimal Formation: The Positive Effect of long-lived Zonal Flows
• High-Temperature Ionization in Protoplanetary Disks
• 3D Radiation Non-ideal Magnetohydrodynamical Simulations Of The Inner Rim In Protoplanetary Disks
• Stellar irradiated discs and implications on migration of embedded planets II: accreting-discs
• Robustness of N2H+ as tracer of the CO snowline
• Differentiation of Planetesimals and the Thermal Consequences of Melt Migration
• Terrestrial Planet Formation Constrained by Mars and the Structure of the Asteroid Belt
• Dust Evolution Can Produce Scattered Light Gaps in Protoplanetary Disks
• Terrestrial Planet Formation in a protoplanetary disk with a local mass depletion: A successful scenario for the formation of Mars
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• Constraining the giant planets' initial configuration from their evolution: implications for the timing of the planetary instability
• Planet formation by pebble accretion in ringed disks
• Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn
• Planetesimals to Terrestrial Planets: collisional evolution amidst a dissipating gas disk
• Dust-Pileup at the Dead-Zone Inner Edge and Implications for the Disk Shadow
• A very early origin of isotopically distinct nitrogen in inner Solar System protoplanets
• A Lagrangian Integrator for Planetary Accretion and Dynamics (LIPAD)
• Planetesimal Formation in Magnetorotationally Dead Zones: Critical Dependence on the Net Vertical Magnetic Flux
• Growing and Trapping Pebbles with Fragile Collisions of Particles in Protoplanetary Disks
• OSSOS XX: The Meaning of Kuiper Belt Colors
• The cool and distant formation of Mars
• The impact of planet wakes on the location and shape of the water iceline in a protoplanetary disk
• Revisiting the pre-main-sequence evolution of stars II. Consequences of planet formation on stellar surface composition
• The effect of a strong pressure bump in the Sun's natal disk: Terrestrial planet formation via planetesimal accretion rather than pebble accretion
• Forming pressure-traps at the snow-line to isolate isotopic reservoirs in the absence of a planet
• The water-ice line as a birthplace of planets: Implications of a species-dependent dust fragmentation threshold
• Linking planetesimal and dust content in protoplanetary disks via a local toy model
• The Formation and Evolution of Ordinary Chondrite Parent Bodies
• Building protoplanetary disks from the molecular cloud: redefining the disk timeline

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• The Exoplanet Radius Valley from Gas-driven Planet Migration and Breaking of Resonant Chains
• Leaky dust traps: How fragmentation impacts dust filtering by planets
• Origin of isotopic diversity among carbonaceous chondrites
• Accretion of the earliest inner solar system planetesimals beyond the water-snowline
• Giants are bullies: how their growth influences systems of inner sub-Neptunes and super-Earths
• How to make giant planets via pebble accretion
• Anatomy of rocky planets formed by rapid pebble accretion I. How icy pebbles determine the core fraction and FeO contents
• Terrestrial planet formation from a ring
• Edge-of-the-Multis: Evidence for a Transition in the Outer Architectures of Compact Multi-Planet Systems
• Implications of Jupiter Inward Gas-Driven Migration for the Inner Solar System
• A Self-Consistent Model for Dust-Gas Coupling in Protoplanetary Disks
• A complete census of planet-hosting binaries
• The interplay between pebble and planetesimal accretion in population synthesis models and its role in giant planet formation
• Interior Controls on the Habitability of Rocky Planets
• A race against the clock: Constraining the timing of cometary bombardment relative to Earth's growth
• Origin of Water in the Terrestrial Planets: Insights from Meteorite Data and Planet Formation Models
• Mixing is easy: New insights for cosmochemical evolution from pre-stellar core collapse
• Identification of a 4.3 billion year old asteroid family and planetesimal population in the Inner Main Belt
• The rapid formation of macromolecules in irradiated ice of protoplanetary disk dust traps
• Exploring the recycling model of Phobos formation: rubble-pile satellites
• Explaining Mercury via a single giant impact is highly unlikely
• Three-dimensional transport of solids in a protoplanetary disk containing a growing giant planet
• Rethinking the role of the giant planet instability in terrestrial planet formation models
• Dust-Gas Coupling in Turbulence- and MHD Wind-Driven Protoplanetary Disks: Implications for Rocky Planet Formation
• Mercury's formation within the Early Instability Scenario
• Terrestrial planet and asteroid belt formation by Jupiter-Saturn chaotic excitation
• Late Accretion of Ceres-like Asteroids and Their Implantation into the Outer Main Belt
• Revisiting equilibrium condensation and rocky planet compositions: Introducing the ECCOplanets code
• Planetesimal and planet formation in transient dust traps
• How the presence of a giant planet affects the outcome of terrestrial planet formation simulations
• Formation of inner planets in the presence of a Cold Jupiter: orbital evolution and relative velocities of planetesimals
• Formation of super-Earths and mini-Neptunes from rings of planetesimals
• Crash Chronicles: relative contribution from comets and carbonaceous asteroids to Earth's volatile budget in the context of an Early Instability
• Terrestrial planet formation during giant planet formation and giant planet migration I: The first 5 million years
• Physicochemical Controls on the Compositions of the Earth and Planets
• The late formation of chondrites as a consequence of Jupiter-induced gaps and rings
• How does the chemical composition of solids influence the formation of planetesimals?
• The Dissolution of Planetesimals in Electrostatic Fields
• Origin of compact exoplanetary systems during disk infall
• Formation of the four terrestrial planets in the Jupiter-Saturn chaotic excitation scenario: fundamental properties and water delivery
• Homogeneous accretion of the Earth in the inner Solar System
• Different arrival times of CM and CI-like bodies from the outer Solar System to the asteroid belt
• Acceleration of planetary migration: Resonance crossing and planetesimal ring
• Chondrule Formation During Low-Speed Collisions of Planetesimals: A Hybrid Splash-Flyby Framework
• Earth accreted increasingly oxidized material as it grew constraining Theia to be small and relatively oxidized
• Coupling dynamical accretion and chemical differentiation: A unified framework for the diversity of Earth and Mars
• Chondrite Parent Bodies as Escaped Satellites of Proto-Planetary Embryos
• Shaken, not stirred: inefficient mixing of CM- and CI-like materials
• A mini-review on combinatorial solutions to the Marcus-Lushnikov irreversible aggregation
• Runaway Growth of Planetesimals Revisited: Presenting Criteria Required for Realistic Modeling of Planetesimal Growth