Making the Solar System

Abstract

We model the early stages of planet formation in the Solar System, including continual planetesimal formation, and planetesimal and pebble accretion onto planetary embryos in an evolving disk driven by a disk wind. The aim is to constrain aspects of planet formation that have large uncertainties by matching key characteristics of the Solar System. The model produces a good fit to these characteristics for a narrow range of parameter space. Planetary growth beyond the ice line is dominated by pebble accretion. Planetesimal accretion is more important inside the ice line. Pebble accretion inside the ice line is slowed by higher temperatures, partial removal of inflowing pebbles by planetesimal formation and pebble accretion further out in the disk, and increased radial velocities due to gas advection. The terrestrial planets are prevented from accreting much water ice because embryos beyond the ice line reach the pebble isolation mass before the ice line enters the terrestrial-planet region. When only pebble accretion is considered, embryos typically remain near their initial mass or grow to the pebble-isolation mass. Adding planetesimal accretion allows Mars-sized objects to form inside the ice line, and allows giant-planet cores to form over a wider region beyond the ice line. In the region occupied by Mercury, pebble Stokes numbers are small. This delays the formation of embryos and stunts their growth, so that only low-mass planets can form here.

Accepted for publication in the Astrophysical Journal

References in corpus (15)

• The origins and concentrations of water, carbon, nitrogen and noble gases on Earth
• Coagulation, fragmentation and radial motion of solid particles in protoplanetary disks
• Particle Stirring in Turbulent Gas Disks: Including Orbital Oscillations
• Closed-form expressions for particle relative velocities induced by turbulence
• Separating gas-giant and ice-giant planets by halting pebble accretion
• The stickiness of micrometer-sized water-ice particles
• Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds
• Dust masses of young disks: constraining the initial solid reservoir for planet formation
• Contacts of Water Ice in Protoplanetary Disks - Laboratory Experiments
• Survival of the mm-cm size grain population observed in protoplanetary disks
• Planetesimal Population Synthesis: Pebble Flux Regulated Planetesimal Formation
• How do T Tauri stars accrete
• Evolution of the Water Snow Line in Magnetically Accreting Protoplanetary Disks
• The importance of thermal torques on the migration of planets growing by pebble accretion
• Steamworlds: atmospheric structure and critical mass of planets accreting icy pebbles

Cited by in corpus (7)

• Sequential giant planet formation initiated by disc substructure
• Which stars can form planets: Planetesimal formation at low metallicities
• Terrestrial planet formation during giant planet formation and giant planet migration I: The first 5 million years
• Long-term evolution of the temperature structure in magnetized protoplanetary disks and its implication for the dichotomy of planetary composition
• FAST Observations of Four Comets to Search for the Molecular Line Emissions between 1.0 and 1.5 GHz Frequencies
• Forming Earth-like and Low-Mass Rocky Exoplanets Through Pebble and Planetesimal Accretion
• Setting the Stage: The Early History of the Solar System