A Hybrid N-body--Coagulation Code for Planet Formation

Abstract

We describe a hybrid algorithm to calculate the formation of planets from an initial ensemble of planetesimals. The algorithm uses a coagulation code to treat the growth of planetesimals into oligarchs and explicit N-body calculations to follow the evolution of oligarchs into planets. To validate the N-body portion of the algorithm, we use a battery of tests in planetary dynamics. Several complete calculations of terrestrial planet formation with the hybrid code yield good agreement with previously published calculations. These results demonstrate that the hybrid code provides an accurate treatment of the evolution of planetesimals into planets.

Astronomical Journal, accepted; 33 pages + 11 figures

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• Planetary Growth with Collisional Fragmentation and Gas Drag
• Making the Earth: Combining Dynamics and Chemistry in the Solar System
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• A New Hybrid N-Body-Coagulation Code for the Formation of Gas Giant Planets
• A New Algorithm for Self-Consistent 3-D Modeling of Collisions in Dusty Debris Disks
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• Variations on Debris Disks II. Icy Planet Formation as a Function of the Bulk Properties and Initial Sizes of Planetesimals
• Monte Carlo simulation of particle interactions at high dynamic range: Advancing beyond the Googol
• A new condition for the transition from runaway to oligarchic growth
• Formation and accretion history of terrestrial planets from runaway growth through to late time: implications for orbital eccentricity
• Accretion among preplanetary bodies: the many faces of runaway growth
• Migration of planets embedded in a circumstellar disk
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• Predicted Space Motions for Hypervelocity and Runaway Stars: Proper Motions and Radial Velocities for the GAIA Era
• Coagulation Calculations of Icy Planet Formation at 15--150 AU: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Transneptunian Objects
• The Formation of Pluto's Low Mass Satellites
• Runaway Stars, Hypervelocity Stars, and Radial Velocity Surveys
• The Fate of Scattered Planets
• Geochemical and planetary dynamical views on the origin of Earth's atmosphere and oceans
• Planetesimals in Debris Disks of Sun-like Stars
• From Disks to Planets
• Solving the Coagulation Equation by the Moments Method
• Formation of Super-Earth Mass Planets at 125-250 AU from a Solar-type Star
• From Pebbles and Planetesimals to Planets and Dust: the Protoplanetary Disk--Debris Disk Connection
• Variations on Debris Disks III. Collisional Cascades and Giant Impacts in the Terrestrial Zones of Solar-type Stars
• Terrestrial planet formation: Dynamical shake-up and the low mass of Mars
• Making Planet Nine: Pebble Accretion at 250--750 AU in a Gravitationally Unstable Ring
• Making Planet Nine: A Scattered Giant in the Outer Solar System
• Migration of small moons in Saturn's rings
• The Formation and Dynamics of Super-Earth Planets
• Rocky Planet Formation: Quick and Neat
• Super-Earths: A New Class of Planetary Bodies
• Impact of the Galactic Disk and Large Magellanic Cloud on the Trajectories of Hypervelocity Stars Ejected from the Galactic Center
• PENTACLE: Parallelized Particle-Particle Particle-Tree Code for Planet Formation
• A Pluto-Charon Sonata: The Dynamical Architecture of the Circumbinary Satellite System
• Coagulation Calculations of Icy Planet Formation Around 0.1--0.5~\msun\ Stars: Super-Earths From Large Planetestimals
• A Pluto--Charon Sonata: Dynamical Limits on the Masses of the Small Satellites
• A Pluto-Charon Concerto: An Impact on Charon as the Origin of the Small Satellites
• A particle-based hybrid code for planet formation
• Evolution of a ring around the Pluto-Charon binary
• On the Estimation of Circumbinary Orbital Properties
• A Pluto--Charon Concerto II. Formation of a Circumbinary Disk of Debris After the Giant Impact
• Magnetic interactions in orbital dynamics
• A Pluto-Charon Sonata III. Growth of Charon from a Circum-Pluto Ring of Debris
• Conglomeration of kilometre-sized planetesimals
• Collisional Cascade Caclulations for Irregular Satellite Swarms in Fomalhaut b
• Hybrid methods in planetesimal dynamics: Formation of protoplanetary systems and the mill condition
• A Pluto--Charon Sonata IV. Improved Constraints on the Dynamical Behavior and Masses of the Small Satellites
• Runaway Growth of Planetesimals Revisited: Presenting Criteria Required for Realistic Modeling of Planetesimal Growth