Dynamics and Accretion of Planetesimals

Abstract

We review the basic dynamics and accretion of planetesimals by showing N-body simulations. The orbits of planetesimals evolve through two-body gravitational relaxation: viscous stirring increases the random velocity and dynamical friction realizes the equiparation of the random energy. In the early stage of planetesimal accretion the growth mode of planetesimals is runaway growth where larger planetesimals grow faster than smaller ones. When a protoplanet (runaway-growing planetesimal) exceeds a critical mass the growth mode shifts to oligarchic growth where similar-sized protoplanets grow keeping a certain orbital separation. The final stage of terrestrial planet formation is collision among protoplanets known as giant impacts. We also summarize the dynamical effects of disk gas on planets and the core accretion model for formation of gas giants and discuss the diversity of planetary systems.

References in corpus (9)

• Forming Planetesimals in Solar and Extrasolar Nebulae
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Constraints on the mass of a habitable planet with water of nebular origin
• Merging Criteria for Giant Impacts of Protoplanets
• Formation of Terrestrial Planets from Protoplanets under a Realistic Accretion Condition
• On the Observability of Giant Protoplanets in Circumstellar Disks
• Infall of planetesimals onto growing giant planets: onset of runaway gas accretion and metallicity of their gas envelopes
• Migration rates of planets due to scattering of planetesimals
• Transition disk chemistry and future prospects with ALMA

Cited by in corpus (24)

• Magnetospheric Truncation, Tidal Inspiral, and the Creation of Short and Ultra-Short Period Planets
• Kuiper Belt-Like Hot and Cold Populations of Planetesimal Inclinations in the $\beta$ Pictoris Belt Revealed by ALMA
• Planetary population synthesis
• Requirements for gravitational collapse in planetesimal formation --- the impact of scales set by Kelvin-Helmholtz and nonlinear streaming instability
• Heavy-metal Jupiters by major mergers: metallicity vs. mass for giant planets
• Stochasticity & Predictability in Terrestrial Planet Formation
• Linking planetesimal and dust content in protoplanetary disks via a local toy model
• A Self-Consistent Model for Dust-Gas Coupling in Protoplanetary Disks
• High Resolution Study of Planetesimal Formation by Gravitational Collapse of Pebble Clouds
• Can Large-Scale Migration Explain the Giant Planet Occurrence Rate?
• Planetary core formation via multi-species pebble accretion
• The vertical structure of debris discs and the role of disc gravity: A primer using a simplified model
• United Theory of Planet Formation (I): Tandem Regime
• Chemistry Along Accretion Streams in a Viscously-Evolving Protoplanetary Disk
• Composition constraints of the TRAPPIST-1 planets from their formation
• Formation of inner planets in the presence of a Cold Jupiter: orbital evolution and relative velocities of planetesimals
• Planetesimal Dynamics in the Presence of a Giant Planet
• Orbital structure of planetary systems formed by giant impacts: stellar mass dependence
• Planetesimal Dynamics in the Presence of a Giant Planet II: Dependence on Planet Mass and Eccentricity
• A Bayesian neural network predicts the dissolution of compact planetary systems
• On planet formation around supermassive black holes and the grain disruption barriers by radiative torques
• Interaction of infalling solid bodies with primordial atmospheres of disk-embedded planets
• Runaway Growth of Planetesimals Revisited: Presenting Criteria Required for Realistic Modeling of Planetesimal Growth
• Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations