Adapting a solid accretion scenario for migrating planets in FARGO3D

Abstract

In this work, we adapt a module for planetary formation within the hydrodynamic code FARGO3D. Planetary formation is modeled by a solid core accretion scenario, with the core growing in oligarchic regime. The initial superficial density of planetesimals is proportional to the initial superficial density of gas in the disc. We include a numerical approach to describe the evolution of the eccentricity and the inclination of planetesimals during the formation. This approach impacts directly on the accretion rate of solids. When the core reaches a critical mass, gas accretion begins, following the original FARGO scheme adapted to the FARGO3D code. To exemplify how the module for planetary formation can be used, we investigate the migration of a planet in a two-dimensional, locally isothermal gas disc with a prescribed accretion rate, analyzing the timescale involved in the planetary migration process along with the timescale for planetary formation. The analysis reveals that the mass of the nucleus must be close to its critical value when crossing the ice line to avoid the planet's fall into the stellar envelope. This will allow enough time for the planet to initiate runaway gas accretion, leading to a rapid mass increase and entering type II planetary migration.

References in corpus (43)

• Towards a Deterministic Model of Planetary Formation I: a Desert in the Mass and Semi Major Axis Distributions of Extra Solar Planets
• Planet-disk interaction and orbital evolution
• Models of Giant Planet formation with migration and disc evolution
• FARGO: a fast eulerian transport algorithm for differentially rotating disks
• The formation and retention of gas giant planets around stars with a range of metallicities
• A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion
• On the Luminosity of Young Jupiters
• The PLUTO Code for Adaptive Mesh Computations in Astrophysical Fluid Dynamics
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Radial Flow of Dust Particles in Accretion Disks
• A torque formula for non-isothermal Type I planetary migration - I. Unsaturated horseshoe drag
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Mass Flow and Accretion through gaps in Accretion Discs
• A Review of Bondi--Hoyle--Lyttleton Accretion
• The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-Gravity
• Oligarchic growth of giant planets
• FARGO3D: A new GPU-oriented MHD code
• Fast accretion of small planetesimals by protoplanetary cores
• The thermal structure and the location of the snow line in the protosolar nebula: axisymmetric models with full 3-D radiative transfer
• Planet heating prevents inward migration of planetary cores
• Migration of massive planets in accreting disks
• Orbital evolution of eccentric planets in radiative discs
• On the Evolution of the Snow Line in Protoplanetary Discs
• Planet formation models: the interplay with the planetesimal disc
• Impacts of planet migration models on planetary populations. Effects of saturation, cooling and stellar irradiation
• Three-dimensional Disk-Planet Torques in a Locally Isothermal Disk
• Critical core mass for enriched envelopes: the role of H2O condensation
• The opacity of grains in protoplanetary atmospheres
• Planet-Disc Interactions and Early Evolution of Planetary Systems
• Understanding how planets become massive. I. Description and validation of a new toy model
• The dynamical role of the circumplanetary disc in planetary migration
• Thermodynamics of Giant Planet Formation: Shocking Hot Surfaces on Circumplanetary Disks
• On the evolution of the snow line in protoplanetary discs II: Analytic approximations
• The accretion of migrating giant planets
• Numerical simulations of the type III migration:I. Disc model and convergence tests
• Formation of solar system analogs I: looking for initial conditions through a population synthesis analysis
• Consequences of the simultaneous formation of giant planets by the core accretion mechanism
• Recent developments in planet migration theory
• Type III migration in a low viscosity disc
• Protoplanetary disks including radiative feedback from accreting planets
• The effect of planetary migration on the corotation resonance
• Theory of planet formation
• Adapting a gas accretion scenario for migrating planets in FARGO3D