Effects of Type I Migration on Terrestrial Planet Formation

Abstract

Planetary embryos embedded in a gas disc suffer a decay in semimajor axis -- type I migration -- due to the asymmetric torques produced by the interior and exterior wakes raised by the body (Goldreich & Tremaine 1980; Ward 1986). This presents a challenge for standard oligarchic approaches to forming the terrestrial planets (Kokubo & Ida 1998) as the timescale to grow the progenitor objects near 1 AU is longer than that for them to decay into the Sun. In this paper we investigate the middle and late stages of oligarchic growth using both semi-analytic methods (based upon Thommes et al. 2003) and N-body integrations, and vary gas properties such as dissipation timescale in different models of the protoplanetary disc. We conclude that even for near-nominal migration efficiencies and gas dissipation timescales of ~1 Myr it is possible to maintain sufficient mass in the terrestrial region to form Earth and Venus if the disc mass is enhanced by factors of ~2-4 over the minimum mass model. The resulting configurations differ in several ways from the initial conditions used in previous simulations of the final stages of terrestrial accretion (e.g. Chambers 2001), chiefly in (1) larger inter-embryo spacings, (2) larger embryo masses, and (3) up to ~0.4 Earth masses of material left in the form of planetesimals when the gas vanishes. The systems we produce are reasonably stable for ~100 Myr and therefore require an external source to stir up the embryos sufficiently to produce final systems resembling the terrestrial planets.

arXiv comment49 pages, 22 figures; accepted in AJ, expected Dec '05

References in corpus (12)

• Disk Frequencies and Lifetimes in Young Clusters
• Making other Earths: Dynamical Simulations of Terrestrial Planet Formation and Water Delivery
• Runaway migration and the formation of hot Jupiters
• On the orbital evolution and growth of protoplanets embedded in a gaseous disc
• Planet Formation by Coagulation: A Focus on Uranus and Neptune
• Oligarchic growth of giant planets
• Fast accretion of small planetesimals by protoplanetary cores
• Type I Planetary Migration with MHD Turbulence
• Low-Mass Proto-Planet Migration in T-Tauri Alpha-Disks
• A Primordial Origin of the Laplace Relation Among the Galilean Satellites
• Eccentricity Evolution of Extrasolar Multiple Planetary Systems due to the Depletion of Nascent Protostellar Disks
• Halting planet migration by photoevaporation from the central source

Cited by in corpus (36)

• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs
• Toward a Deterministic Model of Planetary Formation V. Accumulation Near the Ice Line
• Migration and the formation of systems of hot super-Earths and Neptunes
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
• Toward a Deterministic Model of Planetary Formation VI: Dynamical Interaction and Coagulation of Multiple Rocky Embryos and Super-Earth Systems around Solar Type Stars
• Toward a Deterministic Model of Planetary Formation VII: Eccentricity Distribution of Gas Giants
• On the formation of planetary systems via oligarchic growth in thermally evolving viscous discs
• N-body simulations of planetary accretion around M dwarf stars
• Modeling the Formation of Giant Planet Cores I: Evaluating Key Processes
• Formation of TRAPPIST-1 and other compact systems
• From planetesimals to terrestrial planets: N-body simulations including the effects of nebular gas and giant planets
• Formation of Earth-like Planets During and After Giant Planet Migration
• The potential for Earth-mass planet formation around brown dwarfs
• Accretion of Terrestrial Planets from Oligarchs in a Turbulent Disk
• On the formation of hot Neptunes and super-Earths
• Condition for Capture into First-order Mean Motion Resonances and Application to Constraints on Origin of Resonant Systems
• The Effect of an Early Planetesimal-Driven Migration of the Giant Planets on Terrestrial Planet Formation
• Building Giant-Planet Cores at a Planet Trap
• TOI-1136 is a Young, Coplanar, Aligned Planetary System in a Pristine Resonant Chain
• Global models of planetary system formation in radiatively-inefficient protoplanetary discs
• The effect of type I migration on the formation of terrestrial planets in hot-Jupiter systems
• The Formation of Uranus and Neptune in Solid-Rich Feeding Zones: Connecting Chemistry and Dynamics
• Terrestrial Planet Formation During the Migration and Resonance Crossings of the Giant Planets
• Bayesian Inference on the Isotopic Building Blocks of Mars and Earth
• New methods for large dynamical range problems in planetary formation
• Terrestrial planet formation in low eccentricity warm-Jupiter systems
• Theoretical models of planetary system formation. II. Post-formation evolution
• Probing the impact of varied migration and gas accretion rates for the formation of giant planets in the pebble accretion scenario
• Realistic collisional water transport during terrestrial planet formation: Self-consistent modeling by an N-body--SPH hybrid code
• On the dynamics of resonant super-Earths in disks with turbulence driven by stochastic forcing
• TRAPPIST-1: Dynamical analysis of the transit-timing variations and origin of the resonant chain
• Collisional Fragmentation is Not a Barrier to Close-in Planet Formation
• Overcoming migration during giant planet formation
• Residual Neural Networks for the Prediction of Planetary Collision Outcomes
• Terrestrial Planet Formation in Extra-Solar Planetary Systems
• HydroSyMBA: a 1D hydrocode coupled with an N-body symplectic integrator