The Fate of Planetesimals in Turbulent Disks with Dead Zones. I. The Turbulent Stirring Recipe

Abstract

Turbulence in protoplanetary disks affects planet formation in many ways. While small dust particles are mainly affected by the aerodynamical coupling with turbulent gas velocity fields, planetesimals and larger bodies are more affected by gravitational interaction with gas density fluctuations. For the latter process, a number of numerical simulations have been performed in recent years, but a fully parameter-independent understanding has not been yet established. In this study, we present simple scaling relations for the planetesimal stirring rate in turbulence driven by magnetorotational instability (MRI), taking into account the stabilization of MRI due to Ohmic resistivity. We begin with order-of-magnitude estimates of the turbulence-induced gravitational force acting on solid bodies and associated diffusion coefficients for their orbital elements. We then test the predicted scaling relations using the results of recent Ohmic-resistive MHD simulations by Gressel et al. We find that these relations successfully explain the simulation results if we properly fix order-of-unity uncertainties within the estimates. We also update the saturation predictor for the density fluctuation amplitude in MRI-driven turbulence originally proposed by Okuzumi & Hirose. Combination of the scaling relations and saturation predictor allows to know how the turbulent stirring rate of planetesimals depends on disk parameters such as the gas column density, distance from the central star, vertical resistivity distribution, and net vertical magnetic flux. In Paper II, we apply our recipe to planetesimal accretion to discuss its viability in turbulent disks.

14 pages, 10 figures, accepted for publication in ApJ

References in corpus (15)

• Wind-driven Accretion in Protoplanetary Disks. I: Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind
• Closed-form expressions for particle relative velocities induced by turbulence
• Dust settling in local simulations of turbulent protoplanetary disks
• Dead Zone Accretion Flows in Protostellar Disks
• Advection of Magnetic Fields in Accretion Disks: Not So Difficult After All
• Magnetized Accretion and Dead Zones in Protostellar Disks
• Accretion and destruction of planetesimals in turbulent disks
• Accretion of Terrestrial Planets from Oligarchs in a Turbulent Disk
• Turbulent Torques on Protoplanets in a Dead Zone
• Diffusive Migration of Low-Mass Proto-planets in Turbulent Disks
• On the evolution of mean motion resonances through stochastic forcing: Fast and slow libration modes and the origin of HD128311
• Turbulent diffusion in protoplanetary discs: the effect of an imposed magnetic field
• On the dynamics of planetesimals embedded in turbulent protoplanetary discs with dead zones
• Dead, Undead and Zombie Zones in Protostellar Disks as a Function of Stellar Mass
• A coagulation-fragmentation model for the turbulent growth and destruction of preplanetesimals

Cited by in corpus (32)

• Make Super-Earths, Not Jupiters: Accreting Nebular Gas onto Solid Cores at 0.1 AU and Beyond
• The New Generation Planetary Population Synthesis (NGPPS). I. Bern global model of planet formation and evolution, model tests, and emerging planetary systems
• Formation of TRAPPIST-1 and other compact systems
• The Impact of Dust Evolution and Photoevaporation on Disk Dispersal
• MHD Simulations of Global Accretion Disks with Vertical Magnetic Fields
• Diffusion and Concentration of Solids in the Dead Zone of a Protoplanetary Disk
• Pebble Accretion and the Diversity of Planetary Systems
• On the Viability of the Magnetorotational Instability in Circumplanetary Disks
• Growth after the streaming instability: from planetesimal accretion to pebble accretion
• Radial Transport of Large-Scale Magnetic Fields in Accretion Disks. I. Steady Solutions and an Upper Limit on the Vertical Field Strength
• An Analytic Criterion for Turbulent Disruption of Planetary Resonances
• From Planetesimals to Planets in Turbulent Protoplanetary Disks I. Onset of Runaway Growth
• Dynamics and Formation of the Near-Resonant K2-24 System: Insights from Transit-Timing Variations and Radial Velocities
• Making Planet Nine: Pebble Accretion at 250--750 AU in a Gravitationally Unstable Ring
• TOI-216: Resonant Constraints on Planet Migration
• Dust dynamics in 2D gravito-turbulent disks
• Circumbinary Planet Formation in the Kepler-16 System. II. A Toy Model for In-situ Planet Formation within a Debris Belt
• Orbital Evolution of Moons in Weakly Accreting Circumplanetary Disks
• From Planetesimal to Planet in Turbulent Disks. II. Formation of Gas Giant Planets
• Trapping of Low-Mass Planets Outside the Truncated Inner Edges of Protoplanetary Discs
• The Kepler-223 resonance holds information on turbulence during the gas disk phase
• Magneto-rotational instability in the protolunar disk
• Turbulence, Transport and Waves in Ohmic Dead Zones
• Growth of Magnetorotational Instability in Circumstellar Disks around Class 0 Protostars
• Magnetorotational instability in decretion disks of critically rotating stars and the outer structure of Be and Be/X-ray disks
• Planetesimal Formation by Gravitational Instability of a Porous-Dust Disk
• Dynamics of Porous Dust Aggregates and Gravitational Instability of Their Disk
• Resonance Capture and Stability Analysis for Planet Pairs under Type I Disk Migration
• Ejection of Chondrules from Fluffy Matrices
• Evolution of circumbinary protoplanetary disks with photoevaporative winds driven by External Far Ultraviolet Radiation
• Transition region from turbulent to dead zone in protoplanetary disks: local shearing box simulations
• Gravitational instability of a dust layer composed of porous silicate dust aggregates in a protoplanetary disk