Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds

Abstract

Aims: We investigate the evolution of protoplanetary discs (PPDs hereafter) with magnetically driven disc winds and viscous heating. Methods: We consider an initially massive disc with ~0.1 Msun to track the evolution from the early stage of PPDs. We solve the time evolution of surface density and temperature by taking into account viscous heating and the loss of the mass and the angular momentum by the disc winds within the framework of a standard alpha model for accretion discs. Our model parameters, turbulent viscosity, disc wind mass loss, and disc wind torque, which are adopted from local magnetohydrodynamical simulations and constrained by the global energetics of the gravitational accretion, largely depends on the physical condition of PPDs, particularly on the evolution of the vertical magnetic flux in weakly ionized PPDs. Results: Although there are still uncertainties concerning the evolution of the vertical magnetic flux remaining, surface densities show a large variety, depending on the combination of these three parameters, some of which are very different from the surface density expected from the standard accretion. When a PPD is in a "wind-driven accretion" state with the preserved vertical magnetic field, the radial dependence of the surface density can be positive in the inner region <1-10 au. The mass accretion rates are consistent with observations, even in the very low level of magnetohydrodynamical turbulence. Such a positive radial slope of the surface density gives a great impact on planet formation because (i)it inhibits the inward drift or even results in the outward drift of pebble/boulder-sized solid bodies, and (ii) it also makes the inward type-I migration of proto-planets slower or even reversed. Conclusions: The variety of our calculated PPDs should yield a wide variety of exoplanet systems.

16 pages, 11 figures embedded, accepted by A&A (comments are welcome)

References in corpus (16)

• Photoevaporation of protoplanetary discs II: evolutionary models and observable properties
• Which jet launching mechanism(s) in TTauri stars?
• Global simulations of protoplanetary disks with ohmic resistivity and ambipolar diffusion
• The structure of protoplanetary discs around evolving young stars
• Analytical protostellar disk models 1: the effect of internal dissipation and surface irradiation on the structure of disks and the location of the snow line around Sun-like stars
• Impact of dimensionless numbers on the efficiency of MRI-induced turbulent transport
• A Spitzer view of protoplanetary disks in the gamma Velorum cluster
• X-ray irradiated protoplanetary disk atmospheres I: Predicted emission line spectrum and photoevaporation
• Dead Zone Accretion Flows in Protostellar Disks
• Advection of Magnetic Fields in Accretion Disks: Not So Difficult After All
• The signature of the magnetorotational instability in the Reynolds and Maxwell stress tensors in accretion discs
• Global evolution of the magnetic field in a thin disc and its consequences for protoplanetary systems
• Time evolution of snow regions and planet traps in an evolving protoplanetary disk
• Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system's terrestrial planets
• Asymmetric MHD Outflows/Jets from Accreting T Tauri Stars
• Disk Dissipation Timescale of Pre-main Sequence Stars in Taurus

Cited by in corpus (48)

• On the diversity and statistical properties of protostellar discs
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• Challenges in Planet Formation
• Mass inventory of the giant-planet formation zone in a solar nebula analog
• Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion and disc evolution
• Global Hydromagnetic Simulations of Protoplanetary Disks with Stellar Irradiation and Simplified Thermochemistry
• Global Three-Dimensional Simulations of Outer Protoplanetary Disks with Ambipolar Diffusion
• Nonsticky Ice at the Origin of the Uniformly Polarized Submillimeter Emission from the HL Tau Disk
• Predicted diversity in water content of terrestrial exoplanets orbiting M dwarfs
• On the secular evolution of the ratio between gas and dust radii in protoplanetary discs
• Rings and gaps produced by variable magnetic disk winds and avalanche accretion streams: I. Axisymmetric resistive MHD simulations
• Effect of wind-driven accretion on planetary migration
• Photoevaporative Dispersal of Protoplanetary Disks around Evolving Intermediate-mass Stars
• Magnetically Induced Disk Winds and Transport in the HL Tau Disk
• Large gaps and high accretion rates in photoevaporative transition disks with a dead zone
• Radiation hydrodynamics simulations of protoplanetary disks: Stellar mass dependence of the disk photoevaporation rate
• Evolution of the Water Snow Line in Magnetically Accreting Protoplanetary Disks
• MRI-active inner regions of protoplanetary discs. I. A detailed model of disc structure
• Setting the Stage: Planet formation and Volatile Delivery
• Accretion bursts in magnetized gas-dust protoplanetary disks
• Do the TRAPPIST-1 Planets Have Hydrogen-rich Atmospheres?
• Are the observed gaps in protoplanetary discs caused by growing planets?
• Paleomagnetic evidence for a disk substructure in the early solar system
• Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites
• Formation of giant planets with large metal masses and metal fractions via giant impacts in a rapidly dissipating disk
• [OI] 6300Å emission as a probe of external photoevaporation of protoplanetary discs
• Close-in Super-Earths: The first and the last stages of planet formation in an MRI-accreting disc
• Unified simulations of planetary formation and atmospheric evolution II: Rapid disk clearing by photoevaporation yields low-mass super-Earth atmospheres
• Determining dispersal mechanisms of protoplanetary disks using accretion and wind mass loss rates
• Extreme evaporation of planets in hot thermally unstable protoplanetary discs: the case of FU Ori
• Planetesimal formation around the snow line: I. Monte Carlo simulations of silicate dust pile-up in a turbulent disk
• Episodic accretion and mergers during growth of massive protostars
• Primordial Dusty Rings and Episodic Outbursts in Protoplanetary Discs
• Effects of global gas flows on type I migration
• Distinguishing Magnetized Disc Winds from Turbulent Viscosity through Substructure Morphology in Planet-forming Discs
• Combined Effects of Disk Winds and Turbulence-Driven Accretion on Planet Populations
• Effect of Different Angular Momentum Transport mechanisms on the Distribution of Water in Protoplanetary Disks
• Formation of Planetary Populations III: Core Composition & Atmospheric Evaporation
• Rapid-then-slow migration reproduces mass distribution of TRAPPIST-1 system
• Dynamics of Dusty Vortices II: Stability of 2D dust laden vortices
• Effective dust growth in laminar circumplanetary discs with magnetic wind-driven accretion
• Using planet migration and dust drift to weigh protoplanetary discs
• Structure of Protoplanetary Discs with Magnetically-driven Winds
• The evolution of a circumplanetary disc with a dead zone
• On the crystallinity of silicate dust in evolving protoplanetary disks due to magnetically driven disk winds
• Protoplanetary disk formation from the collapse of a prestellar core
• Early Initiation of Inner Solar System Formation at Dead-Zone Inner Edge