Global Structure of Magnetorotationally Turbulent Protoplanetary Discs

Abstract

The aim of the present paper is to investigate the spatial structure of a protoplanetary disc whose dynamics is governed by magnetorotational turbulence. We perform a series of local 3D chemo-radiative MHD simulations located at different radii of a disc which is twice as massive as the standard minimum mass solar nebula of Hayashi (1981). The ionisation state of the disc is calculated by including collisional ionisation, stellar X-rays, cosmic rays and the decay of radionuclides as ionisation sources, and by solving a simplified chemical network which includes the effect of the absorption of free charges by μm-sized dust grains. In the region where the ionisation is too low to assure good coupling between matter and magnetic fields, a non-turbulent central "dead zone" forms, which ranges approximately from a distance of 2 AU to 4 AU from the central star. The approach taken in the present work allows for the first time to derive the global spatial structure of a protoplanetary disc from a set of physically realistic numerical simulations.

11 pages, 12 figures, MNRAS accepted

References in corpus (9)

• Accretion disc viscosity: how big is alpha?
• Dynamics of Protoplanetary Disks
• Effect of Ambipolar Diffusion on the Non-linear Evolution of Magnetorotational Instability in Weakly Ionized Disks
• Dust settling in local simulations of turbulent protoplanetary disks
• Dead Zone Accretion Flows in Protostellar Disks
• Global MHD simulations of stratified and turbulent protoplanetary discs. I. Model properties
• Turbulence and Steady Flows in 3D Global Stratified MHD Simulations of Accretion Disks
• Global MHD simulations of stratified and turbulent protoplanetary discs. II. Dust settling
• Heating and Cooling Protostellar Disks

Cited by in corpus (20)

• Planet-disk interaction and orbital evolution
• Wind-driven Accretion in Protoplanetary Disks. I: Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind
• Stellar irradiated discs and implications on migration of embedded planets I: equilibrium discs
• Local outflows from turbulent accretion disks
• Vertical shear instability in accretion disc models with radiation transport
• Magnetized Accretion and Dead Zones in Protostellar Disks
• Stellar irradiated discs and implications on migration of embedded planets II: accreting-discs
• Particle dynamics in discs with turbulence generated by the vertical shear instability
• Forming spectroscopic massive proto-binaries by disk fragmentation
• Planet Formation in Circumbinary Configurations: Turbulence Inhibits Planetesimal Accretion
• Bouncing Behavior of Microscopic Dust Aggregates
• Accretion in giant planet circumplanetary disks
• The reliability of approximate radiation transport methods for irradiated disk studies
• Testing large-scale vortex formation against viscous layers in three-dimensional discs
• The CRONOS Code for Astrophysical Magnetohydrodynamics
• Magnetorotational turbulence in stratified shearing boxes with perfect gas equation of state and finite thermal diffusivity
• Protostellar Disk Evolution Over Million-Year Timescales with a Prescription for Magnetized Turbulence
• MRI-driven angular momentum transport in protoplanetary disks
• On the importance of wave planet interactions for the migration of two super-Earths embedded in a protoplanetary disk
• A Self-Consistent Reduced Model for Dusty Magnetorotationally Unstable Discs