Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 420, Issue 3, Pages 2419-2428Publisher
WILEY-BLACKWELL
DOI: 10.1111/j.1365-2966.2011.20207.x
Keywords
accretion, accretion discs; magnetic fields; MHD; radiative transfer; turbulence; protoplanetary discs
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Funding
- Deutsche Forschungsgemeinschaft DFG [DFG Forschergruppe 759]
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The aim of this paper is to investigate the spatial structure of a protoplanetary disc whose dynamics is governed by magnetorotational turbulence. We perform a series of local three-dimensional chemoradiative magnetohydrodynamic simulations located at different radii of a disc which is twice as massive as the standard minimum mass solar nebula of Hayashi. The ionization state of the disc is calculated by including collisional ionization, stellar X-rays, cosmic rays and the decay of radionuclides as ionization sources, and by solving a simplified chemical network which includes the effect of the absorption of free charges by mu m-sized dust grains. In the region where the ionization is too low to ensure good coupling between matter and magnetic fields, a non-turbulent central dead zone forms, which ranges approximately from a distance of 2 to 4 au from the central star. The approach taken in this work allows for the first time to derive the global spatial structure of a protoplanetary disc from a set of physically realistic numerical simulations.
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