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Global structure of magnetorotationally turbulent protoplanetary discs
被引:21
|作者:
Flaig, M.
[1
]
Ruoff, Patrick
[2
]
Kley, W.
[1
]
Kissmann, R.
[3
]
机构:
[1] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
[2] Inst Anthropomat, Karlsruhe Inst Technol, D-76131 Karlsruhe, Germany
[3] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria
关键词:
accretion;
accretion discs;
magnetic fields;
MHD;
radiative transfer;
turbulence;
protoplanetary discs;
3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS;
STRATIFIED ACCRETION DISKS;
T TAURI DISKS;
MHD SIMULATIONS;
IONIZATION FRACTION;
PROTOSTELLAR DISKS;
VERTICAL STRUCTURE;
SOLAR NEBULA;
INSTABILITY;
DIFFUSION;
D O I:
10.1111/j.1365-2966.2011.20207.x
中图分类号:
P1 [天文学];
学科分类号:
0704 ;
摘要:
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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页码:2419 / 2428
页数:10
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