Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2011-11-23
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
11 pages, 12 figures, MNRAS accepted
Scientific paper
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 {\mu}m-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.
Flaig Markus
Kissmann Ralf
Kley Willy
Ruoff P.
No associations
LandOfFree
Global Structure of Magnetorotationally Turbulent Protoplanetary Discs does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Global Structure of Magnetorotationally Turbulent Protoplanetary Discs, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Global Structure of Magnetorotationally Turbulent Protoplanetary Discs will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-377263