Dust, Chemistry & Radiation Transport in MRI-Turbulent Protoplanetary Discs

M. Flaig, W. Kley, R. Kissman and P. Ruoff
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M. Flaig: Universität Tübingen, Institut für Astronomie & Astrophysik
W. Kley: Universität Tübingen, Institut für Astronomie & Astrophysik
R. Kissman: Universität Innsbruck, Institut für Astro- und Teilchenphysik
P. Ruoff: Universität Tübingen, Institut für Astronomie & Astrophysik

A chapter in High Performance Computing in Science and Engineering '10, 2011, pp 103-116 from Springer

Abstract: Abstract It is our aim to set up 3D protoplanetary disc models that include all the physically relevant factors, namely magnetic fields, radiation transport, chemistry and dust, coupled to each other in a self-consistent manner. The present report describes results obtained from radiation magnetohydrodynamics simulations, where for the first time a detailed radiation transport scheme has been included into a 3D turbulent protoplanetary disc model. By virtue of the conservative properties of our numerical scheme, the heating of the disc gas is automatically consistent with the losses in kinetic and magnetic energy due to turbulent dissipation. Our models achieve a quasi-steady state of saturated turbulence, characterised by a Shakura-Syunyaev alpha of α∼0.02, where the turbulent heating is balanced by cooling due to radiation transport. By performing a suite of simulations with varying box sizes and resolutions, we are able to estimate to what extend the turbulent saturation level and the heating rates depend on these numerical parameters. For high enough resolution the simulations yield consistent results, indicate convergence.

Keywords: Accretion Disc; Magnetic Pressure; Radiation Transport; Monthly Notice; Angular Momentum Transport (search for similar items in EconPapers)
Date: 2011
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DOI: 10.1007/978-3-642-15748-6_8

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