2007/04/23 by G. Lesur, P-Y. Longaretti · 1 citation
Physics and Astronomy · #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.11888.x
published as Mon.Not.Roy.Astron.Soc.378:1471-1480,2007 · 11 pages, 11 figures, accepted to MNRAS
arxiv created 2007/04/23 · arxiv updated 2009/12/01
The magneto-rotational instability is presently the most promising source of turbulent transport in accretion disks. However, some important issues still need to be addressed to quantify the role of MRI in disks; in particular no systematic investigation of the role of the physical dimensionless parameters of the problem on the dimensionless transport has been undertaken yet. First, we complete existing investigations on the field strength dependence by showing that the transport in high magnetic pressure disks close to marginal stability is highly time-dependent and surprisingly efficient. Second, we bring to light a significant dependence of the global transport on the magnetic Prandtl number, with α∝ Pmδ for the explored range: 0.12<Pm<8 and 200<Re<6400 (δ being in the range 0.25 to 0.5). We show that the dimensionless transport is not correlated to the dimensionless linear growth rate, contrarily to a largely held expectation. More generally, these results stress the need to control dissipation processes in astrophysical simulations.