Turbulent resistivity characterization in accretion disc MRI turbulence.

Details Turbulent resistivity characterization in accretion disc MRI turbulence. Turbulent resistivity characterization in accretion disc MRI turbulence.

Nov 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008sf2a.conf..491l&link_type=abstract

"SF2A-2008: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: C. Charbonnel, F. Combes

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The magneto-rotational instability (MRI) is widely recognized as the most promising process to provide a turbulent transport satisfying the observational constraints. Although nearly all disk models make reference to this instability as the source of turbulence, important aspects of the MRI-driven turbulent transport properties are not well-known, in particular concerning the "resistive" transport. We have performed local simulations of the MRI to quantify this problem. We find that the resistive transport is systematically smaller than the angular momentum transport for a given configuration, and that the resistivity tensor is anisotropic.

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