Modeling the Magnetorotational Instability in Nearly Inviscid Systems

Details Modeling the Magnetorotational Instability in Nearly Inviscid Systems Modeling the Magnetorotational Instability in Nearly Inviscid Systems

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aps..dppjp1058t&link_type=abstract

American Physical Society, 46th Annual Meeting of the Division of Plasma Physics, 15-19 November, 2004, Savannah, GA. MEETING I

Physics

Plasma Physics

Scientific paper

A question of considerable interest in the astrophysical community involves the mechanism of angular momentum transport through accretion disks. Accretion disks, like many astrophysical flows, are nearly inviscid. It is uncertain if purely hydrodynamic turbulence could cause the dissipation required for gas to flow inward toward the central object. However, when the gas is warm enough to become partially ionized, accretion disks become magnetohydrodynamic fluids. When threaded by a weak magnetic field, these rotating fluids can show signs of the magnetorotational instability (MRI), a promising candidate for the main mechanism for angular momentum transport in accretion disks. Basic characteristics of MRI are presented, as well as evidence that the MRI has been observed in the laboratory. Simulation results, which demonstrate key MRI features, are also presented.

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