Existence of the Magnetorotational Instability

Details Existence of the Magnetorotational Instability Existence of the Magnetorotational Instability

Jul 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008apj...682..602m&link_type=abstract

The Astrophysical Journal, Volume 682, Issue 1, pp. 602-607.

Astronomy and Astrophysics

Astronomy

3

Accretion, Accretion Disks, Magnetohydrodynamics: Mhd

Scientific paper

By posing and solving a global axisymmetric eigenvalue problem on an infinite domain with modes vanishing at zero and infinity for a differentially rotating MHD plasma, the conditions for the occurrence of a purely growing low-frequency mode known as the magnetorotational instability (MRI) are mapped. It is shown that the MRI criterion drawn from the ``local dispersion relation'' is at best inadequate and may even be misleading. The physics of the MRI is rather nuanced. It is dictated by the details of the radial profile of the rotation velocity Ω(r) and not just by the sign and the magnitude of its gradient, Ω'. The salient features of the class of profiles for which the MRI-like eigenmodes may occur are given along with the eigenspectrum. For a variety of other profiles, it is shown that an unstable magnetorotational mode is not a valid eigensolution.

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