Existence of the Magnetorotational Instability

By posing and solving a global axisymmetric eigenvalue problem on an infinite domain with modes vanishing at zero and infinity for a differentially rotatingMHD plasma, the conditions for the occurrence of a purely growing lowfrequency 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 theMRI is rather nuanced. It is dictated by the details of the radial profile of the rotation velocity (r) and not just by the sign and the magnitude of its gradient, 0. 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. Subject headinggs: accretion, accretion disks — MHD