Revisiting linear dynamics of non-axisymmetric perturbations in weakly magnetized accretion discs

• Published in: Monthly notices of the Royal Astronomical Society Vol. 435; no. 3; pp. 2552 - 2567
• Main Authors: Mamatsashvili, G. R., Chagelishvili, G. D., Bodo, G., Rossi, P.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 01-11-2013
• Subjects: Approximation; Comparative analysis; Fluid mechanics; Magnetic fields; Ordinary differential equations; Simulation; MHD; protoplanetary discs; planetary systems; turbulence; accretion, accretion discs; instabilities
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stt1470

We investigate the linear dynamics of non-axisymmetric perturbations in incompressible, vertically stratified Keplerian discs threaded by a weak non-zero net vertical magnetic field in the local shearing box approximation. Perturbations are decomposed into shearing waves or spatial harmonics whose temporal evolution is then followed via numerical integration of the linearized ideal magnetohydrodynamic equations of the shearing box. There are two basic modes in the system - inertia-gravity waves and magnetic mode, which displays the magnetorotational instability (MRI). Distinct from previous related studies, we introduce 'eigen-variables' characterizing each (counter-propagating) component of the inertia-gravity and magnetic modes, which are governed by a set of four first-order coupled ordinary differential equations. This allows us to identify a new process of linear coupling of the two above non-axisymmetric modes due to the disc's differential rotation. We also carry out a comparative analysis of the dynamics of non-axisymmetric and axisymmetric magnetic mode perturbations. It is demonstrated that the growth of 'optimal' and close-to-optimal non-axisymmetric harmonics of this mode, having transient nature, can prevail over the exponential growth of axisymmetric ones (i.e. over the axisymmetric MRI) during dynamical time. A possible implication of this result for axisymmetric channel solutions emerging in numerical simulations is discussed. In particular, the formation of the (axisymmetric) channel may be affected/impeded by non-axisymmetric modes already at the early linear stage leading to its untimely disruption - the outcome strongly depends on the amplitude and spectrum of initial perturbation. Thus, this competition may result in an uncertainty in the magnetic mode's non-linear dynamics. Even so, we consider that incompressible perturbations, in the final part, speculate on the dynamics in the compressible case. It is shown that a maximum growth of non-axisymmetric magnetic mode occurs at vertical wavelengths close to the disc scaleheight, for which compressibility effects are important. This indirectly suggests that compressibility plays a role in the dynamics of the non-axisymmetric MRI and, ultimately, in the resulting turbulent state.