Nonaxisymmetric MHD instabilities of Chandrasekhar states in Taylor-Couette geometry

TL;DR

This study investigates nonaxisymmetric magnetohydrodynamic instabilities in Chandrasekhar states within Taylor-Couette flow, analyzing linear and nonlinear behaviors across different profiles and their implications for astrophysical phenomena.

Contribution

It provides a comprehensive analysis of nonaxisymmetric MHD instabilities in Chandrasekhar states, including linear stability and nonlinear energy spectra, highlighting differences based on azimuthal mode numbers and flow profiles.

Findings

Modes with m>10 can become unstable at high magnetic Reynolds numbers.

Energy spectra become steeper for large azimuthal mode numbers.

Magnetic energy exceeds kinetic energy for Rm>100.

Abstract

We consider axially periodic Taylor-Couette geometry with insulating boundary conditions. The imposed basic states are so-called Chandrasekhar states, where the azimuthal flow $U_\phi$ and magnetic field $B_\phi$ have the same radial profiles. Mainly three particular profiles are considered: the Rayleigh limit, quasi-Keplerian, and solid-body rotation. In each case we begin by computing linear instability curves and their dependence on the magnetic Prandtl number Pm. For the azimuthal wavenumber m=1 modes, the instability curves always scale with the Reynolds number and the Hartmann number. For sufficiently small Pm these modes therefore only become unstable for magnetic Mach numbers less than unity, and are thus not relevant for most astrophysical applications. However, modes with m>10 can behave very differently. For sufficiently flat profiles, they scale with the magnetic Reynolds number and the Lundquist number, thereby allowing instability also for the large magnetic Mach numbers of astrophysical objects. We further compute fully nonlinear, three-dimensional equilibration of these instabilities, and investigate how the energy is distributed among the azimuthal (m) and axial (k) wavenumbers. In comparison spectra become steeper for large m, reflecting the smoothing action of shear. On the other hand kinetic and magnetic energy spectra exhibit similar behavior: if several azimuthal modes are already linearly unstable they are relatively flat, but for the rigidly rotating case where m=1 is the only unstable mode they are so steep that neither Kolmogorov nor Iroshnikov-Kraichnan spectra fit the results. The total magnetic energy exceeds the kinetic energy only for large magnetic Reynolds numbers Rm>100.