On the linear theory of Kelvin-Helmholtz instabilities of relativistic magnetohydrodynamic planar flows

Details On the linear theory of Kelvin-Helmholtz instabilities of relativistic magnetohydrodynamic planar flows On the linear theory of Kelvin-Helmholtz instabilities of relativistic magnetohydrodynamic planar flows

2008-02-19

arxiv.org/abs/0802.2607v3

Astronomy and Astrophysics

Astrophysics

8 pages, 9 figures

Scientific paper

10.1051/0004-6361:200809605

We investigate the linear stability properties of the plane interface separating two relativistic magnetized flows in relative motion. The two flows are governed by the (special) relativistic equations for a magnetized perfect gas in the infinite conductivity approximation. By adopting the vortex-sheet approximation, the relativistic magnetohydrodynamics equations are linearized around the equilibrium state and the corresponding dispersion relation is derived and discussed. The behavior of the configuration and the regimes of instability are investigated following the effects of four physical parameters, namely: the flow velocity, the relativistic and Alfv\'enic Mach numbers and the inclination of the wave vector on the plane of the interface. From the numerical solution of the dispersion relation, we find in general two separate regions of instability, associated respectively with the slow and fast magnetosonic modes. Modes parallel to the flow velocity are destabilized only for sufficiently low magnetization. For the latter case, stabilization is attained, additionally, at sufficiently large relativistic velocities between the two flows in relative motion. The relevance of these results to the study of the stability of astrophysical jets is briefly commented.

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