Linear and non linear tearing and Kelvin-Helmholtz driven instabilities in current-sheets with velocity shears: three-dimensional compressive MHD simulations.

Details Linear and non linear tearing and Kelvin-Helmholtz driven instabilities in current-sheets with velocity shears: three-dimensional compressive MHD simulations. Linear and non linear tearing and Kelvin-Helmholtz driven instabilities in current-sheets with velocity shears: three-dimensional compressive MHD simulations.

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh42a..07l&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH42A-07

Astronomy and Astrophysics

Astrophysics

7526 Magnetic Reconnection (2723, 7835), 7836 Mhd Waves And Instabilities (2149, 2752, 6050), 7839 Nonlinear Phenomena (4400, 6944), 7863 Turbulence (4490)

Scientific paper

Magnetic shear driven instabilities play a major role both in the dynamics of astrophysical objects and, in particular, in the evolution of several structures in the heliosphere. Although tearing-driven dynamics in two dimensions are relatively well understood, in three dimensions the overall dynamics can be highly complex due to the onset of secondary instabilities. The presence of sheared flows, and the resulting stream plus current-sheet interaction, adds to this complexity. Considering two different perturbed equilibrium configurations of a current-sheet, a pressure-balanced and a force-free configuration, we present the three dimensional evolution of a tearing instability driven current- sheet in the presence of velocity shears, in the framework of compressible and resistive MHD. The large scale structure of the initial configuration determines the linear and non linear evolution of the system: primary (resistive and/or Kelvin-Helmholtz like) modes are selected according to the geometry of the magnetic field, secondary instability development depends on the initial equilibrium configuration with the strongest modes characterized by a specific direction in Fourier space. The competition between primary and secondary modes determines the global plasma structure in the non linear regime and, in all cases, the magnetic energy spectrum is observed to be highly anisotropic.

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