Abstract
We show in this paper that intermediate shocks are formed from kinetic Alfven waves through wave form continuous steepening. From the action of nonlinear interaction and dispersion Alfven solitons are formed and then evolve into shocks. We calculated the traveling stationary structures directly from nonlinear autonomous equations which we had derived. These traveling stationary structures correspond to intermediate shock, switch-on shock or Alfven solitary waves. Another kind of rare discontinuity was discovered in the calculation from the rarefying solitary waves. The solitary wave series remain on the front of the shocks because of no strong dissipation appears in the equation. When we added some anomalous dissipation terms to the equations, intermediate shocks with increased in entropy appeared.
Highlights
Is there any intermediate shock in the solar wind? How is intermediate shock produced? These are problems discussed by space scientists recently
K field respectively, and kJ. >> 11 stand for the kinetic Alfven wave. p1 is the ion gyroradius In the solar wind it seems reasonable for k1p;2 k11 for the kinetic Alfven wave energy is propagating along the magnetic field: am
We will show by numerical analysis that the dispersive, nonlinear kinetic Alfven wave can evolve into intermediate shocks, Alfven solitons and magnetic kink along with the different parameters in the solar wind
Summary
Is there any intermediate shock in the solar wind? How is intermediate shock produced? These are problems discussed by space scientists recently. Corresponding to MHD wave modes, intermediate shock should be formed through Alfven wave evolution. The Alfven wave is a kind of transverse wave propagating along the magnetic field and has no nonlinear interaction and dissipation in the theory. We show that intermediate shock is evolved from the kinetic Alfven wave instead of from the MHD Alfven wave. >> k11 for the kinetic Alfven wave energy is propagating along the magnetic field: am ( 2 2) II = =VA - - Jk11. Alfven wave first evolves into Alfven solitons, into intermediate shock by the dissipation effect. We will show by numerical analysis that the dispersive, nonlinear kinetic Alfven wave can evolve into intermediate shocks, Alfven solitons and magnetic kink along with the different parameters in the solar wind
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