To the problem of the solar wind interaction with magnetized interstellar plasma

Abstract: The interaction between the solar wind and the magnetized plasma component of the local interstellar medium (LISM) is computed by solving axisymmetric magnetohydrodynamic (MHD) equations. The solar wind is assumed to be non-magnetized. The magnetic field of the undisturbed LISM is assumed to be parallel to the supersonic incident flow. The influence of the magnetic field on a shape and position of the bow shock, the heliopause and the terminal shock is investigated. It is shown that the distance between the bow shock and the heliopause along the critical streamline becomes shorter in magnetized case, that leads to greater transparentness of this region in respect to interstellar observed. The numerical results of Fujimoto and Matsuda (1991) on a similar problem are discussed.Note: Research direction:Mathematical modelling in actual problems of science and technic