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We examine MHD simulations of the propagation of a strong shock wave throughthe interstellar two-phase medium composed of small-scale cloudlets and diffusewarm neutral medium in two-dimensional geometry. The pre-shock two-phase mediumis provided as a natural consequence of the thermal instability that isexpected to be ubiquitous in the interstellar medium. We show that theshock-compressed shell becomes turbulent owing to the preshock densityinhomogeneity and magnetic field amplification takes place in the shell. Themaximum field strength is determined by the condition that plasma beta ~ 1,which gives the field strength on the order of 1 mG in the case of shockvelocity ~ 1,000 km/s. The strongly magnetized region shows filamentary andknot-like structures in two-dimensional simulations. The spatial scale of theregions with magnetic field of 1 mG in our simulation is roughly 0.05 pc whichis comparable to the spatial scale of the X-ray hot spots recently discoveredin supernova remnants where the magnetic field strength is indicated to beamplified up to the order of 1 mG. This result may also suggest that theturbulent region with locally strong magnetic field is expected to be spreadout in the region with frequent supernova explosions, such as in the Galacticcenter and starburst galaxies.

Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between A Strong Shock Wave and Multi-Phase Interstellar Medium