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Turbulence and Magnetic Field Amplification in Supernova Remnants: Interactions Between a Strong Shock Wave and Multiphase Interstellar Medium

  • Authors: Tsuyoshi Inoue, Ryo Yamazaki, and Shu-ichiro Inutsuka

INOUE, YAMAZAKI, & INUTSUKA 2009 The Astrophysical Journal 695 825.

  • Provider: AAS Journals

Caption: Figure 7.

Cross section profiles along the y-axis at x = 1.0 pc of Model 1 (solid) and x-axis at y = 1.0 pc of Model 2 (dotted). The number density, magnetic field strength, velocity component normal to the shock ( v y for Model 1 and v x for Model 2), and velocity component tangential to the shock ( v x for Model 1 and v y for Model 2) are plotted from the top to bottom panel. The shock front is located around position 1.85 pc (Model 1) and 1.90 pc (Model 2). The left and the right sides of these are downstream and upstream, respectively.

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