Figure 1: Schematic view of the MHD wake a a spherical cloud. | |
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Figure 2: Illustration of the compression associated with the propagation of Alfvén-like perturbation in a curved magnetic field. The field lines are represented by the parallel curves and define a local Alfvén velocity , is the curvature radius and is a transverse perturbation along the curvature direction. For straight lines, the Alfvénic transverse perturbation has no compression, whereas in a curved geometry, the volume of small elements of flux tubes changes with the distance to the curvature center: any displacement towards the curvature center drives a compression and any displacement away from the curvature center drives a depression. | |
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Figure 3: Total dissipation versus magnetic field strength for different radii of curvature . The power is normalized to the X-ray luminosity in the Galactic center region, so that 1 is the power required to balance the radiative cooling. Contributions Q_{A1}, Q_{S} and for the power dissipated in the Alfvén wing by non-linear effect, in the slow wing, and in the fast perturbation respectively, are also plotted, although the estimates for the slow and fast perturbations lose accuracy below 100 G. | |
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Figure A.1: The equilibrium magnetic field and notation definitions. |
Figure B.2: Dissipation rate as a function of the 2-D bulk Reynolds number. Here, . Points are the result of numerical integration of Eq. (B.8). The two asymptotes and result from its analytical integration in the viscous and non viscous regimes. |