All Figures

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig1.eps} }% \end{figure}$ Figure 1: Schematic view of the MHD wake a a spherical cloud.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{4356fig2.eps}\end{figure}$ 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 $v_{\rm A}$ , $R_{\rm c}$ is the curvature radius and $v_{\rm r}$ 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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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig3.ps} } \end{figure}$ Figure 3: Total dissipation versus magnetic field strength for different radii of curvature $R_{\rm c}$ . 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 $Q_{\rm F}$ 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 $\mu$ G.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig6.eps} }% \end{figure}$ Figure A.1: The equilibrium magnetic field and notation definitions.

In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig4.ps} }% \end{figure}$ Figure B.1: Total dissipation per unit height in the MHD flow around an infinite cylinder for ${\cal R}_{\rm 2D}$ . Flow comes from the left hand side. The upper, mid and lower panels show the main velocity, the perturbed density and the perturbed flow divergence, respectively. Dashed and plain contours are negative and positive contours, respectively.

In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig5.eps} }% \end{figure}$ Figure B.2: Dissipation rate as a function of the 2-D bulk Reynolds number. Here, $Q_0 = \rho _0 r_{\rm c} v_{\rm c}^5/v_{\rm m}^2$ . Points are the result of numerical integration of Eq. (B.8). The two asymptotes $Q/Q_0 = 1.83 {\cal R}_{\rm 2D}$ and $Q/Q_0 = 5.45{\cal R}_{\rm 2D}^{-1}$ result from its analytical integration in the viscous and non viscous regimes.

In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{4356fig1.eps} }% \end{figure}$	Figure 1: Schematic view of the MHD wake a a spherical cloud.
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