All Figures

	Figure 1: Comparison of numerical solutions of the 1D, pure diffusion problem to analytical solutions for t= 0 ( upper panel) and t=100 ( lower panel). Continuous lines denote analytical solutions for different times and crosses represent numerical solutions.
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In the text

	Figure 2: Diffusion of cosmic rays along an inclined magnetic field: a) the initial spheroidal distribution of at t= 0 and b) the ellipsoidal distribution at t=100.
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In the text

	Figure 3: Diffusion of cosmic rays along an inclined magnetic field at t=100. Two cuts of the ellipsoid shown in Fig. 2 are made ( b) along the major axis (crosses) and along the minor axis (asterisks). The full and dotted lines represent the corresponding cuts of the fitted 2D Gaussian profile.
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In the text

	Figure 4: Diffusion of cosmic rays along an inclined magnetic field at t=40: a) the cosmic ray energy density and magnetic field and b) distribution of gas density and gas velocity.
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In the text

	Figure 5: Geometry of the initial state stratified by vertical gravity: a) the slice in yz-plane showing the stratification of the background distribution of cosmic rays and magnetic field along with the localized cosmic ray injection region, b) the initial, horizontal magnetic field is parallel to the horizontal and parallel to the y-axis.
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In the text

	Figure 6: Propagation of cosmic rays in a vertically stratified atmosphere for the diffusion coefficient , after the local injection of cosmic ray energy: a) cosmic ray energy density and magnetic field in the yz-plane at x=0 and b) in the xy-plane at z=400, c) the density perturbation and the gas velocity in the xz-plane.
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In the text

	Figure 7: Same as Fig. 6 for the diffusion coefficient at t=100.
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In the text

	Figure 8: Same as Fig. 7 at t=150.
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In the text