Fig. 2
Spectral evolution of turbulence energy density, Ew (top), and differential proton number density, N (bottom), for a SNR freely expanding into a uniform ISM (thick lines) at the age of 100 (black), 400 (red), and 1000 (green) years. For comparison, Ew and N derived with Bohm-like diffusion are given with thin lines. The shell and k0 are the same as in Fig. 1.
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