All Figures

Figure 1: The distribution of the electron temperature (solid line), of the dust temperature (dotted line), and of the electron density (dashed line) downstream ( top panels) and of the fractional abundances of some significant ions downstream ( bottom panels) for model m3 (left diagram) and model m9 (right diagram). H+1/H: solid line; N+1/N: short-dashed line: S+1/S: long-dashed line; O+2/O: dotted line.

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In the text

	Figure 2: [NII] 6548, [NII] 6583, and H line profiles (solid lines) calculated by model MB3 for region D3 observed by Blair et al. (1991). Dotted lines correspond to model m1, short-dashed line to m3. The fluxes are calculated at the emitting nebula.
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In the text

	Figure 3: Comparison of single-cloud models with observational data (black squares). m3: solid lines; m6: long-dashed lines; m7: dotted lines; m9: short-dashed lines; m10: dash-dotted lines.
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In the text

Figure 4: Consistent modeling of the Kepler SNR continuum SED by the summed model (thick solid line: bremsstrahlung; thin solid line: synchrotron radiation; dashed line: IR emission) and model m10 (dotted lines). The observational data are represented by black squares. The data point at 5400 Å from Leibowitz & Danziger (1983) is represented by an open square. The asterisks refer to Douvion et al. (2001a).

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In the text