The bright, dusty aftermath of giant eruptions and H-rich supernovae - Late interaction of supernova shocks and dusty circumstellar shells created by 45, 50, and 60 M⊙ stars

Open Access

Fig. 5

Upper panels: SNR (only gas) kinetic (solid), thermal (dotted), and radiated (dashed) energies as a function of time for S₂₀₀ (left) and B₂₀₀ (right). Lower panels: evolution of the dust mass, normalized to that ejected by the eruption. For all panels, thicker lines correspond to S₂₀₀ and S₂₀₀, while thinner lines to B_200−Test and S_200−Test, respectively.

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