Same as Fig. 6, but now comparing the photospheric properties for models r0e2 (smooth ejecta) and r0e2cl (same as model r0e2 but the ejecta is clumped, with a 10% volume filling factor). The clumped model is initially similar to the smooth counterpart, but as time progresses after bolometric maximum (which occurs in both at about 30 d), the clumped ejecta cools and recombines faster, entering the nebular phase 150 d after explosion, which is 30 d earlier than in model r0e2.
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