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There is both observational and theoretical evidence that the ejecta ofcore-collapse supernovae (SNe) are structured. Rather than being smooth andhomogeneous, the material is made of over-dense and under-dense regions ofdistinct composition. Here, we explore the effect of clumping on the SNradiation during the photospheric phase using 1-D non-local thermodynamicequilibrium radiative transfer and an ejecta model arising from ablue-supergiant explosion (yielding a Type II-peculiar SN). Neglecting chemicalsegregation, we adopt a velocity-dependent volume-filling factor approach thatassumes that the clumps are small but does not change the column density alongany sightline. We find that clumping boosts the recombination rate in thephotospheric layers, leading to a faster recession of the photosphere, anincrease in bolometric luminosity, and a reddening of the SN colors throughenhanced blanketing. The SN bolometric light curve peaks earlier andtransitions faster to the nebular phase. On the rise to maximum, the strongestluminosity contrast between our clumped and smooth models is obtained at theepoch when the photosphere has receded to ejecta layers where the clumpingfactor is only 0.5 -- this clumping factor may be larger in Nature. Clumping isseen to have a similar influence in a Type II-Plateau SN model. As we neglectboth porosity and chemical segregation our models underestimate the true impactof clumping. These results warrant further study of the influence of clumpingon the observables of other SN types during the photospheric phase.

Impact of clumping on core-collapse supernova radiation