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Previous numerical simulations of double-peaked SNe IIb light curves havedemonstrated that the radius and mass of the hydrogen-rich envelope of theprogenitor star can significantly influence the brightness and timescale of theearly-time light curve around the first peak. In this study, we investigate howThomson scattering and chemical mixing in the SN ejecta affect the opticallight curves during the early stages of the SNe IIb using radiationhydrodynamics simulations. By comparing the results from two differentnumerical codes (i.e., \stella{} and \snec{}), we find that the opticalbrightness of the first peak can be reduced by more than a factor of 3 due tothe effect of Thomson scattering that causes the thermalization depth to belocated below the Rosseland-mean photosphere, compared to the correspondingcase where this effect is ignored. We also observe a short-lived plateau-likefeature lasting for a few days in the early-time optical light curves of ourmodels, in contrast to typical observed SNe IIb that show a quasi-lineardecrease in optical magnitudes after the first peak. A significant degree ofchemical mixing between the hydrogen-rich envelope and the helium core in SNejecta is required to reconcile this discrepancy between the model predictionand observation. Meanwhile, to properly reproduce the first peak, a significantmixing of \nifs{} into the hydrogen-rich outermost layers should be restricted.Our findings indicate that inferring the SN IIb progenitor structure from asimplified approach that ignores these two factors may introduce substantialuncertainty.

The effects of Thomson scattering and chemical mixing on early-time light curves of double peaked type IIb supernovae