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Recent studies have demonstrated the diversity in type Ia supernovae (SNe Ia)at early times and highlighted a need for a better understanding of theexplosion physics as manifested by observations soon after explosion. To thisend, we present a Monte Carlo code designed to model the light curves ofradioactively driven, hydrogen-free transients from explosion to approximatelymaximum light. In this initial study, we have used a parametrised descriptionof the ejecta in SNe Ia, and performed a parameter study of the effects of the$^{56}$Ni distribution on the observed colours and light curves for a fixed$^{56}$Ni mass of 0.6 $M_\odot$. For a given density profile, we find thatmodels with $^{56}$Ni extending throughout the entirety of the ejecta aretypically brighter and bluer shortly after explosion. Additionally, the shapeof the density profile itself also plays an important role in determining theshape, rise time, and colours of observed light curves. We find that themulti-band light curves of at least one SNe Ia (SN 2009ig) are inconsistentwith less extended $^{56}$Ni distributions, but show good agreement with modelsthat incorporate $^{56}$Ni throughout the entire ejecta. We further demonstratethat comparisons with full $UVOIR$ colour light curves are powerful tools indiscriminating various $^{56}$Ni distributions, and hence explosion models.

Modelling the early time behaviour of type Ia supernovae: effects of the $^{56}$Ni distribution