We propose an alternative explanation for the post-breakout emission of SN 2008D that cannot be reproduced by the explosion of a normal Wolf-Rayet star. We explored several physical scenarios and proposed that the early emission was enhanced by the presence of 56Ni in the outermost layers of the ejecta in addition to the usual internal distribution. This kind of double-peaked 56Ni distribution could be explained by the formation of jets during the explosion.