  In recent years a number of double-humped supernovae have been discovered.
This is a feature predicted by the dual-shock Quark-Nova model where a SN
explosion is followed (a few days to a few weeks later) by a Quark-Nova
explosion. SN 2009ip and SN 2010mc are the best observed examples of
double-humped SNe. Here, we show that the dual-shock Quark-Nova model naturally
explains their lightcurves including the late time emission, which we attribute
to the interaction between the mixed SN and QN ejecta and the surrounding CSM.
Our model applies to any star (O-stars, LBVs, WRs etc.) provided that the SN
explosion mass is ~ 20M_sun which point to the conditions for forming a
Quark-Nova.
