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  %This energy can generate circumstellar environments with 10−3–1 solar masses reaching 100 AU before %explosion. We predict a correlation between the energy associated with pre-SN mass ejection and the %time to core collapse, with the most intense mass loss preferentially occurring closer to core collapse.  \begin{itemize}  \item \textbf{Line Driven Winds}  \item \textbf{Binary Interactions}  The ejection of the H-rich envelope can be the result of binary interaction during Roche-lobe overflow (RLOF) or common envelope (CE) phase (e.g. Podsiadlowski et al. 1992). Since the observed fraction of $\sim37\%$ of H-poor SNe among core-collapse explosions is too large to be reconciled with the evolution of single massive stars (e.g. Li et al. 2011, Smith et al. 2011), it is reasonable to expect that at least some SNe Ibc originate in binaries. The binary interaction and the stellar death of one of the two stars are however not necessarily related events, so that we would not generally expect the two phenomena to be synchronized. A stellar explosion can be driven by the CE evolution only under peculiar circumstances, like the inspiral of a compact object to the central core of the companion star (Chevalier 2012). As a result, simulations show that only a small fraction $\sim2-3$\% of SNe Ib/c progenitors to experience the ejection of the H envelope due to binary interaction in the last centuries before explosion (Chevalier 2012).