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Intense stellar mass loss during the final years before core collapse could be caused by   internal gravity waves excited by core convection during Neon and Oxygen fusion (Quataert \& Shiode 2012). Most importantly, the model predicts 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 (Shiode \& Quataert 2014).   Binary interaction in the final years before core collapse during Roche-lobe overflow (RLOF) or common envelope (CE) phase (e.g. Podsiadlowski et al. 1992)  could also cause enhanced, irregular mass loss. 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.  The  rate of stars exploding during or short-after the onset of binary interactions should be interaction is  small ($< 5$\%, De Mink, Priv. Comm.) and inthis case  no correlation is expected between mass loss rate and time to core collapse.   %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 %\begin{itemize}  %\item  \textbf{Binary Interactions} The %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). %\item \textbf{Eruptive Massloss}  %\item \textbf{Pulsationally Enhanced Massloss}  \end{itemize} %\end{itemize}