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\section{Steady vs Eruptive Massloss}  The mass loss rates during the last few hundred years of evolution of some core collapse supernova progenitors seem to violate the maximum values allowed by line-driven winds ($\dot{M} \sim 10^{-4}$M$_\odot$yr$^{-1}$, Smith \& Owocki 2006, \citet{Smith_2006},  see also Fig.~\ref{fig}). 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). This mechanism is able to explain mass loss rates of $\sim 0.01 − 1 $M$_\odot$yr$^{-1}$ and velocities of $\sim 200 − 500$ km s$^{-1}$ (Quataert et al. 2015). 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).