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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).   Intense Intense, eruptive  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). 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 could also cause enhanced enhanced, irregular  mass loss. The rate of stars exploding during or short-after the onset of binary interactions should be small ($< 5$\%, De Mink, Priv. Comm.) and in this case no correlation is expected between mass loss rate and time to core collapse.