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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 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, 2014). 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. collapse (Shiode \& Quataert 2014).  Binary interaction in the final years before core collapse could also cause enhanced 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.