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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 duringOxygen and  Neon and Oxygen  fusion (Quataert \& Shiode 2012, 2014). 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.   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.    %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.