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In the ONeMg cores of $8.8-9.5~{\rm M}_\odot$ stars, neon and oxygen burningis ignited off-center. Whether the neon-oxygen flame propagates to the centeris critical to determine whether these stars undergo Fe core collapse orelectron capture induced ONeMg core collapse. We present more details of starsthat ignite neon and oxygen burning off-center. The neon flame is establishedin a similar manner to the carbon flame of super-AGB stars, albeit with anarrower flame width. The criteria for establishing a flame are able to be metif the strict Schwarzschild criterion for convective instability is adopted.Mixing across the interface of the convective shell disrupts the conditions forthe propagation of the burning front and instead the shell burns as a series ofinward-moving flashes. While this may not directly affect whether the burningwill reach the center (as in super-AGB stars), the core is allowed to contractbetween each shell flash. Reduction of the electron fraction in the shellreduces the Chandrasekhar mass and the center reaches the threshold density forthe URCA process to activate and steer the remaining evolution of the core.This highlights the importance of a more accurate treatment of mixing in thestellar interior for yet another important question in stellar astrophysics -determining the properties of stellar evolution and supernova progenitors atthe boundary between electron capture supernova and iron core-collapsesupernova.

The final fate of stars that ignite neon and oxygen off-center: electron capture or iron core-collapse supernova?