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Hybrid C/O/Ne white dwarfs

Project summary
In this project, we show that the inclusion of even a small amount of convective boundary mixing at the bottom of the convective C-burning shell leads to the stall of the C-flame propagation to the centre of a super-AGB star and, as a result, to the formation of a hybrid C/O/Ne core.
About the simulation codes
We used the stellar evolution code of MESA (revision 5329) to simulate the evolution of intermediate-mass stars from the pre-MS through to the white-dwarf cooling phase. To simulate thermohaline convection in the CO core, we have used the same spectral code, kindly provided to us by Bill Merryfield, that we previously employed in our simulations of thermohaline mixing in RGB stars.
Images and movies
Link to the paper