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In the classical picture, electron-capture supernovae and theaccretion-induced collapse of oxygen-neon white dwarfs (ONeWDs) undergo anoxygen deflagration phase before gravitational collapse produces a neutron star(NS). These types of core collapse events are postulated to explain severalastronomical phenomena. In this work, the deflagration phase is simulated forthe first time using multidimensional hydrodynamics, with the aim of gainingnew insight into the explosive deaths of $8-10~M_\odot$ stars and ONeWDs thataccrete material from a binary companion star. The main aim is to determinewhether these events are thermonuclear or core-collapse supernova explosions,and hence whether NSs are formed by such phenomena. The deflagration issimulated in ONe cores with three different central ignition densities. Theintermediate density case is perhaps the most realistic, being based on recentnuclear physics calculations and 1D stellar models. The 3D hydrodynamicsimulations presented in this work begin from a centrally confined flamestructure using a level-set-based flame approach and are performed in $256^3$and $512^3$ numerical resolutions. In the simulations with intermediate and lowignition density, the cores do not appear to collapse into NSs. Instead, almosta solar mass of material becomes unbound from the cores, leaving boundremnants. These simulations represent the case in which semiconvective mixingduring the electron-capture phase preceding the deflagration is inefficient.The masses of the bound remnants double when Coulomb corrections are includedin the EoS, however they still do not exceed the effective Chandrasekhar massand, hence, would not collapse into NSs. The simulations with the highestignition density ($\log_{10}\rho_{\rm c}=10.3$), representing the case wheresemiconvective mixing is very efficient, show clear signs that the core willcollapse into a NS.

Do electron-capture supernovae make neutron stars? First multidimensional hydrodynamic simulations of the oxygen deflagration