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Table 1

Summary of the 3D O deflagration simulations.

id. res. bCC gYe,rem iΔx
(g cm-3) (Y/N) (M) (M) (M) (km)

G13 2563 9.90 N 0.647 0.173 0.741 0.231 0.491 1.384 0.870
G14 5123 9.90 N 0.438 0.115 0.951 0.362 0.491 1.381 0.427
G15 2563 9.90 Y 1.212 0.223 0.177 0.047 0.493 1.392 0.870
J01 2563 9.95 N 0.631 0.171 0.768 0.233 0.491 1.379 0.870
J02 2563 9.95 Y 1.291 0.226 0.104 0.025 0.493 1.392 0.870

H01* 2563 10.3 N 1.401 0.022 0.000 0.000 0.486 1.356 0.870

Notes. The horizontal dashed line separates those models above it, in which enough material becomes unbound from the ONe core/WD that the remaining bound remnant has a mass below the effective Chandrasekhar limit MCh, from those below (i.e. the H series of models) which will collapse to form a neutron star. The quoted Fe masses are actually the sum of all the Fe-group elements. .


These diagnostics were calculated for H01 at t ≈ 330 ms, at which time the simulation was stopped because the maximum density reached ~1011 g cm-3, exhibiting clear signs of core collapse. Thus, for the H01 model is the mass of Fe-group elements in the core after ~330 ms


Ignition (central) density of ONe core at ignition of O deflagration.


Coulomb corrections included in EoS.


Total mass of bound ONeFe WD remnant


Mass of Fe-group elements in bound remnant.


Total ejected mass


Mass of ejected Fe-group elements.


Average electron fraction of bound remnant.


Effective Chandrasekhar mass of bound remnant.


Initial cell size for inner (flame) mesh.

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