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

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Table 1

Summary of the 3D O deflagration simulations.

id.	res.		^bCC					^g ⟨ Y_e,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 M_Ch, 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

^(a)

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

^(b)

Coulomb corrections included in EoS.

^(c)

Total mass of bound ONeFe WD remnant

^(d)

Mass of Fe-group elements in bound remnant.

^(e)

Total ejected mass

^(f)

Mass of ejected Fe-group elements.

^(g)

Average electron fraction of bound remnant.

^(h)

Effective Chandrasekhar mass of bound remnant.

⁽ⁱ⁾

Initial cell size for inner (flame) mesh.

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