The impact of chemical differentiation of white dwarfs on thermonuclear supernovae

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Table 2

Results of sub-Chandrasekhar explosions.

Age^a	h _ig^b	M(⁵⁶Ni)	M(Fe,sta)^c	M(IME)	K
(Gyr)	(km)	(M_⊙)	(M_⊙)	(M_⊙)	(10⁵¹ erg)

–^d	0	0.70	0.055	0.22	1.39
0.6	0	0.69	0.054	0.23	1.34
8.0	0	0.68	0.058	0.24	1.35
0.6	70	0.63	0.054	0.28	1.31
8.0	70	0.64	0.057	0.30	1.34

Notes. All models: mass of the carbon-oxygen core, M_core = 1 M_⊙; mass of the He envelope M_env = 0.080 M_⊙; central density, ρ_c = 5.8 × 10⁷ g cm^-3; density at the base of the He envelope, ρ_base = 2.1 × 10⁶ g cm^-3.

^(a)

Time since the beginning of the cooling sequence.

^(b)

Altitude at which the He detonation starts.

^(c)

Ejected mass of stable Fe-group nuclei.

^(d)

Reference model, with a homogeneous composition of the core of 49% carbon and oxygen plus 2% ²²Ne.

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