The impact of chemical differentiation of white dwarfs on thermonuclear supernovae

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Table 1

Results of Chandrasekhar-mass explosions.

Age^a	ρ _DDT	M(⁵⁶Ni)	M(IME)^b	K^c	m _max^d
(Gyr)	(g cm^-3)	(M_⊙)	(M_⊙)	(10⁵¹ erg)	(mag)

0.6	1.6 × 10⁷	0.40	0.67	1.26	–18.78
8.0	1.6 × 10⁷	0.43	0.70	1.37	–18.84
1.0^e	1.6 × 10⁷	0.41	0.67	1.27	−18.79
9.6^e	1.6 × 10⁷	0.43	0.69	1.38	−18.88
1.0^e	3.0 × 10⁷	0.71	0.42	1.42	−19.45
9.6^e	3.0 × 10⁷	0.74	0.42	1.51	−19.50
0.6	2.4 × 10⁷^f	0.59	0.52	1.37	−19.23
8.0	3.7 × 10⁷^g	0.83	0.34	1.54	−19.63

Notes. All models: central density, ρ_c = 3.0 × 10⁹ g cm^-3.

^(a)

Time since the beginning of the cooling sequence.

^(b)

Synthesized mass of intermediate-mass elements, from Si to Ca.

^(c)

Kinetic energy of the ejecta.

^(d)

Bolometric magnitude at maximum.

^(e)

Model with the diffusion coefficient of ²²Ne increased by a factor 5.

^(f)

Deflagration-to-detonation transition density estimated from the chemical composition at the flame front (Eq. (2)): X(¹²C) = 0.36, X(²²Ne) = 0.020.

^(g)

Deflagration-to-detonation transition density estimated from the chemical composition at the flame front using Eq. (2): X(¹²C) = 0.24, X(²²Ne) = 0.022.

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