Theoretical uncertainties of the Type Ia supernova rate

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Table 2

Critical mass ratio Q_crit for stable RLOF for different types of donor stars, in the case of a non-degenerate and a degenerate accretor.

Type of donor	Non-degenerate	Degenerate
	accretor^a,b	accretor^a

MS, M > 0.7 M_⊙^c	0.625^d (MS accretor)	–
MS, M < 0.7 M_⊙^c	1.44	1.0
HG	0.25	0.21
GB, AGB^e		0.87
He-HG	0.25	0.21
He-GB	1.28	0.87
WD	–	1.6

Notes.

^(a)

The symbol – indicates that no value is defined.

^(b)

Based on Hurley et al. (2002).

^(c)

We distinguish between MS stars (M > 0.7 M_⊙) and low-mass MS stars (M < 0.7 M_⊙), because the latter are almost completely convective, and react differently to mass loss and gain.

^(d)

Based on de Mink et al. (2007).

^(e)

At solar metallicity x≈ 0.3 (Hurley et al. 2000, 2002).

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