Impact of convective overshooting on the single-degenerate model of Type Ia supernovae

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Table 1.

SN Ia birth rate for δ_ov = 0.00.

M_WD/M_⊙	△log₁₀a	M_A/M_⊙	M_B/M_⊙	△q	ν/yr⁻¹	$\bar{ν} / {yr}^{- 1}$ $\bar{\nu}/\mathrm{yr}^{-1}$
0.65–0.7	0.07	2.42	3.20	0.2001	0.00016	0.00027
0.65–0.7	0.13	2.42	3.20	0.2414	0.00039

0.7–0.75	0.13	3.20	3.86	0.1396	0.00011	0.00032
0.7–0.75	0.53	3.20	3.86	0.1709	0.00053

0.75–0.8	0.53	3.86	4.48	0.1226	0.00023	0.00031
0.75–0.8	0.57	3.86	4.48	0.1967	0.00039

0.8–0.9	0.57	4.48	5.60	0.1967	0.00045	0.00051
0.8–0.9	0.63	4.48	5.60	0.2235	0.00056

0.9–1.0	0.63	5.60	6.63	0.1625	0.00023	0.00030
0.9–1.0	0.69	5.60	6.63	0.2340	0.00036

1.0–1.1	0.69	6.63	7.58	0.1891	0.00019	0.00021
1.0–1.1	0.72	6.63	7.58	0.2192	0.00023

1.1–1.2	0.72	7.58	8.48	0.1863	0.00013	0.00016
1.1–1.2	0.76	7.58	8.48	0.2377	0.00018

Notes. For each range of WD masses M_WD, M_A, and M_B represent the corresponding lower and upper zero-age progenitor masses, respectively. Δq and Δlog₁₀a denote the typical mass ratio and separation ranges for the regions in Figs. 2, 3, and 4 that lead to SNe Ia. The ν and $\bar{ν}$ $\bar{\nu}$ are the calculated SN Ia birth rate, representing the extremes of the distribution applied across the entire range, with $\bar{ν}$ $\bar{\nu}$ being a simple mean of these two extremes.

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