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Table 1

Main-sequence companion star models.

Model1 Mwd Mc,i Mc,f Pf af af/R2 Mstripped vkick SNe Ia2
[M] [M] [M] [d] [1011 cm] [M] [km  s-1]

ms_20a 0.70 2.00 0.74 0.98 3.72 3.06 0.181 51.01 disk instability
ms_20b 0.90 2.00 1.17 0.46 2.40 2.75 0.105 58.78 disk instability
ms_22a 0.80 2.20 1.21 0.29 1.77 2.72 0.173 105.29 weak H-shell flash
ms_20c 0.80 2.00 1.22 0.56 2.74 2.71 0.171 64.32 weak H-shell flash
ms_24a 0.90 2.40 1.40 0.33 1.95 2.63 0.172 94.95 stable H burning
ms_20d 1.00 2.00 1.40 0.57 2.83 2.63 0.113 53.32 weak H-shell flash
ms_23a 0.90 2.30 1.50 0.35 2.08 2.59 0.162 85.66 stable H burning
ms_24b 1.00 2.40 1.88 0.37 2.25 2.46 0.116 66.91 stable H burning
ms_28a 1.10 2.80 2.00 0.33 2.11 2.43 0.159 84.50 optically thick wind
ms_30a 1.20 3.00 2.45 0.44 2.64 2.33 0.141 65.34 optically thick wind

Notes. Mwd and Mc,i are the initial masses of WD and its companion at the beginning of mass transfer, respectively. Mc,f, Pf, af and R2 denote the final mass of companion star, the orbital period, the binary separation and the radius of secondary at the moment of supernova explosion, respectively. Mstripped and vkick are the stripped mass and the kick velocity caused by supernova impact.

(1)

All models have been named with the same way. For example, ms_20(a, b, c, d), the “ms” corresponds to CO WD + MS system, the middle number “20” means the Mc,f is 2.0   M. The final alphabet “a”, “b”, “c” or “d” denote the different models with the different Mc,f but the same Mc,i.

(2)

The WD explodes as an SN Ia in the disk instability phase, in the optically thick wind phase, in the stable H-shell burning phase and in the weak H-shell flash phase, respectively.

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