Table 1.
Three He donor models studied in this work.
| Model |
 |
 |
 |
log Pf |
 |
af |
 |
 |
 |
 |
Vkick | Lpeak | tpeak | Ein |
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| (M⊙) | (M⊙) | (M⊙) | (days) | (K) | (1010 cm) | (km s−1) | (km s−1) | (%) | (km s−1) | (103 L⊙) | (103 yr) | (1049 erg) | ||
| A | 1.00 | 0.35 | 0.30 | −2.08 | 4.10 | 1.34 | 0.37 | 901 | 320 | 5.7 | 201 | 0.08 | 2.96 | 1.15 |
| B | 1.00 | 0.50 | 0.45 | −1.75 | 4.50 | 2.28 | 0.70 | 654 | 288 | 3.1 | 95 | 1.48 | 0.06 | 1.07 |
| C | 1.00 | 0.55 | 0.50 | −1.70 | 4.53 | 2.50 | 0.77 | 614 | 287 | 2.8 | 83 | 2.09 | 0.04 | 1.08 |
Notes. 
and 
are the initial masses of the WD and donor at the beginning of mass transfer. 
, Pf, 
, af, 
, 
, and 
denote the final mass, orbital period, effective temperature, binary separation, radius, orbital velocity, and rotational velocity of the donor star at the moment of the SN explosion, respectively. We assume that the He donor star is tidally locked to its orbital motion. ΔM and Vkick are the total stripped donor masses and kick velocity caused by the SN impact. Lpeak and tpeak give the peak luminosity and the corresponding post-impact evolutionary time of our MESA models before the deposited energy is radiated away, i.e. before the stars go back to the thermal equilibrium state. Ein corresponds to the total amount of energy deposited into the donor star due to the interaction with SN Ia ejecta.
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