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Table 2.

Results of the models computed.

Model ΔMWD (M⊙) ΔMesc (M⊙) Δ M WD ( M ejecta + M disk ) $ \frac{\Delta M_{\mathrm{WD}}}{(M_{\mathrm{ejecta}} + M_{\mathrm{disk}})} $ Δ M esc ( M ejecta + M disk ) $ \frac{\Delta M_{\mathrm{esc}}}{(M_{\mathrm{ejecta}} + M_{\mathrm{disk}})} $ ΔMSS, lost (M⊙) ΔMSS, WD (M⊙) Disk disruption
A 9.84 × 10−8 3.14 × 10−6 3.04% 96.96% 5.5 × 10−10 5.92 × 10−7 Yes
B 1.61 × 10−7 2.14 × 10−6 7.01% 92.99% 1.1 × 10−9 2.37 × 10−6 Yes
C 1.92 × 10−7 3.05 × 10−6 5.94% 94.06% 2.75 × 10−9 1.93 × 10−6 Yes
D 2.96 × 10−7 2.95 × 10−6 9.14% 90.86% 1.1 × 10−9 2.01 × 10−6 Yes
E 1.95 × 10−6 4.58 × 10−6 29.87% 70.13% 1.58 × 10−8 2.22 × 10−6 Partially
F 8.69 × 10−7 2.35 × 10−6 26.97% 73.03% 3.85 × 10−8 9.41 × 10−7 Partially
G 3.46 × 10−7 2.89 × 10−6 10.72% 89.28% − 5.35 × 10−7 Yes
H 5.21 × 10−7 2.71 × 10−6 16.12% 83.88% 8.3 × 10−8 1.04 × 10−6 Yes

Notes. Mass (ejecta plus disk) gravitationally bound to the white dwarf, ΔMWD, and total mass leaving the binary system, ΔMesc, together with their fractions (in %) over the total ejecta plus disk masses, after collision of the disk with the nova ejecta. ΔMSS, lost is the mass lost from the system by the secondary star in the interaction with the nova ejecta, while ΔMSS, WD is the mass of the secondary that is ultimately accreted by the white dwarf.

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