We present 1-D non-Local-Thermodynamic-Equilibrium time-dependent radiative-transfer simulations for a large grid of supernovae ( SNe ) IIb/Ib/Ic that result from the terminal explosion of the mass donor in a close-binary system .
Our sample covers ejecta masses M _ { e } of 1.7–5.2 M _ { \odot } , kinetic energies E _ { kin } of 0.6–5.0 \times 10 ^ { 51 } erg , and ^ { 56 } N i masses of 0.05–0.30 M _ { \odot } .
We find a strong correlation between the ^ { 56 } N i mass and the photometric properties at maximum , and between the rise time to bolometric maximum and the post-maximum decline rate .
We confirm the small scatter in ( V - R ) at 10 d past R -band maximum .
The quantity V _ { m } \equiv \sqrt { 2 E _ { kin } / M _ { e } } is comparable to the Doppler velocity measured from He i 5875 Å at maximum in SNe IIb/Ib , although some scatter arises from the uncertain level of chemical mixing .
The O i 7772 Å line may be used for SNe Ic , but the correspondence deteriorates with higher ejecta mass/energy .
We identify a temporal reversal of the Doppler velocity at maximum absorption in the \sim 1.05 \mu m feature in all models .
The reversal is due to He i alone and could serve as a test for the presence of helium in SNe Ic .
Because of variations in composition and ionisation , the ejecta opacity shows substantial variations with both velocity and time .
This is in part the origin of the offset between our model light curves and the predictions from the Arnett model .