2015MNRAS.447.1370D

We present non-LTE (non-Local-Thermodynamic-Equilibrium) time-dependent radiative transfer simulations for ejecta produced by the detonation of a helium shell at the surface of a low-mass carbon/oxygen white dwarf (WD). This mechanism is one possible origin for supernovae (SNe) with faint and fast-decaying light curves, such as.Ia SNe and Ca-rich transients. Our initial ejecta conditions at 1d are given by the 0.18 B explosion model COp45HEp2 of Waldman et al. The 0.2M_☉ ejecta initially contains 0.11M_☉ of He, 0.03M_☉ of Ca, and 0.03M_☉ of Ti. We obtain an ∼ 5d rise to a bolometric maximum of 3.59x10⁴¹erg/s, primarily powered by 48V decay. Multi-band light curves show distinct morphologies, with a rise to maximum magnitude (-14.3 to -16.7 mag) that varies between 3 to 9d from the U to the K bands. Near-IR light curves show no secondary maximum. Because of the presence of both Hei and Siii lines at early times we obtain a hybrid Type Ia/Ib classification. During the photospheric phase line blanketing is caused primarily by Tiii. At nebular times, the spectra show strong CaII lines in the optical (but no [Oi] 6300-6364Å emission), and Tiii in the near-IR. Overall, these results match qualitatively the very disparate properties of.Ia SNe and Ca-rich transients. Although the strong Tiii blanketing and red colours that we predict are rarely observed, they are seen, for example, in OGLE-2013- SN-079. Furthermore, we obtain a faster light-curve evolution than, for example, PTF10iuv, indicating an ejecta mass >0.2M_☉. An alternate scenario may be the merger of two WDs, one or both composed of He.