2017/10/31 by Kevin Wilk, D. John Hillier, Luc Dessart · 1 citation
Physics and Astronomy · #astro-ph.SR #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stx2816
25 pages, 24 figures, Accepted for publication in MNRAS
arxiv created 2017/10/31 · arxiv updated 2017/12/27
We present one-dimensional non-local thermodynamic equilibrium time-dependent radiative transfer simulations (using CMFGEN) of two sub-Chandrasekhar (sub-M\rm Ch), one M\rm Ch and one super-M\rm Ch Type Ia SN ejecta models. Three originate from M\rm Ch delayed detonation models, and the fourth is a sub-M\rm Ch detonation model. Ejecta masses are 1.02, 1.04, 1.40, and 1.70 M_\odot, and all models have 0.62 M_\odot of 56\rm Ni. Sub-M\rm Ch model light curves evolve faster, reaching bolometric maximum 2--3 days earlier and having 3--4 days shorter bolometric half light widths. The models vary by ∼12 per cent at maximum bolometric luminosity and by 0.17 mag in B\rm max. While ΔM15(B) increases with ejecta mass it only varies by ∼5 per cent around 1 mag. Sub-M\rm Ch models are 0.25 mag bluer in B-R at B\rm max. Optical spectra share many similarities, but lower mass models exhibit less UV line blanketing during the photospheric phase. At nebular times, significant NIR spectroscopic differences are seen. In particular, emission lines of the Ca II NIR triplet; [S III] λλ9068,9530; [Ca II] λλ7291,7324; [Ar III] λλ7135,7751; and [Ni II] 1.939 μm are stronger in higher mass models. The [Ni II] 1.939 μm line is absent in the sub-M\rm Ch detonation model, and provides a valuable potential tool to distinguish sub-M\rm Ch explosions from M\rm Ch explosions. In general, the nebular phase models are too highly ionized. We attribute this to the neglect of clumping and/or the distribution of intermediate mass and iron group elements. The two sub-M\rm Ch models, while exploded by different mechanisms, can be distinguished in the J and H bands at late times (e.g., +200 days).