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Date and Time of the Query: 2019-08-22 T20:36:18 PDT
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For refcode 2018MNRAS.474.3187W:
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Copyright by Royal Astronomical Society. 2018MNRAS.474.3187W Ejecta mass diagnostics of Type Ia supernovae Wilk, Kevin D.; Hillier, D. John; Dessart, Luc Abstract. We present one-dimensional non-local thermodynamic equilibrium time-dependent radiative transfer simulations (using CMFGEN) of two sub-Chandrasekhar (sub-M_Ch_), one M_Ch_ and one super-M_Ch_ Type Ia SN ejecta models. Three originate from M_Ch_ delayed detonation models, and the fourth is a sub-M_Ch_ detonation model. Ejecta masses are 1.02, 1.04, 1.40 and 1.70 M_&sun;_, and all models have 0.62 M_&sun;_ of ^56^Ni. Sub-M_Ch_ model light curves evolve faster, reaching bolometric maximum 2-3 d earlier and having 3-4 d shorter bolometric half-light widths. The models vary by ~12 per cent at maximum bolometric luminosity and by 0.17 mag in B_max_. While DeltaM_15_(B) increases with ejecta mass, it only varies by ~5 per cent around 1 mag. Sub-M_Ch_ models are 0.25 mag bluer in B - R at B_max_. Optical spectra share many similarities, but lower mass models exhibit less UV line blanketing during the photospheric phase. At nebular times, significant near-infrared (NIR) spectroscopic differences are seen. In particular, emission lines of the Ca II NIR triplet; [S III] lambdalambda9068,9530; [Ca II] lambdalambda7291,7324; [Ar III] lambdalambda7135,7751 and [Ni II] 1.939 micron are stronger in higher mass models. The [Ni II] 1.939 micron line is absent in the sub-M_Ch_ detonation model, and provides a valuable potential tool to distinguish sub-M_Ch_ explosions from M_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_Ch_ models, while exploded by different mechanisms, can be distinguished in the J and H bands at late times (e.g. +200 d). Key words: radiative transfer, supernovae: general, white dwarfs
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