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Published March 2013 | Supplemental Material + Published
Journal Article Open

One-dimensional delayed-detonation models of Type Ia supernovae: confrontation to observations at bolometric maximum

Abstract

The delayed-detonation explosion mechanism applied to a Chandrasekhar-mass white dwarf offers a very attractive model to explain the inferred characteristics of Type Ia supernovae (SNe Ia). The resulting ejecta are chemically stratified, have the same mass and roughly the same asymptotic kinetic energy, but exhibit a range in ^(56)Ni mass. We investigate the contemporaneous photometric and spectroscopic properties of a sequence of delayed-detonation models, characterized by ^(56)Ni masses between 0.18 and 0.81 M_⊙. Starting at 1 d after explosion, we perform the full non-local thermodynamic equilibrium, time-dependent radiative transfer with the code CMFGEN, with an accurate treatment of line blanketing, and compare our results to SNe Ia at bolometric maximum. Despite the 1D treatment, our approach delivers an excellent agreement to observations. We recover the range of SN Ia luminosities, colours and spectral characteristics from the near-ultraviolet to 1 μm, for standard as well as low-luminosity 91bg-like SNe Ia. Our models predict an increase in rise time to peak with increasing ^(56)Ni mass, from ∼15 to ∼21 d, yield peak bolometric luminosities that match Arnett's rule to within 10 per cent and reproduce the much smaller scatter in near-infrared magnitudes compared to the optical. We reproduce the morphology of individual spectral features, the stiff dependence of the R(Si) spectroscopic ratio on ^(56)Ni mass and the onset of blanketing from Ti ii/Sc ii in low-luminosity SNe Ia with a ^(56)Ni mass ≲0.3 M_⊙. We find that ionization effects, which often dominate over abundance variations, can produce high-velocity features in Ca ii lines, even in 1D. Distinguishing between different SN Ia explosion mechanisms is a considerable challenge but the results presented here provide additional support to the viability of the delayed-detonation model.

Additional Information

© 2012 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2012 November 23. Received 2012 November 23; in original form 2012 October 15. First published online: December 21, 2012. LD acknowledges financial support from the European Community through an International Re-integration Grant, under grant number PIRG04-GA-2008-239184. DJH acknowledges support from STScI theory grants HST-AR-11756.01.A and HST-AR-12640.01 and NASA theory grant NNX10AC80G. The work of AMK was supported by the NSF grant AST-0709181 'Collaborative Research: Three-Dimensional Simulations of Type Ia Supernovae: Constraining Models with Observations.' This work was granted access to the HPC resources of CINES under the allocation 2011-c2011046608 and 2012-c2012046608 made by GENCI (Grand Equipement National de Calcul Intensif). A subset of the computations was also performed at Caltech Center for Advanced Computing Research on the cluster Zwicky funded through NSF grant PHY-0960291 and the Sherman Fairchild Foundation. The authors wish to thank Eduardo Bravo for sending us his delayed-detonation model DDTc; Ryan Chornock, Alex Filippenko and Jeff Silverman for sending us spectra of SN 2007hj published by Silverman et al. (2012); Rubina Kotak for sending us the spectrum of SN 2003gs used in this paper ahead of publication and Ivo Seitenzahl for providing neutronization rates in machine-readable form. This research has made use of the CfA Supernova Archive, which is funded in part by the National Science Foundation through grant AST 0907903; the Online Supernova Spectrum Archive (SUSPECT) and the Weizmann Interactive Supernova data Repository (WISEREP; Yaron & Gal-Yam 2012

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Published - MNRAS-2013-Blondin-2127-42.pdf

Supplemental Material - sts484_online_appendix.pdf

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August 19, 2023
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