Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for Type Ia supernovae

• Published in: Monthly notices of the Royal Astronomical Society Vol. 438; no. 2; pp. 1762 - 1783
• Main Authors: Fink, Michael, Kromer, Markus, Seitenzahl, Ivo R., Ciaraldi-Schoolmann, Franco, Röpke, Friedrich K., Sim, Stuart A., Pakmor, Rüdiger, Ruiter, Ashley J., Hillebrandt, Wolfgang
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 21.02.2014
• Subjects: abundances; Astronomy; Dwarf stars; hydrodynamics; nuclear reactions; nucleosynthesis; radiative transfer; Supernovae; supernovae: general; white dwarfs; hydrodynamics; nuclear reactions, nucleosynthesis, abundances; white dwarfs; supernovae: general; radiative transfer
• ISSN: 0035-8711; 1365-2966; 1365-2966
• DOI: 10.1093/mnras/stt2315

We investigate whether pure deflagration models of Chandrasekhar-mass carbon–oxygen white dwarf stars can account for one or more subclass of the observed population of Type Ia supernova (SN Ia) explosions. We compute a set of 3D full-star hydrodynamic explosion models, in which the deflagration strength is parametrized using the multispot ignition approach. For each model, we calculate detailed nucleosynthesis yields in a post-processing step with a 384 nuclide nuclear network. We also compute synthetic observables with our 3D Monte Carlo radiative transfer code for comparison with observations. For weak and intermediate deflagration strengths (energy release E nuc ≲ 1.1 × 1051 erg), we find that the explosion leaves behind a bound remnant enriched with 3 to 10 per cent (by mass) of deflagration ashes. However, we do not obtain the large kick velocities recently reported in the literature. We find that weak deflagrations with E nuc ∼ 0.5 × 1051 erg fit well both the light curves and spectra of 2002cx-like SNe Ia, and models with even lower explosion energies could explain some of the fainter members of this subclass. By comparing our synthetic observables with the properties of SNe Ia, we can exclude the brightest, most vigorously ignited models as candidates for any observed class of SN Ia: their B − V colours deviate significantly from both normal and 2002cx-like SNe Ia and they are too bright to be candidates for other subclasses.