Three-dimensional delayed-detonation models with nucleosynthesis for Type Ia supernovae

• Published in: Monthly notices of the Royal Astronomical Society Vol. 429; no. 2; pp. 1156 - 1172
• Main Authors: Seitenzahl, Ivo R., Ciaraldi-Schoolmann, Franco, Röpke, Friedrich K., Fink, Michael, Hillebrandt, Wolfgang, Kromer, Markus, Pakmor, Rüdiger, Ruiter, Ashley J., Sim, Stuart A., Taubenberger, Stefan
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 21.02.2013
• Subjects: Dwarf stars; Isotopes; Simulation; Supernovae; supernovae: general; nuclear reactions, nucleosynthesis, abundances; white dwarfs
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/sts402

We present results for a suite of 14 three-dimensional, high-resolution hydrodynamical simulations of delayed-detonation models of Type Ia supernova (SN Ia) explosions. This model suite comprises the first set of three-dimensional SN Ia simulations with detailed isotopic yield information. As such, it may serve as a data base for Chandrasekhar-mass delayed-detonation model nucleosynthetic yields and for deriving synthetic observables such as spectra and light curves. We employ a physically motivated, stochastic model based on turbulent velocity fluctuations and fuel density to calculate in situ the deflagration-to-detonation transition probabilities. To obtain different strengths of the deflagration phase and thereby different degrees of pre-expansion, we have chosen a sequence of initial models with 1, 3, 5, 10, 20, 40, 100, 150, 200, 300 and 1600 (two different realizations) ignition kernels in a hydrostatic white dwarf with a central density of 2.9 × 109 g cm−3, as well as one high central density (5.5 × 109 g cm−3) and one low central density (1.0 × 109 g cm−3) rendition of the 100 ignition kernel configuration. For each simulation, we determined detailed nucleosynthetic yields by post-processing 106 tracer particles with a 384 nuclide reaction network. All delayed-detonation models result in explosions unbinding the white dwarf, producing a range of 56Ni masses from 0.32 to 1.11 M. As a general trend, the models predict that the stable neutron-rich iron-group isotopes are not found at the lowest velocities, but rather at intermediate velocities (∼3000-10 000 km s−1) in a shell surrounding a 56Ni-rich core. The models further predict relatively low-velocity oxygen and carbon, with typical minimum velocities around 4000 and 10 000 km s−1, respectively.