NUCLEOSYNTHESIS IN TWO-DIMENSIONAL DELAYED DETONATION MODELS OF TYPE Ia SUPERNOVA EXPLOSIONS

By K. Maeda, Friedrich K. Röpke, M. Fink, W. Hillebrandt, C. Travaglio, F. Thielemann. 2010

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For the explosion mechanism of Type Ia supernovae (SNe Ia), different scenarios have been suggested. In these, the propagation of the burning front through the exploding white dwarf (WD) star proceeds in different modes, and consequently imprints of the explosion model on the nucleosynthetic yields can be expected. The nucleosynthetic characteristics of various explosion mechanisms are explored based on three two-dimensional explosion simulations representing extreme cases: a pure turbulent deflagration, a delayed detonation following an approximately spherical ignition of the initial deflagration, and a delayed detonation arising from a highly asymmetric deflagration ignition. Apart from this initial condition, the deflagration stage is treated in a parameter-free approach. The detonation is initiated when the turbulent burning enters the distributed burning regime. This occurs at densities around 107 g cm−3—relatively low as compared to existing nucleosynthesis studies for one-dimensional spherically symmetric models. The burning in these multidimensional models is different from that in one-dimensional simulations as the detonation wave propagates both into unburned material in the high-density region near the center of a WD and into the low-density region near the surface. Thus, the resulting yield is a mixture of different explosive burning products, from carbon-burning products at low densities to complete silicon-burning products at the highest densities, as well as electron-capture products synthesized at the deflagration stage. Detailed calculations of the nucleosynthesis in all three models are presented. In contrast to the deflagration model, the delayed detonations produce a characteristic layered structure and the yields largely satisfy constraints from Galactic chemical evolution. In the asymmetric delayed detonation model, the region filled with electron capture species (e.g., 58Ni, 54Fe) is within a shell, showing a large off-set, above the bulk of 56Ni distribution, while species produced by the detonation are distributed more spherically.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/7ea68eb9878945fc9e47d47b218b5e96b4c6862a

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Citations in the corpus

Nucleosynthesis in Stars and the Chemical Enrichment of Galaxies (2013, background): “Optical observations have also shown [FeII] λ 7155 and [NiII] λ 7378 for 12 Type Ia supernovae (Maeda et al. 2010b).”
THE SPECTROSCOPIC DIVERSITY OF TYPE Ia SUPERNOVAE (2000, methodology): “We thus reproduce the main result of Maeda et al. (2010a), although they base their spectroscopic classification on the velocity gradient of the Si iiλ6355 line defined by Benetti et al. (2005) as opposed to its absorption velocity at maximum (all the HV SN Ia in Fig.”
Three-dimensional delayed-detonation models with nucleosynthesis for Type Ia supernovae (2012, background): “…(e.g. Travaglio et al. 2004; Röpke et al. 2006a) such detailed information for delayed detonation explosion models is currently only available for a few two-dimensio al (Meakin et al. 2009; Maeda et al. 2010b) or one-dimensional explosion models (e.g. Iwamoto et al. 1999; Brachwitz et al. 2000).”
NEUTRON-RICH CHROMIUM ISOTOPE ANOMALIES IN SUPERNOVA NANOPARTICLES (2010, methodology): “…measured isotopic ratios with total yields, they could be compared with nucleosynthetic predictions for tracer particles in multi-dimensional simulations of SNIa explosions (Travaglio et al. 2004, 2005; Brown et al. 2005; Röpke et al. 2006; Meakin et al. 2009; Fink et al. 2010; Maeda et al. 2010).”