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

By I. Seitenzahl, F. Ciaraldi-Schoolmann, F. Roepke, M. Fink, W. Hillebrandt, M. Kromer, Rüdiger Pakmor, A. Ruiter, S. Sim, Stefan Taubenberger. 2012

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We present results for a suite of fourteen 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 I a simulations with detailed isotopic yield information. As such, it may serve as a database for Chandrasekhar-mass delayeddetonation 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 t he deflagration to detonation transition (DDT) 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 central density of 2.9× 10 9 g cm −3 , plus in addition one high central density (5.5× 10 9 g cm −3 ) and one low central density (1.0× 10 9 g cm −3 ) rendition of the 100 ignition kernel configuration. For each simulatio n we determined detailed nucleosynthetic yields by post-processing 10 6 tracer particles with a 384 nuclide reaction network. All delayed detonation models result in explosions unbinding the white dwarf, producing a range of 56 Ni 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 (∼3, 000− 10, 000 km s −1 ) in a shell surrounding a 56 Ni-rich core. The models further predict relatively low velocity oxygen and carbon, with typical minimum velocities around 4, 000 and 10, 000 km s −1 , respectively.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/46246ab3204d48933791932142611cdba352194f

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Citations in the corpus

Sub-Chandrasekhar-mass White Dwarf Detonations Revisited (2017, methodology): “Thus, at least part of the discrepancy found by Seitenzahl et al. (2013a) between the solar Mn/Fe ratio and nucleosynthesis in sub-MCh detonations can be alleviated by including pure detonations of lower-mass WDs.”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “Ti is produced in CCSN and in SNIa (e.g., Rauscher et al. 2002; Seitenzahl et al. 2013).”
Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae (2013, methodology): “A1(a) and is used in this study and in Seitenzahl et al. (2013).”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, methodology): “Different progenitor metallicities and masses, and different accretion histories, could affect the number and location of ignition “kernels”, and thus the transition to detonation (e.g. Blondin et al. 2011; Kasen, Röpke & Woosley 2009; Seitenzahl et al. 2013b; Umeda et al. 1999).”
CORE-COLLAPSE SUPERNOVAE FROM 9 TO 120 SOLAR MASSES BASED ON NEUTRINO-POWERED EXPLOSIONS (2015, background): “It might be circumvented in more modern multidimensional models (e.g., Seitenzahl et al. 2013b) especially if the white dwarf expands appreciably during the deflagration stage prior to detonating.”