期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 438, 期 2, 页码 1762-1783出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stt2315
关键词
hydrodynamics; nuclear reactions, nucleosynthesis, abundances; radiative transfer; supernovae: general; white dwarfs
资金
- Deutsche Forschungsgemeinschaft via the Transregional Collaborative Research Center TRR 33
- Emmy Noether Programme [RO 3676/1-1]
- ARCHES prize of the German Ministry of Education and Research (BMBF)
- graduate school 'Theoretical Astrophysics and Particle Physics' at the University of Wurzburg [GRK 1147]
- Excellence Cluster EXC 153
- German-Australian exchange programme [DAAD/Go8]
- European Research Council (ERC-StG) [EXAGAL-308037]
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 less than or similar to 1.1 x 10(51) 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 similar to 0.5 x 10(51) 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.
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