Journal
ASTRONOMY & ASTROPHYSICS
Volume 656, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/202140881
Keywords
methods: numerical; nuclear reactions; nucleosynthesis; abundances; stars: abundances; supernovae: general; white dwarfs
Categories
Funding
- Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) [138713538 -SFB 881]
- Klaus Tschira Foundation
- ERC [724560]
- Lendulet grant of the Hungarian Academy of Sciences [LP17-2014]
- Australian Research Council [FT160100028]
- COST (European Cooperation in Science and Technology) [CA16117]
- European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme [759253]
- Gauss Centre for Supercomputing e.V.
- BEIS capital funding via STFC capital grants [ST/P002307/1, ST/R002452/1]
- STFC [ST/R00689X/1]
- Australian Government
- Science and Technology Facilities Council [ST/T000198/1] Funding Source: researchfish
- European Research Council (ERC) [724560] Funding Source: European Research Council (ERC)
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The study explores the potential explosion mechanisms of Type Ia supernovae from sub-Chandrasekhar mass carbon-oxygen white dwarfs and finds a significant impact of progenitor metallicity on nucleosynthetic yields. Experimental data demonstrate a strong influence of metallicity on yields, with an increase in Mn-55 production with metallicity. The results suggest that the contribution of Type Ia supernovae from these white dwarfs might be lower than previously estimated.
Double detonations in sub-Chandrasekhar mass carbon-oxygen white dwarfs (WD) with helium shells ares potential explosion mechanisms for Type Ia supernovae. The mechanism consists of a shell detonation and subsequent core detonation. The focus of our study is the effect of the progenitor metallicity on the nucleosynthetic yields. For this, we computed and analyzed a set of 11 different models with varying core and shell masses at four different metallicities each. This results in a total of 44 models at metallicities between 0.01 Z(circle dot) and 3 Z(circle dot). Our models show a strong impact of the metallicity in the high-density regime. The presence of Ne-22 causes a neutron-excess that shifts the production from Ni-56 to stable isotopes such as Fe-54 and Ni-58 in the alpha-rich freeze-out regime. The isotopes of the metallicity implementation further serve as seed nuclei for additional reactions in the shell detonation. The production of Mn-55 increases with metallicity, confirming the results of previous work. A comparison of elemental ratios relative to iron shows a good match to solar values for some models. Super-solar values are reached for Mn at 3 Z(circle dot) and solar values in some models at Z(circle dot). This indicates that the required contribution of Type Ia supernovae originating from Chandrasekhar-mass WDs can be lower than estimated in previous work to reach solar values of [Mn/Fe] at [Fe/H] = 0. Our galactic chemical evolution models suggest that Type Ia supernovae from sub-Chandrasekhar mass white dwarfs, along with core-collapse supernovae, could account for more than 80% of the solar Mn abundance. Using metallicity-dependent Type Ia supernova yields helps to reproduce the upward trend of [Mn/Fe] as a function of metallicity for the solar neighborhood. These chemical evolution predictions, however, depend on the massive star yields adopted in the calculations.
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