期刊
ASTROPHYSICAL JOURNAL
卷 799, 期 1, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/799/1/54
关键词
atomic processes; Galaxy: abundances; Galaxy: evolution; nuclear reactions, nucleosynthesis, abundances; supernovae: general
资金
- B2FH Association
- CILEA Consortium through a LISA Initiative (Laboratory for Interdisciplinary Advanced Simulation) grant
- University of Washington (Institute for Nuclear Theory, Seattle, WA, INT Program) [INT-14-2b]
- Deutsche Forschungsgemeinschaft via the Emmy Noether Program [RO 3676/1-1]
- graduate school Theoretical Astrophysics and Particle Physics at the University of Wurzburg [GRK 1147]
- German Ministry of Education and Research (BMBF)
- DAAD/Go8 German-Australian exchange program
- Swiss NSF
- European Research Council [GA 321263-FISH]
- Transregional Collaborative Research Centre TRR33 The Dark Universe und the Cluster of Excellence Origin and Structure of the Universe at Munich Technical University
The bulk of p isotopes is created in the gamma processes mainly by sequences of photodisintegrations and beta decays in explosive conditions in Type Ia supernovae (SNIa) or in core collapse supernovae (ccSN). The contribution of different stellar sources to the observed distribution of p-nuclei in the solar system is still under debate. We explore single degenerate Type Ia supernovae in the framework of two-dimensional SNIa delayed-detonation explosion models. Travaglio et al. discussed the sensitivity of p-nuclei production to different SNIa models, i.e., delayed detonations of different strength, deflagrations, and the dependence on selected s-process seed distributions. Here we present a detailed study of p-process nucleosynthesis occurring in SNIa with s-process seeds at different metallicities. Based on the delayed-detonation model DDT-a of TRV11, we analyze the dependence of p-nucleosynthesis on the s-seed distribution obtained from different strengths of the C-13 pocket. We also demonstrate that Pb-208 seed alone changes the p-nuclei production considerably. The heavy-s seeds (140 <= A < 208) contribute with about 30%-40% to the total light-p nuclei production up to Ba-132 (with the exception of Mo-94 and Ba-130, to which the heavy-s seeds contribute with about 15% only). Using a Galactic chemical evolution code from Travaglio et al., we study the contribution of SNIa to the solar stable p-nuclei. We find that explosions of Chandrasekhar-mass single degenerate systems produce a large amount of p-nuclei in our Galaxy, both in the range of light (A <= 120) and heavy p-nuclei, at almost flat average production factors (within a factor of about three). We discussed in details p-isotopes such as Mo-94 with a behavior diverging from the average, which we attribute to uncertainties in the nuclear data or in SNIa modeling. Li et al. find that about 70% of all SNeIa are normal events. If these are explained in the framework of explosions of Chandrasekhar-mass white dwarfs resulting from the single-degenerate progenitor channel, we find that they are responsible for at least 50% of the p-nuclei abundances in the solar system.
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