Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M ☉ progenitors: implications for Mo and Ru production
Nucleosynthesis in 2D core-collapse supernovae of 11.2 and 17.0 M ☉ progenitors: implications for Mo and Ru production
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11.2 和 17.0 M ☉ 前身的二维核心塌缩超新星中的核合成：对 Mo 和 Ru 产生的影响
DOI：
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发表时间：
2017
期刊：
影响因子：
--
通讯作者：
F. Thielemann
中科院分区：
文献类型：
--
作者：
M. Eichler;K. Nakamura;T. Takiwaki;T. Kuroda;K. Kotake;M. Hempel;R. Cabez'on;M. Liebendorfer;F. Thielemann
核心塌缩超新星是银河系历史上最早的重元素污染源。因此，重要的是要研究其喷射物的核成分，并了解它们对前体结构(例如质量、致密性、金属丰度)的依赖。在这里，我们提供了一个详细的核合成研究，基于两个长期的，二维的核心塌缩超新星模拟，分别是11.2mlsubg⊙L/subg和17.0mlsubg⊙L/subg星。我们发现在这两个模型中都可以产生远远超出铁基的核(直到Z-≈44)，并详细讨论了p-核lsupg92，94l/supgMo和lsupg96，98l/supgRu的核合成。虽然我们在两个模拟中都观察到了在稍富中子的条件下产生lsupg92l/supgMo和lsupg94l/supgMo，但只有通过νp工艺才能有效地产生lsupg96,981/supgRu。此外，νp工艺中Ru的生产在很大程度上依赖于喷射物中非常富质子的物质的存在。与太阳系和太阳系前颗粒中这些同位素之间的丰度比相比，这种生产机制的解体产生了有趣的结果。
Core-collapse supernovae are the first polluters of heavy elements in the galactic history. As such, it is important to study the nuclear compositions of their ejecta, and understand their dependence on the progenitor structure (e.g., mass, compactness, metallicity). Here, we present a detailed nucleosynthesis study based on two long-term, two-dimensional core-collapse supernova simulations of a 11.2 Mlsubg⊙l/subg and a 17.0 Mlsubg⊙l/subg star. We find that in both models nuclei well beyond the iron group (up to Z≈44) can be produced, and discuss in detail also the nucleosynthesis of the p-nuclei lsupg92,94l/supgMo and lsupg96,98l/supgRu. While we observe the production of lsupg92l/supgMo and lsupg94l/supgMo in slightly neutron-rich conditions in both simulations, lsupg96,98l/supgRu can only be produced efficiently via the νp-process. Furthermore, the production of Ru in the νp-process heavily depends on the presence of very proton-rich material in the ejecta. This disentanglement of production mechanisms has interesting consequences when comparing to the abundance ratios between these isotopes in the solar system and in presolar grains.
DOI：
10.1146/annurev-nucl-102115-044747
发表时间：
2016-02
影响因子：
12.4
作者：
H. Janka;T. Melson;A. S. M. Astrophysics;Garching;Physik Dept.;Tum
通讯作者：
H. Janka;T. Melson;A. S. M. Astrophysics;Garching;Physik Dept.;Tum
影响因子：
8.6
作者：
G. Martínez-Pinedo;T. Fischer;A. Lohs;L. Huther
通讯作者：
G. Martínez-Pinedo;T. Fischer;A. Lohs;L. Huther