Role of Core-collapse Supernovae in Explaining Solar System Abundances of p Nuclides
Role of Core-collapse Supernovae in Explaining Solar System Abundances of p Nuclides
复制标题
核心塌陷超新星在解释太阳系 p 核素丰度中的作用
DOI：
--
复制
发表时间：
2018
期刊：
影响因子：
--
通讯作者：
Christopher West
中科院分区：
文献类型：
--
作者：
C. Travaglio;T. Rauscher;T. Rauscher;A. Heger;M. Pignatari;Christopher West;Christopher West
在74Se和196hg之间的重而稳定的富质子同位素（p核）的产生是由于在不同类型的恒星中激活的不同核合成过程的贡献。尽管这些过程已经受到了各种各样的研究，但它们对银河系化学演化（GCE）的相对贡献仍然存在争议。本文首次将核心坍缩超新星（ccSNe）的金属丰度和前体质量依赖产率纳入化学演化模型，研究了GCE中p核素的核合成。我们使用了来自两组不同恒星产量的金属丰度和祖先质量网格，并跟踪了ccSNe对银河系丰度的贡献作为时间的函数。结合以往对热核超新星（SNIa）中p核产生的研究，并使用相同的GCE描述，这使我们能够比较SNIa和ccSNe在银河系中p核产生中的各自作用。在太阳金属丰度下，ccSN中的γ过程在很大范围内（13 M⊙-25 M⊙）是非常有效的。由于这是一个二次过程，其效率取决于重元素的初始丰度，因此其贡献大大低于太阳金属丰度。这使得仅通过ccSNe的贡献来解释太阳系中p核素的库存具有挑战性。特别是，我们发现ccSNe对太阳p核素丰度的贡献不到10%，只有少数例外。由于ccSNe中其他核合成位点的贡献不确定，如中微子风或富含α-的冻结，我们得出结论，轻p核素74Se， 78Kr， 84Sr和92Mo可能仍然完全或部分地在ccSNe中产生。γ-过程在一组恒星模型中占74Se相对太阳丰度的两倍，在另一组恒星模型中占196Hg相对太阳丰度的两倍。由于Pb同位素208,207,206Pb的光分解，我们的一组模型在不确定范围内再现了最重p核196Hg的太阳丰度。对于所有其他p核素，丰度低至太阳水平的2%。
The production of the heavy stable proton-rich isotopes between 74Se and 196Hg—the p nuclides—is due to the contribution from different nucleosynthesis processes, activated in different types of stars. Whereas these processes have been subject to various studies, their relative contributions to Galactic chemical evolution (GCE) are still a matter of debate. Here we investigate for the first time the nucleosynthesis of p nuclides in GCE by including metallicity and progenitor mass-dependent yields of core-collapse supernovae (ccSNe) into a chemical evolution model. We used a grid of metallicities and progenitor masses from two different sets of stellar yields and followed the contribution of ccSNe to the Galactic abundances as a function of time. In combination with previous studies on p-nucleus production in thermonuclear supernovae (SNIa), and using the same GCE description, this allows us to compare the respective roles of SNeIa and ccSNe in the production of p-nuclei in the Galaxy. The γ process in ccSN is very efficient for a wide range of progenitor masses (13 M⊙–25 M⊙) at solar metallicity. Since it is a secondary process with its efficiency depending on the initial abundance of heavy elements, its contribution is strongly reduced below solar metallicity. This makes it challenging to explain the inventory of the p nuclides in the solar system by the contribution from ccSNe alone. In particular, we find that ccSNe contribute less than 10% of the solar p nuclide abundances, with only a few exceptions. Due to the uncertain contribution from other nucleosynthesis sites in ccSNe, such as neutrino winds or α-rich freeze out, we conclude that the light p-nuclides 74Se, 78Kr, 84Sr, and 92Mo may either still be completely or only partially produced in ccSNe. The γ-process accounts for up to twice the relative solar abundances for 74Se in one set of stellar models and 196Hg in the other set. The solar abundance of the heaviest p nucleus 196Hg is reproduced within uncertainties in one set of our models due to photodisintegration of the Pb isotopes 208,207,206Pb. For all other p nuclides, abundances as low as 2% of the solar level were obtained.
影响因子：
4.8
作者：
N. Nishimura;N. Nishimura;T. Rauscher;T. Rauscher;Raphael Hirschi;Raphael Hirschi;A. Murphy;G. Cescutti;G. Cescutti;C. Travaglio
通讯作者：
N. Nishimura;N. Nishimura;T. Rauscher;T. Rauscher;Raphael Hirschi;Raphael Hirschi;A. Murphy;G. Cescutti;G. Cescutti;C. Travaglio
影响因子：
5.3
作者：
Schulz, Toni;Muenker, Carsten;Peters, Stefan T. M.
通讯作者：
Peters, Stefan T. M.